text:
late-type stars, measuring
separate abundances for \textasciitilde 15 elements per star and creating the first
high-precision spectroscopic survey of all Galactic stellar populations
(bulge, bar, disks, halo) with a uniform set of stellar tracers and
spectral diagnostics. The Multi-object APO Radial Velocity Exoplanet
Large-area Survey (MARVELS) will monitor radial velocities of more than
8000 FGK stars with the sensitivity and cadence (10-40 m s-1,
\textasciitilde 24 visits per star) needed to detect giant planets with periods up to
two years, providing an unprecedented data set for understanding the
formation and dynamical evolution of giant planet systems. As of 2011
January, SDSS-III has obtained spectra of more than 240,000 galaxies,
29,000 z {$>$}= 2.2 quasars, and 140,000 stars, including 74,000 velocity
measurements of 2580 stars for MARVELS.},
  file = {/Users/Oliver/Zotero/storage/PT2UG3UM/Eisenstein et al. - 2011 - SDSS-III Massive Spectroscopic Surveys of the Dis.pdf},
  journal = {The Astronomical Journal},
  keywords = {cosmology: observations,Galaxy: evolution,planets and satellites: detection,surveys}
}

@article{elsworth+1995,
  title = {Slow Rotation of the {{Sun}}'s Interior},
  author = {Elsworth, Y. and Howe, R. and Isaak, G. R. and McLeod, C. P. and Miller, B. A. and New, R. and Wheeler, S. J. and Gough, D. O.},
  year = {1995},
  month = aug,
  volume = {376},
  pages = {669--672},
  issn = {0028-0836},
  doi = {10.1038/376669a0},
  abstract = {THE rotation of the Sun is not that of a rigid body; at its surface, the gas near the poles has a lower angular velocity than that near the equator1. This latitudinal variation persists to the base of the convection zone, below which the angular velocity becomes
approximately uniform2,3. Any variations of angular velocity at much greater depths are, however, poorly
constrained4-10. Observations of solar oscillation
modes have been used to probe density variations in the Sun; rotational splitting of degenerate modes, although difficult to resolve, provides important constraints on the dynamical structure11. Here we report observations of rotationally split modes made over a three-year period with the Birmingham Solar Oscillations Network. Our results indicate that there is a substantial region inside the Sun that is rotating more slowly than the surface. This situation seems likely to be transient\textemdash the minimum-energy state would have all the deeper
regions rotating with the same angular velocity\textemdash and is at variance with our current ideas about the rotational evolution of main-sequence stars12. We have no solution to the dynamical problem this poses.},
  journal = {Nature}
}

@article{elsworth+2017,
  title = {A New Method for the Asteroseismic Determination of the Evolutionary State of Red-Giant Stars},
  author = {Elsworth, Yvonne and Hekker, Saskia and Basu, Sarbani and Davies, Guy R.},
  year = {2017},
  month = apr,
  volume = {466},
  pages = {3344},
  doi = {10.1093/mnras/stw3288},
  abstract = {Determining the ages of red-giant stars is a key problem in stellar astrophysics. One of the difficulties in this determination is to know the evolutionary state of the individual stars - I.e. have they started to burn Helium in their cores? That is the topic of this paper. Asteroseismic data provide a route to achieving this information. What we present here is a highly autonomous way of determining the evolutionary state from an analysis of the power spectrum of the light curve. The method is fast and efficient and can provide results for a large number of stars. It uses the structure of the dipole-mode oscillations, which have a mixed character in red-giant stars, to determine some measures that are used in the categorization. It does not require that all the individual components of any given mode be separately characterized. Some 6604 red-giant stars have been classified. Of these, 3566 are determined to be on the red-giant branch, 2077 are red-clump and 439 are secondary-clump stars. We do not specifically identify the low-metallicity, horizontal-branch stars. The difference between red-clump and secondary-clump stars is dependent on the manner in which Helium burning is first initiated. We discuss that the way the boundary between these classifications is set may lead to mis-categorization in a small number of stars. The remaining 522 stars were not classified either because they lacked sufficient power in the dipole modes (so-called depressed dipole modes) or because of conflicting values in the parameters.},
  file = {/Users/Oliver/Zotero/storage/K5YTJJWZ/Elsworth et al. - 2017 - A new method for the asteroseismic determination o.pdf;/Users/Oliver/Zotero/storage/6ZEXSHTU/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{epstein+pinsonneault2014,
  title = {How {{Good}} a {{Clock}} Is {{Rotation}}? {{The Stellar Rotation}}-{{Mass}}-{{Age Relationship}} for {{Old Field Stars}}},
  shorttitle = {How {{Good}} a {{Clock}} Is {{Rotation}}?},
  author = {Epstein, Courtney R. and Pinsonneault, Marc H.},
  year = {2014},
  month = jan,
  volume = {780},
  pages = {159},
  doi = {10.1088/0004-637X/780/2/159},
  abstract = {The rotation-mass-age relationship offers a promising avenue for measuring the ages of field stars, assuming the attendant uncertainties to this technique can be well characterized. We model stellar angular momentum evolution starting with a rotation distribution from open cluster M37. Our predicted rotation-mass-age relationship shows significant zero-point offsets compared to an alternative angular momentum loss law and published gyrochronology relations. Systematic errors at the 30\% level are permitted by current data, highlighting the need for empirical guidance. We identify two fundamental sources of uncertainty that limit the precision of rotation-based ages and quantify their impact. Stars are born with a range of rotation rates, which leads to an age range at fixed rotation period. We find that the inherent ambiguity from the initial conditions is important for all young stars, and remains large for old stars below 0.6 M \textsubscript{{$\Sun$}}. Latitudinal surface differential rotation also introduces a minimum uncertainty into rotation period measurements and, by extension, rotation-based ages. Both models and the data from binary star systems 61 Cyg and {$\alpha$} Cen demonstrate that latitudinal differential rotation is the limiting factor for rotation-based age precision among old field stars, inducing uncertainties at the \textasciitilde 2 Gyr level. We also examine the relationship between variability amplitude, rotation period, and age. Existing ground-based surveys can detect field populations with ages as old as 1-2 Gyr, while space missions can detect stars as old as the Galactic disk. In comparison with other techniques for measuring the ages of lower main sequence stars, including geometric parallax and asteroseismology, rotation-based ages have the potential to be the most precise chronometer for 0.6-1.0 M \textsubscript{{$\Sun$}} stars.},
  file = {/Users/Oliver/Zotero/storage/2C6YU3YW/Epstein and Pinsonneault - 2014 - How Good a Clock is Rotation The Stellar Rotation.pdf;/Users/Oliver/Zotero/storage/F6J3QUWS/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{esselstein+2018,
  title = {The {{K2 M67 Study}}: {{Establishing}} the {{Limits}} of {{Stellar Rotation Period Measurements}} in {{M67}} with {{K2 Campaign}} 5 {{Data}}},
  shorttitle = {The {{K2 M67 Study}}},
  author = {Esselstein, Rebecca and Aigrain, Suzanne and Vanderburg, Andrew and Smith, Jeffrey C. and Meibom, Soren and Van Saders, Jennifer and Mathieu, Robert},
  year = {2018},
  month = jun,
  volume = {859},
  pages = {167},
  issn = {1538-4357},
  doi = {10.3847/1538-4357/aac20e},
  abstract = {The open cluster M67 offers the unique opportunity to measure rotation periods for solar-age stars across a range of masses, potentially filling a critical gap in the understanding of angular momentum loss in older main sequence stars. The observation of M67 by NASA K2 Campaign 5 provided light curves with high enough precision to make this task possible, albeit challenging, as the pointing instability, 75d observation window, crowded field, and typically low-amplitude signals mean determining accurate rotation periods on the order of 25 - 30d is inherently difficult. Lingering, non-astrophysical signals with power at {$>$}25d found in a set of Campaign 5 A and F stars compounds the problem. To achieve a quantitative understanding of the best-case scenario limits for reliable period detection imposed by these inconveniences, we embarked on a comprehensive set of injection tests, injecting 120,000 sinusoidal signals with periods ranging from 5 to 35d and amplitudes from 0.05\% to 3.0\% into real Campaign 5 M67 light curves processed using two different pipelines. We attempted to recover the signals using a normalized version of the Lomb-Scargle periodogram and setting a detection threshold. We find that while the reliability of detected periods is high, the completeness (sensitivity) drops rapidly with increasing period and decreasing amplitude, maxing at 15\% recovery rate for the solar case (i.e. 25d period, 0.1\% amplitude). This study highlights the need for caution in determining M67 rotation periods from Campaign 5 data, but this can be extended to other clusters observed by K2 and, soon, TESS.},
  archivePrefix = {arXiv},
  eprint = {1805.09922},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/87QHJ8E3/Esselstein et al. - 2018 - The K2 M67 Study Establishing the Limits of Stell.pdf;/Users/Oliver/Zotero/storage/H2U83RRT/1805.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{esselstein+2018a,
  title = {The {{{\emph{K2}}}} {{M67 Study}}: {{Establishing}} the {{Limits}} of {{Stellar Rotation Period Measurements}} in {{M67}} with {{{\emph{K2}}}} {{Campaign}} 5 {{Data}}},
  shorttitle = {The {{{\emph{K2}}}} {{M67 Study}}},
  author = {Esselstein, Rebecca and Aigrain, Suzanne and Vanderburg, Andrew and Smith, Jeffrey C. and Meibom, Soren and Saders, Jennifer Van and Mathieu, Robert},
  year = {2018},
  month = jun,
  volume = {859},
  pages = {167},
  issn = {1538-4357},
  doi = {10.3847/1538-4357/aac20e},
  abstract = {The open cluster M67 offers a unique opportunity to measure rotation periods for solar-age stars across a range of masses, potentially filling a critical gap in the understanding of angular momentum loss in older main sequence stars. The observation of M67 by NASA K2 Campaign 5 provided light curves with high enough precision to make this task possible, albeit challenging, as the pointing instability, 75 day observation window, crowded field, and typically low-amplitude signals mean that determining accurate rotation periods on the order of 25\textendash 30 days is inherently difficult. Lingering, non-astrophysical signals with power at 25 days found in a set of Campaign 5 A and F stars compounds the problem. To achieve a quantitative understanding of the best-case scenario limits for reliable period detection imposed by these inconveniences, we embarked on a comprehensive set of injection tests, injecting 120,000 sinusoidal signals with periods ranging from 5 to 35 days and amplitudes from 0.05\% to 3.0\% into real Campaign 5 M67 light curves processed using two different pipelines. We attempted to recover the signals using a normalized version of the Lomb\textendash Scargle periodogram and setting a detection threshold. We find that, while the reliability of detected periods is high, the completeness (sensitivity) drops rapidly with increasing period and decreasing amplitude, maxing at a 15\% recovery rate for the solar case (i.e., 25 day period, 0.1\% amplitude). This study highlights the need for caution in determining M67 rotation periods from Campaign 5 data, but this can be extended to other clusters observed by K2 (and soon, TESS).},
  file = {/Users/Oliver/Zotero/storage/V2R3QWDM/Esselstein et al. - 2018 - The iK2i M67 Study Establishing the Limits o.pdf},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{etangs+2017,
  title = {Search for Rings and Satellites around the Exoplanet {{CoRoT}}-9b Using {{Spitzer}} Photometry},
  author = {des Etangs, A. Lecavelier and H{\'e}brard, G. and Blandin, S. and Cassier, J. and Deeg, H. J. and Bonomo, A. S. and Bouchy, F. and D{\'e}sert, J.-M. and Ehrenreich, D. and Deleuil, M. and D{\'i}az, R. F. and Moutou, C.},
  year = {2017},
  month = may,
  abstract = {Using Spitzer photometry at 4.5 microns, we search for rings and satellites around the long period transiting planet CoRoT-9b. We observed two transits in 2010 and 2011. From their non-detection, we derive upper limits on the plausible physical characteristics of these objects in the planet environment. We show that a satellite larger than about 2.5 Earth radii is excluded at 3-\$\textbackslash sigma\$ for a wide range of elongations at the two epochs of observations. Combining the two observations, we conclude that rings are excluded for a wide variety of sizes and inclination. We find that for a ring extending up to the Roche limit, its inclination angle from the edge-on configuration as seen from the Earth must be lower than 13\{\textbackslash deg\} in the case of silicate composition and lower than 3\{\textbackslash deg\} in the case of material with water ice density.},
  archivePrefix = {arXiv},
  eprint = {1705.01836},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/CXWX2V5H/Etangs et al. - 2017 - Search for rings and satellites around the exoplan.pdf;/Users/Oliver/Zotero/storage/Q5Q6DS39/1705.html},
  journal = {arXiv:1705.01836 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{farr+2018,
  title = {Aldebaran b's {{Temperate Past Uncovered}} in {{Planet Search Data}}},
  author = {Farr, Will M. and Pope, Benjamin J. S. and Davies, Guy R. and North, Thomas S. H. and White, Timothy R. and Barrett, Jim W. and Miglio, Andrea and Lund, Mikkel N. and Antoci, Victoria and Fredslund Andersen, Mads and Grundahl, Frank and Huber, Daniel},
  year = {2018},
  month = oct,
  volume = {865},
  pages = {L20},
  issn = {0004-637X},
  doi = {10.3847/2041-8213/aadfde},
  abstract = {The nearby red giant Aldebaran is known to host a gas giant planetary companion from decades of ground-based spectroscopic radial velocity measurements. Using Gaussian Process-based Continuous Auto-Regressive Moving Average models, we show that these historic data also contain evidence of acoustic oscillations in the star itself, and verify this result with further dedicated ground-based spectroscopy using the SONG telescope and space-based photometry with the Kepler Space Telescope. From the frequency of these oscillations we determine the mass of Aldebaran to be 1.16 {$\pm$} 0.07 \{M\}{$\odot$} , and note that
this implies its planet will have been subject to insolation comparable to the Earth for some of the star's main sequence lifetime. Our
approach to sparse, irregularly sampled time series astronomical observations has the potential to unlock asteroseismic measurements for thousands of stars in archival data, and push to lower-mass planets around red giant stars.},
  file = {/Users/Oliver/Zotero/storage/5HZCQEPJ/Farr et al. - 2018 - Aldebaran b’s Temperate Past Uncovered in Planet S.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {methods: data analysis,methods: statistical,planets and satellites: individual: Aldebaran b,stars: individual: Aldebaran,stars: oscillations: including pulsations,techniques: radial velocities}
}

@article{feltzing+2017,
  title = {On the Metallicity Dependance of the [{{Y}}/{{Mg}}] - Age Relation for Solar Type Stars},
  author = {Feltzing, S. and Howes, L. M. and McMillan, P. J. and Stonkute, E.},
  year = {2017},
  month = feb,
  volume = {465},
  pages = {L109-L113},
  issn = {1745-3925, 1745-3933},
  doi = {10.1093/mnrasl/slw209},
  abstract = {Several recent studies of Solar twins in the Solar neighbourhood have shown a tight correlation between various elemental abundances and age, in particular [Y/Mg]. If this relation is real and valid for other types of stars as well as elsewhere in the Galaxy it would provide a very powerful tool to derive ages of stars without the need to resort to determining their masses (evolutionary stage) very precisely. The method would also likely work if the stellar parameters have relatively large errors. The studies presented in the recent literature span a narrow range of [Fe/H]. By studying a larger sample of Solar neighbourhood dwarfs with a much larger range in [Fe/H], we find that the relation between [Y/Mg] and age depends on the [Fe/H] of the stars. Hence, it appears that the [Y/Mg] - age relation is unique to Solar analogues.},
  archivePrefix = {arXiv},
  eprint = {1610.03852},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HD26269H/Feltzing et al. - 2017 - On the metallicity dependance of the [YMg] - age .pdf;/Users/Oliver/Zotero/storage/MACSCUR3/1610.html},
  journal = {Monthly Notices of the Royal Astronomical Society: Letters},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{fleming+2019,
  title = {Rotation {{Period Evolution}} in {{Low}}-Mass {{Binary Stars}}: {{The Impact}} of {{Tidal Torques}} and {{Magnetic Braking}}},
  shorttitle = {Rotation {{Period Evolution}} in {{Low}}-Mass {{Binary Stars}}},
  author = {Fleming, David P. and Barnes, Rory and Davenport, James R. A. and Luger, Rodrigo},
  year = {2019},
  month = aug,
  volume = {881},
  pages = {88},
  issn = {0004-637X},
  doi = {10.3847/1538-4357/ab2ed2},
  abstract = {We examine how tides, stellar evolution, and magnetic braking shape the
rotation period (P rot) evolution of low-mass stellar
binaries up to orbital periods (P orb) of 100 days across a
wide range of tidal dissipation parameters using two common equilibrium
tidal models. We find that many binaries with P orb {$\lessequivlnt$} 20
days tidally lock, and most with P orb {$\lessequivlnt$} 4 days tidally
lock into synchronous rotation on circularized orbits. At short P
orb, tidal torques produce a population of fast rotators that
single-star-only models of magnetic braking fail to produce. In many
cases, we show that the competition between magnetic braking and tides
produces a population of subsynchronous rotators that persists for 1
Gyr, even in short-P orb binaries, qualitatively reproducing
the subsynchronous eclipsing binaries discovered in the Kepler field by
Lurie et al. Both equilibrium tidal models predict that binaries can
tidally interact out to P orb {$\approx$} 80 days, while the
constant phase lag tidal model predicts that binaries can tidally lock
out to P orb {$\approx$} 100 days. Tidal torques often force the P
rot evolution of stellar binaries to depart from the
long-term magnetic-braking-driven spin-down experienced by single stars,
revealing that P rot is not a valid proxy for age in all
cases, i.e., gyrochronology can underpredict ages by up to 300\% unless
one accounts for binarity. We suggest that accurate determinations of
orbital eccentricties and P rot can be used to discriminate
between which equilibrium tidal models best describe tidal interactions
in low-mass binary stars.},
  file = {/Users/Oliver/Zotero/storage/5GQEJESH/Fleming et al. - 2019 - Rotation Period Evolution in Low-mass Binary Stars.pdf},
  journal = {The Astrophysical Journal},
  keywords = {binaries: close,stars: evolution,stars: kinematics and dynamics,stars: rotation}
}

@article{flower1996,
  title = {Transformations from {{Theoretical Hertzsprung}}-{{Russell Diagrams}} to {{Color}}-{{Magnitude Diagrams}}: {{Effective Temperatures}}, {{B}}-{{V Colors}}, and {{Bolometric Corrections}}},
  shorttitle = {Transformations from {{Theoretical Hertzsprung}}-{{Russell Diagrams}} to {{Color}}-{{Magnitude Diagrams}}},
  author = {Flower, Phillip J.},
  year = {1996},
  month = sep,
  volume = {469},
  pages = {355},
  doi = {10.1086/177785},
  abstract = {This paper provides improved numerical relations between effective temperatures of stars, their B - V colors, and their bolometric corrections (B Cs) for the purpose of comparing theoretical stellar evolutionary calculations to color-magnitude diagrams of star clusters. Temperatures and bolometric correction measurements for 335 stars from the literature form the observational basis for the transformations. Measured temperatures range from 2900 to 52,500 K. Polynomial fits to the observations give relations between effective temperatures and B - V colors and between temperatures and bolometric corrections. Hot supergiants appear to have a T\textsubscript{eff}:B-V relation slightly different from those of main-sequence stars, subgiants, and giants. All luminosity classes appear to follow a unique T\textsubscript{eff}:BC relation. The T\textsubscript{eff}:BC relation for stars with temperatures less than{\~ }5000 K, however, is uncertain because temperatures of the coolest stars are determined from uncertain angular diameters.},
  file = {/Users/Oliver/Zotero/storage/677VJRCY/Flower - 1996 - Transformations from Theoretical Hertzsprung-Russe.pdf;/Users/Oliver/Zotero/storage/9Q3MJL8M/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{foreman-mackey+2012,
  title = {{{DAFT}}: {{Beautifully Rendered Probabilistic Graphical Models}}},
  author = {{Foreman-Mackey}, Dan\# and Hogg, David W. and Fulford, David S.},
  year = {2012}
}

@article{foreman-mackey+2013,
  title = {Emcee: {{The MCMC Hammer}}},
  shorttitle = {Emcee},
  author = {{Foreman-Mackey}, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan},
  year = {2013},
  month = mar,
  volume = {125},
  pages = {306--312},
  issn = {00046280, 15383873},
  doi = {10.1086/670067},
  abstract = {We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman \& Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to \$\textbackslash sim N\^2\$ for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our implementation and API. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the MIT License.},
  archivePrefix = {arXiv},
  eprint = {1202.3665},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/9NJ332NE/Foreman-Mackey et al. - 2013 - emcee The MCMC Hammer.pdf;/Users/Oliver/Zotero/storage/4QHEWCXP/1202.html},
  journal = {Publications of the Astronomical Society of the Pacific},
  keywords = {Astrophysics - Instrumentation and Methods for Astrophysics,Physics - Computational Physics,Statistics - Computation},
  number = {925}
}

@article{foreman-mackey+2017,
  title = {Fast and {{Scalable Gaussian Process Modeling}} with {{Applications}} to {{Astronomical Time Series}}},
  author = {{Foreman-Mackey}, Daniel and Agol, Eric and Ambikasaran, Sivaram and Angus, Ruth},
  year = {2017},
  month = dec,
  volume = {154},
  pages = {220},
  issn = {0004-6256},
  doi = {10.3847/1538-3881/aa9332},
  abstract = {The growing field of large-scale time domain astronomy requires methods
for probabilistic data analysis that are computationally tractable, even
with large data sets. Gaussian processes (GPs) are a popular class of
models used for this purpose, but since the computational cost scales,
in general, as the cube of the number of data points, their application
has been limited to small data sets. In this paper, we present a novel
method for GPs modeling in one dimension where the computational
requirements scale linearly with the size of the data set. We
demonstrate the method by applying it to simulated and real astronomical
time series data sets. These demonstrations are examples of
probabilistic inference of stellar rotation periods, asteroseismic
oscillation spectra, and transiting planet parameters. The method
exploits structure in the problem when the covariance function is
expressed as a mixture of complex exponentials, without requiring evenly
spaced observations or uniform noise. This form of covariance arises
naturally when the process is a mixture of stochastically driven damped
harmonic oscillators\textemdash providing a physical motivation for and
interpretation of this choice\textemdash but we also demonstrate that it can
be a useful effective model in some other cases. We present a
mathematical description of the method and compare it to existing
scalable GP methods. The method is fast and interpretable, with a range
of potential applications within astronomical data analysis and beyond.
We provide well-tested and documented open-source implementations of
this method in C++, Python, and Julia.},
  file = {/Users/Oliver/Zotero/storage/NUK4M2QS/Foreman-Mackey et al. - 2017 - Fast and Scalable Gaussian Process Modeling with A.pdf},
  journal = {The Astronomical Journal},
  keywords = {asteroseismology,methods: data analysis,methods: statistical,planetary systems,stars: rotation}
}

@article{foreman-mackey2016,
  title = {Corner.Py: {{Scatterplot}} Matrices in {{Python}}},
  shorttitle = {Corner.Py},
  author = {{Foreman-Mackey}, Daniel},
  year = {2016},
  month = jun,
  volume = {1},
  doi = {10.21105/joss.00024},
  abstract = {This Python module uses matplotlib (Hunter 2007) to visualize multidimensional samples using a scatterplot matrix. In these
visualizations, each one- and two-dimensional projection of the sample is plotted to reveal covariances. corner was originally conceived to display the results of Markov Chain Monte Carlo simulations and the defaults are chosen with this application in mind but it can be used for displaying many qualitatively different samples.},
  file = {/Users/Oliver/Zotero/storage/UAB9QZH6/Foreman-Mackey - 2016 - corner.py Scatterplot matrices in Python.pdf},
  journal = {The Journal of Open Source Software}
}

@article{fossat+2017,
  title = {Asymptotic g Modes: {{Evidence}} for a Rapid Rotation of the Solar Core},
  shorttitle = {Asymptotic g Modes},
  author = {Fossat, E. and Boumier, P. and Corbard, T. and Provost, J. and Salabert, D. and Schmider, F. X. and Gabriel, A. H. and Grec, G. and Renaud, C. and Robillot, J. M. and {Roca-Cort{\'e}s}, T. and {Turck-Chi{\`e}ze}, S. and Ulrich, R. K. and Lazrek, M.},
  year = {2017},
  month = aug,
  volume = {604},
  pages = {A40},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201730460},
  abstract = {Context. Over the past 40 years, helioseismology has been enormously successful in the study of the solar interior. A shortcoming has been the lack of a convincing detection of the solar g modes, which are oscillations driven by gravity and are hidden in the deepest part of the solar body - its hydrogen-burning core. The detection of g modes is expected to dramatically improve our ability to model this core, the rotational characteristics of which have, until now, remained unknown. Aims: We present the identification of very low frequency g modes in the asymptotic regime and two important parameters that have long been waited for: the core rotation rate, and the asymptotic equidistant period spacing of these g modes. Methods: The GOLF instrument on board the SOHO space observatory has provided two decades of full-disk helioseismic data. The search for g modes in GOLF measurements has been extremely difficult because of solar and instrumental noise. In the present study, the p modes of the GOLF signal are analyzed differently: we search for possible collective frequency modulations that are produced by periodic changes in the deep solar structure. Such
modulations provide access to only very low frequency g modes, thus allowing statistical methods to take advantage of their asymptotic properties. Results: For oscillatory periods in the range between 9 and nearly 48 h, almost 100 g modes of spherical harmonic degree 1 and more than 100 g modes of degree 2 are predicted. They are not observed individually, but when combined, they unambiguously provide their asymptotic period equidistance and rotational splittings, in excellent agreement with the requirements of the asymptotic approximations. When the period equidistance has been measured, all of the individual frequencies of each mode can be determined. Previously, p-mode
helioseismology allowed the g-mode period equidistance parameter P0 to be bracketed inside a narrow range, between
approximately 34 and 35 min. Here, P0 is measured to be 34 min 01 s, with a 1 s uncertainty. The previously unknown g-mode
splittings have now been measured from a non-synodic reference with very high accuracy, and they imply a mean weighted rotation of 1277 {$\pm$} 10 nHz (9-day period) of their kernels, resulting in a rapid rotation frequency of 1644 {$\pm$} 23 nHz (period of one week) of the solar core itself, which is a factor 3.8 {$\pm$} 0.1 faster than the rotation of
the radiative envelope. Conclusions: The g modes are known to be the keys to a better understanding of the structure and dynamics of the solar core. Their detection with these precise parameters will certainly stimulate a new era of research in this field.},
  file = {/Users/Oliver/Zotero/storage/VRTUB3KI/Fossat et al. - 2017 - Asymptotic g modes Evidence for a rapid rotation .pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {Sun: helioseismology,Sun: interior,Sun: oscillations,Sun: rotation}
}

@article{frandsen+2013,
  title = {{{KIC}} 8410637: A 408-Day Period Eclipsing Binary Containing a Pulsating Giant Star},
  shorttitle = {{{KIC}} 8410637},
  author = {Frandsen, S. and Lehmann, H. and Hekker, S. and Southworth, J. and Debosscher, J. and Beck, P. and Hartmann, M. and Pigulski, A. and Kopacki, G. and Ko{\l}aczkowski, Z. and St{\c e}{\'s}licki, M. and Thygesen, A. O. and Brogaard, K. and Elsworth, Y.},
  year = {2013},
  month = aug,
  volume = {556},
  pages = {A138},
  doi = {10.1051/0004-6361/201321817},
  abstract = {Context. Detached eclipsing binaries (dEBs) are ideal targets for accurately measuring the masses and radii of their component stars. If at least one of the stars has evolved off the main sequence (MS), the masses and radii give a strict constraint on the age of the stars. Several dEBs containing a bright K giant and a fainter MS star have been discovered by the Kepler satellite. The mass and radius of a red giant (RG) star can also be derived from its asteroseismic signal. The parameters determined in this way depend on stellar models and may contain systematic errors. It is important to validate the asteroseismically determined mass and radius with independent methods. This can be done when stars are members of stellar clusters or members of dEBs. \\
 Aims: This paper presents an analysis of the dEB system KIC 8410637, which consists of an RG and an MS star. The aim is to derive accurate masses and radii for both components and provide the foundation for a strong test of the asteroseismic method and the accuracy of the deduced mass, radius, and age. \\
 Methods: We analysed high-resolution, high-signal-to-noise spectra from three different spectrographs. We also calculated a fit to the Kepler light curve and used ground-based photometry to determine the flux ratios between the component stars in the BVRI passbands. \\
 Results: We measured the masses and radii of the stars in the dEB, and the classical parameters T\textsubscript{eff}, log g, and [Fe/H] from the spectra and ground-based photometry. The RG component of KIC 8410637 is most likely in the core helium-burning red clump phase of evolution and has an age and composition that are very similar to the stars in the open cluster NGC 6819. The mass of the RG in KIC 8410637 should therefore be similar to the mass of RGs in NGC 6819, thus lending support to the latest version of the asteroseismic scaling relations. This is the first direct measurement of both mass and radius for an RG to be compared with values for RGs from asteroseismic scaling relations thereby providing an accurate comparison. We find excellent agreement between log g values derived from the binary analysis and asteroseismic scaling relations. \\
 Conclusions: We have determined the masses and radii of the two stars in the binary accurately. A detailed asteroseismic analysis will be presented in a forthcoming paper, allowing an informative comparison between the parameters determined for the dEB and from asteroseismology. Based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\'isica de Canarias.},
  file = {/Users/Oliver/Zotero/storage/88YLUTFN/Frandsen et al. - 2013 - KIC 8410637 a 408-day period eclipsing binary con.pdf;/Users/Oliver/Zotero/storage/UK8AA8MP/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{franzon+schramm2017,
  title = {Effects of Magnetic Fields in White Dwarfs},
  author = {Franzon, B. and Schramm, S.},
  year = {2017},
  month = feb,
  abstract = {We perform calculations of white dwarfs endowed with strong magnetic fields. White dwarfs are the progenitors of supernova Type Ia explosions and they are widely used as candles to show that the Universe is expanding and accelerating. However, observations of ultraluminous supernovae have suggested that the progenitor of such an explosion should be a white dwarf with mass above the well-known Chandrasekhar limit \$\textbackslash sim \textbackslash,\$1.4 \$\textbackslash rm\{M\_\{\textbackslash odot\}\}\$. In corroboration with other works, but by using a fully general relativistic framework, we obtained also strongly magnetized white dwarfs with masses \$\textbackslash rm\{M \textbackslash sim 2.0\textbackslash,\textbackslash, M\_\{\textbackslash odot\}\}\$.},
  archivePrefix = {arXiv},
  eprint = {1702.00571},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/KQREGVJV/Franzon and Schramm - 2017 - Effects of magnetic fields in white dwarfs.pdf;/Users/Oliver/Zotero/storage/MC6FNMNM/1702.html},
  journal = {arXiv:1702.00571 [astro-ph]},
  keywords = {Astrophysics - High Energy Astrophysical Phenomena,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{fusillo+2017,
  title = {Can Magnetic Fields Suppress Convection in the Atmosphere of Cool White Dwarfs? {{A}} Case Study on {{WD2105}}-820},
  shorttitle = {Can Magnetic Fields Suppress Convection in the Atmosphere of Cool White Dwarfs?},
  author = {Fusillo, Nicola Pietro Gentile and Tremblay, Pier-Emmanuel and Jordan, Stefan and G{\"a}nsicke, Boris T. and Kalirai, Jason S. and Cummings, Jeffrey},
  year = {2017},
  month = oct,
  abstract = {Around 10\% of white dwarfs exhibit global magnetic structures with fields ranging from 1 kG to hundreds of MG. Recently, the first radiation magnetohydrodynamics simulations of the atmosphere of white dwarfs showed that convection should be suppressed in their photospheres for magnetic fields with strengths B \$\textbackslash gtrsim\$ 50 kG. These predictions are in agreement with our knowledge of stellar physics (e.g. energy transfer in strong magnetic field regions of the solar photosphere), but have yet to be directly confirmed from white dwarf observations. We obtained COS far-UV spectroscopy of the weakly magnetic, hydrogen-atmosphere, white dwarf WD2105-820 and of three additional non-magnetic, convective remnants (all in the \$T\_\{\textbackslash mathrm\{eff\}\}\$ range 9000-11,000 K). We fitted both the COS and the already available optical spectra with convective and radiative atmospheric models. As expected, we find that for two of the non-magnetic comparison stars only convective model fits predict consistent \$T\_\{\textbackslash mathrm\{eff\}\}\$ values from both the optical and the FUV spectra. In contrast, for WD2105-820 only the best fitting radiative model produced consistent results.},
  archivePrefix = {arXiv},
  eprint = {1710.02151},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/NSSWBWJE/Fusillo et al. - 2017 - Can magnetic fields suppress convection in the atm.pdf;/Users/Oliver/Zotero/storage/XZ8762EA/1710.html},
  journal = {arXiv:1710.02151 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{gai+2011,
  title = {An In-Depth Study of Grid-Based Asteroseismic Analysis},
  author = {Gai, Ning and Basu, Sarbani and Chaplin, William J. and Elsworth, Yvonne},
  year = {2011},
  month = apr,
  volume = {730},
  pages = {63},
  issn = {0004-637X, 1538-4357},
  doi = {10.1088/0004-637X/730/2/63},
  abstract = {NASA's Kepler mission is providing basic asteroseismic data for hundreds of stars. One of the more common ways of determining stellar characteristics from these data is by the so-called grid-based modeling. We have made a detailed study of grid-based analysis techniques to study the errors (and error correlations) involved. As had been reported earlier, we find that it is relatively easy to get very precise values of stellar radii using grid-based techniques. However, we find that there are small, but significant, biases that can result because of the grid of models used. The biases can be minimized if metallicity is known. Masses cannot be determined as precisely as the radii and suffer from larger systematic effects. We also find that the errors in mass and radius are correlated. A positive consequence of this correlation is that log g can be determined both precisely and accurately with almost no systematic biases. Radii and log g can be determined with almost no model dependence to within 5\% for realistic estimates of errors in asteroseismic and conventional observations. Errors in mass can be somewhat higher unless accurate metallicity estimates are available. Age estimates of individual stars are the most model dependent. The errors are larger, too. However, we find that for star clusters, it is possible to get a relatively precise age if one assumes that all stars in a given cluster have the same age.},
  file = {/Users/Oliver/Zotero/storage/IXMTFSIV/Gai et al. - 2011 - AN IN-DEPTH STUDY OF GRID-BASED ASTEROSEISMIC ANAL.pdf},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{gaiacollaboration+2016,
  title = {Gaia {{Data Release}} 1. {{Summary}} of the Astrometric, Photometric, and Survey Properties},
  author = {{Gaia Collaboration} and Brown, A. G. A. and Vallenari, A. and Prusti, T. and {de Bruijne}, J. and Mignard, F. and Drimmel, R. and {co-authors}, 585},
  year = {2016},
  month = nov,
  volume = {595},
  pages = {A2},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201629512},
  abstract = {At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. We summarize Gaia DR1 and provide illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. Gaia DR1 consists of: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the Hipparcos and Tycho-2 catalogues and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set,consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of \textasciitilde 3000 Cepheid and RR Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas/yr for the proper motions. A systematic component of \textasciitilde 0.3 mas should be added to the parallax uncertainties. For the subset of \textasciitilde 94000 Hipparcos stars in the primary data set, the proper motions are much more precise at about 0.06 mas/yr. For the secondary astrometric data set, the typical uncertainty of the positions is \textasciitilde 10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to \textasciitilde 0.03 mag over the magnitude range 5 to 20.7. Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data.},
  archivePrefix = {arXiv},
  eprint = {1609.04172},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/7CKHCN69/Gaia Collaboration et al. - 2016 - Gaia Data Release 1. Summary of the astrometric, p.pdf;/Users/Oliver/Zotero/storage/H8FK7CF2/1609.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics - Instrumentation and Methods for Astrophysics}
}

@article{gaiacollaboration+2018,
  title = {Gaia {{Data Release}} 2. {{Summary}} of the Contents and Survey Properties},
  author = {{Gaia Collaboration} and Brown, A. G. A. and Vallenari, A. and Prusti, T. and Bruijne, De and J, J. H. and Babusiaux, C. and {Bailer-Jones}, C. a. L.},
  year = {2018},
  month = apr,
  pages = {arXiv:1804.09365},
  abstract = {We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the \$G\_\textbackslash mathrm\{BP\}\$ (330--680 nm) and \$G\_\textbackslash mathrm\{RP\}\$ (630--1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent.},
  file = {/Users/Oliver/Zotero/storage/YMF9ZE7B/Collaboration et al. - 2018 - Gaia Data Release 2. Summary of the contents and s.pdf;/Users/Oliver/Zotero/storage/B5MCICD8/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{gallet+delorme2019,
  title = {Star-Planet Tidal Interaction and the Limits of Gyrochronology},
  author = {Gallet, Florian and Delorme, Philippe},
  year = {2019},
  month = may,
  volume = {1905},
  pages = {arXiv:1905.06070},
  abstract = {Age estimation techniques such as gyrochronology and magnetochronology can't be applied to stars that exchanged angular momentum with their close environment. This is especially true for massive close-in
planetary companion (with a periods of few days or less), which could have been strongly impacted the rotational evolution of the host star, along the stellar evolution, through the star-planet tidal interaction. We showed that the interaction of a close-in massive planet with its host star can strongly modify the surface rotation rate of this latter, in most of the cases associated to a planetary engulfment. In such cases, a gyrochronology analysis of the star would wrongly make it appear as "rejuvenated", thus preventing us to use this method with confidence. To try overcome this issue, we eventually proposed the proof of concept of a new age determination technique that we call the tidal-chronology, which is based on the observed couple \$\textbackslash rm
P\_\{rot,\textbackslash star\}\$-\$\textbackslash rm P\_\{orb\}\$ of a given star-planet system. The
gyrochronology technique can only be applied to isolated star or star-planet systems outside a specific range of \$\textbackslash rm P\_\{rot,\textbackslash star\}\$-\$\textbackslash rm P\_\{orb\}\$. This region tends to expand for increasing stellar and planetary mass. In that forbidden region, or if any planetary engulfment is suspected, gyrochronology should be used with extreme caution while tidal-chronology could be considered. While this technique does not provide a precise age for the system yet, it is already an extension of gyrochronology and could be helpful to determine a more precise range of possible age for planetary system composed of a star between 0.3 and 1.2 \$M\_\{\textbackslash odot\}\$ and a planet more massive than 1 \$\textbackslash rm M\_\{jup\}\$ initially located at few hundredth au of the host star.},
  journal = {arXiv e-prints},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics}
}

@article{garcia+2004,
  title = {About the Rotation of the Solar Radiative Interior},
  author = {Garc{\'i}a, R. A. and Corbard, T. and Chaplin, W. J. and Couvidat, S. and {Eff-Darwich}, A. and {Jim{\'e}nez-Reyes}, S. J. and Korzennik, S. G. and Ballot, J. and Boumier, P. and Fossat, E. and Henney, C. J. and Howe, R. and Lazrek, M. and Lochard, J. and Pall{\'e}, P. L. and {Turck-Chi{\`e}ze}, S.},
  year = {2004},
  month = apr,
  volume = {220},
  pages = {269--285},
  issn = {0038-0938},
  doi = {10.1023/B:SOLA.0000031395.90891.ce},
  abstract = {In the modern era of helioseismology we have a wealth of high-quality data available, e.g., more than 6 years of data collected by the various instruments on board the SOHO mission, and an even more extensive ground-based set of observations covering a full solar cycle. Thanks to this effort a detailed picture of the internal rotation of the Sun has been constructed. In this paper we present some of the actions that should be done to improve our knowledge of the inner rotation profile discussed during the workshop organized at Saclay on June 2003 on this topic. In particular we will concentrate on the extraction of the rotational frequency splittings of low- and medium-degree modes and their influence on the rotation of deeper layers. Furthermore, for the first time a full set of individual |m|-component rotational splittings is computed for modes {$\mathscr{l}\leq$}4 and 1{$<\nu<$}2 mHz, opening new
studies on the latitudinal dependence of the rotation rate in the radiative interior. It will also be shown that these splittings have the footprints of the differential rotation of the convective zone which can be extremely useful to study the differential rotation of other stars where only these low-degree modes will be available.},
  journal = {Solar Physics}
}

@article{garcia+2007,
  title = {Tracking {{Solar Gravity Modes}}: {{The Dynamics}} of the {{Solar Core}}},
  shorttitle = {Tracking {{Solar Gravity Modes}}},
  author = {Garc{\'i}a, Rafael A. and {Turck-Chi{\`e}ze}, Sylvaine and {Jim{\'e}nez-Reyes}, Sebastian J. and Ballot, J{\'e}r{\^o}me and Pall{\'e}, Pere L. and {Eff-Darwich}, Antonio and Mathur, Savita and Provost, Janine},
  year = {2007},
  month = jun,
  volume = {316},
  pages = {1591},
  issn = {0036-8075},
  doi = {10.1126/science.1140598},
  abstract = {Solar gravity modes have been actively sought because they directly probe the solar core (below 0.2 solar radius), but they have not been conclusively detected in the Sun because of their small surface
amplitudes. Using data from the Global Oscillation at Low Frequency instrument, we detected a periodic structure in agreement with the period separation predicted by the theory for gravity dipole modes. When studied in relation to simulations including the best physics of the Sun determined through the acoustic modes, such a structure favors a faster rotation rate in the core than in the rest of the radiative zone.},
  file = {/Users/Oliver/Zotero/storage/F2A295HY/García et al. - 2007 - Tracking Solar Gravity Modes The Dynamics of the .pdf},
  journal = {Science}
}

@article{garcia+2008,
  title = {Influence of {{Low}}-{{Degree High}}-{{Order}} p-{{Mode Splittings}} on the {{Solar Rotation Profile}}},
  author = {Garc{\'i}a, R. A. and Mathur, S. and Ballot, J. and {Eff-Darwich}, A. and {Jim{\'e}nez-Reyes}, S. J. and Korzennik, S. G.},
  year = {2008},
  month = sep,
  volume = {251},
  pages = {119--133},
  issn = {0038-0938},
  doi = {10.1007/s11207-008-9144-5},
  abstract = {The solar rotation profile is well constrained down to about 0.25 R
{$\odot$} thanks to the study of acoustic modes. Since the radius
of the inner turning point of a resonant acoustic mode is inversely
proportional to the ratio of its frequency to its degree, only the
low-degree p modes reach the core. The higher the order of these modes,
the deeper they penetrate into the Sun and thus they carry more
diagnostic information on the inner regions. Unfortunately, the
estimates of frequency splittings at high frequency from Sun-as-a-star
measurements have higher observational errors because of mode blending,
resulting in weaker constraints on the rotation profile in the inner
core. Therefore inversions for the solar internal rotation use only
modes below 2.4 mHz for {$\mathscr{l}\leq$}3. In the work presented here, we used
an 11.5-year-long time series to compute the rotational frequency
splittings for modes {$\mathscr{l}\leq$}3 using velocities measured with the GOLF
instrument. We carried out a theoretical study of the influence of the
low-degree modes in the region from 2 to 3.5 mHz on the inferred
rotation profile as a function of their error bars.},
  file = {/Users/Oliver/Zotero/storage/V2YJ367Z/García et al. - 2008 - Influence of Low-Degree High-Order p-Mode Splittin.pdf},
  journal = {Solar Physics},
  keywords = {Core,Helioseismology,Interior,Inverse modeling,Observations,Radiative zone,Rotation}
}

@article{garcia+2011,
  title = {Preparation of {{Kepler}} Light Curves for Asteroseismic Analyses},
  author = {Garc{\'i}a, R. A. and Hekker, S. and Stello, D. and {Guti{\'e}rrez-Soto}, J. and Handberg, R. and Huber, D. and Karoff, C. and Uytterhoeven, K. and Appourchaux, T. and Chaplin, W. J. and Elsworth, Y. and Mathur, S. and Ballot, J. and {Christensen-Dalsgaard}, J. and Gilliland, R. L. and Houdek, G. and Jenkins, J. M. and Kjeldsen, H. and McCauliff, S. and Metcalfe, T. and Middour, C. K. and {Molenda-Zakowicz}, J. and Monteiro, M. J. P. F. G. and Smith, J. C. and Thompson, M. J.},
  year = {2011},
  month = jun,
  volume = {414},
  pages = {L6-L10},
  issn = {0035-8711},
  doi = {10.1111/j.1745-3933.2011.01042.x},
  abstract = {The Kepler mission is providing photometric data of exquisite quality for the asteroseismic study of different classes of pulsating stars. These analyses place particular demands on the pre-processing of the data, over a range of time-scales from minutes to months. Here, we describe processing procedures developed by the Kepler Asteroseismic Science Consortium to prepare light curves that are optimized for the asteroseismic study of solar-like oscillating stars in which outliers, jumps and drifts are corrected.},
  file = {/Users/Oliver/Zotero/storage/6DCHZZSZ/García et al. - 2011 - Preparation of Kepler light curves for asteroseism.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,methods: data analysis}
}

@article{garcia+2014,
  title = {Rotation and Magnetism of {{Kepler}} Pulsating Solar-like Stars. {{Towards}} Asteroseismically Calibrated Age-Rotation Relations},
  author = {Garc{\'i}a, R. A. and Ceillier, T. and Salabert, D. and Mathur, S. and {van Saders}, J. L. and Pinsonneault, M. and Ballot, J. and Beck, P. G. and Bloemen, S. and Campante, T. L. and Davies, G. R. and {do Nascimento}, J.-D. and Mathis, S. and Metcalfe, T. S. and Nielsen, M. B. and Su{\'a}rez, J. C. and Chaplin, W. J. and Jim{\'e}nez, A. and Karoff, C.},
  year = {2014},
  month = dec,
  volume = {572},
  pages = {A34},
  doi = {10.1051/0004-6361/201423888},
  abstract = {Kepler ultra-high precision photometry of long and continuous observations provides a unique dataset in which surface rotation and variability can be studied for thousands of stars. Because many of these old field stars also have independently measured asteroseismic ages, measurements of rotation and activity are particularly interesting in the context of age-rotation-activity relations. In particular, age-rotation relations generally lack good calibrators at old ages, a problem that this Kepler sample of old-field stars is uniquely suited to address. We study the surface rotation and photometric magnetic activity of a subset of 540 solar-like stars on the main-sequence and the subgiant branch for which stellar pulsations have been measured. The rotation period was determined by comparing the results from two different analysis methods: i) the projection onto the frequency domain of the time-period analysis, and ii) the autocorrelation function of the light curves. Reliable surface rotation rates were then extracted by comparing the results from two different sets of calibrated data and from the two complementary analyses. General photometric levels of magnetic activity in this sample of stars were also extracted by using a photometric activity index, which takes into account the rotation period of the stars. We report rotation periods for 310 out of 540 targets (excluding known binaries and candidate planet-host stars); our measurements span a range of 1 to 100 days. The photometric magnetic activity levels of these stars were computed, and for 61.5\% of the dwarfs, this level is similar to the range, from minimum to maximum, of the solar magnetic activity. We demonstrate that hot dwarfs, cool dwarfs, and subgiants have very different rotation-age relationships, highlighting the importance of separating out distinct populations when interpreting stellar rotation periods. Our sample of cool dwarf stars with age and metallicity data of the highest quality is consistent with gyrochronology relations reported in the literature. Full Table 3 is only available at the CDS via anonymous ftp to \href{http://cdsarc.u-strasbg.fr}{http://cdsarc.u-strasbg.fr} (ftp://130.79.128.5) or via \href{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/572/A34}{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/572/A34}},
  file = {/Users/Oliver/Zotero/storage/TFT3I2J2/García et al. - 2014 - Rotation and magnetism of Kepler pulsating solar-l.pdf;/Users/Oliver/Zotero/storage/L2HJKFEB/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  keywords = {Core Gyrochronology,Seismic rotation},
  language = {en}
}

@article{garcia+2014a,
  title = {Impact on Asteroseismic Analyses of Regular Gaps in {{Kepler}} Data},
  author = {Garc{\'i}a, R. A. and Mathur, S. and Pires, S. and R{\'e}gulo, C. and Bellamy, B. and Pall{\'e}, P. L. and Ballot, J. and Barcel{\'o} Forteza, S. and Beck, P. G. and Bedding, T. R. and Ceillier, T. and Roca Cort{\'e}s, T. and Salabert, D. and Stello, D.},
  year = {2014},
  month = aug,
  volume = {568},
  pages = {A10},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201323326},
  abstract = {Context. The NASA Kepler mission has observed more than 190 000 stars in the constellations of Cygnus and Lyra. Around 4 years of almost
continuous ultra high-precision photometry have been obtained reaching a duty cycle higher than 90\% for many of these stars. However, almost regular gaps due to nominal operations are present in the light curves on different time scales. Aims: In this paper we want to
highlight the impact of those regular gaps in asteroseismic analyses, and we try to find a method that minimizes their effect on the frequency domain. Methods: To do so, we isolate the two main time scales of quasi regular gaps in the data. We then interpolate the gaps and compare the power density spectra of four different stars: two red giants at different stages of their evolution, a young F-type star, and a
classical pulsator in the instability strip. Results: The spectra obtained after filling the gaps in the selected solar-like stars show a net reduction in the overall background level, as well as a change in the background parameters. The inferred convective properties could change as much as \textasciitilde 200\% in the selected example, introducing a bias in the p-mode frequency of maximum power. When asteroseismic scaling relations are used, this bias can lead to a variation in the surface gravity of 0.05 dex. Finally, the oscillation spectrum in the classical pulsator is cleaner than the original one.},
  file = {/Users/Oliver/Zotero/storage/BPWXW7A3/García et al. - 2014 - Impact on asteroseismic analyses of regular gaps i.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {asteroseismology,methods: data analysis,stars: oscillations}
}

@article{garcia+ballot2019,
  title = {Asteroseismology of Solar-Type Stars},
  author = {Garcia, R. A. and Ballot, J.},
  year = {2019},
  month = dec,
  volume = {16},
  pages = {4},
  issn = {2367-3648, 1614-4961},
  doi = {10.1007/s41116-019-0020-1},
  abstract = {Until the last few decades, investigations of stellar interiors had been restricted to theoretical studies only constrained by observations of their global properties and external characteristics. However, in the last thirty years the field has been revolutionized by the ability to perform seismic investigations of stellar interiors. This revolution begun with the Sun, where helioseismology has been yielding information competing with what can be inferred about the Earth's interior from geoseismology. The last two decades have witnessed the advent of asteroseismology of solar-like stars, thanks to a dramatic development of new observing facilities providing the first reliable results on the interiors of distant stars. The coming years will see a huge development in this field. In this review we focus on solar-type stars, i.e., cool main-sequence stars where oscillations are stochastically excited by surface convection. After a short introduction and a historical overview of the discipline, we review the observational techniques generally used, and we describe the theory behind stellar oscillations in cool main-sequence stars. We continue with a complete description of the normal mode analyses through which it is possible to extract the physical information about the structure and dynamics of the stars. We then summarize the lessons that we have learned and discuss unsolved issues and questions that are still unanswered.},
  archivePrefix = {arXiv},
  eprint = {1906.12262},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/GV9URBMJ/Garcia and Ballot - 2019 - Asteroseismology of solar-type stars.pdf;/Users/Oliver/Zotero/storage/WE63B9HU/1906.html},
  journal = {Living Reviews in Solar Physics},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{garraffo+2016,
  title = {The {{Missing Magnetic Morphology Term}} in {{Stellar Rotation Evolution}}},
  author = {Garraffo, Cecilia and Drake, Jeremy J. and Cohen, Ofer},
  year = {2016},
  month = nov,
  volume = {595},
  pages = {A110},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201628367},
  abstract = {This study examines the relationship between magnetic field complexity and mass and angular momentum losses. Observations of open clusters have revealed a bimodal distribution of the rotation periods of solar-like stars that has proven difficult to explain under the existing rubric of magnetic braking. Recent studies suggest that magnetic complexity can play an important role in controlling stellar spin-down rates. However, magnetic morphology is still neglected in most rotation evolution models due to the difficulty of properly accounting for its effects on wind driving and angular momentum loss. Using state-of-the-art magnetohydrodynamical magnetized wind simulations we study the effect that different distributions of the magnetic flux at different levels of geometrical complexity have on mass and angular momentum loss rates. Angular momentum loss rates depend strongly on the level of complexity of the field but are independent of the way this complexity is distributed. We deduce the analytical terms representing the magnetic field morphology dependence of mass and angular momentum loss rates. We also define a parameter that best represents complexity for real stars. As a test, we use these analytical methods to estimate mass and angular momentum loss rates for \$8\$ stars with observed magnetograms and compare them to the simulated results. Magnetic field complexity provides a natural physical basis for stellar rotation evolution models requiring a rapid transition between weak and strong spin-down modes.},
  archivePrefix = {arXiv},
  eprint = {1607.06096},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/DATKBQQ6/Garraffo et al. - 2016 - The Missing Magnetic Morphology Term in Stellar Ro.pdf;/Users/Oliver/Zotero/storage/8YEGPU44/1607.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{garraffo+2018,
  title = {The {{Revolution Revolution}}: {{Magnetic Morphology Driven Spin}}-Down},
  shorttitle = {The {{Revolution Revolution}}},
  author = {Garraffo, C. and Drake, J. J. and Dotter, A. and Choi, J. and Burke, D. J. and Moschou, S. P. and {Alvarado-G{\'o}mez}, J. D. and Kashyap, V. L. and Cohen, O.},
  year = {2018},
  month = jul,
  volume = {862},
  pages = {90},
  doi = {10.3847/1538-4357/aace5d},
  abstract = {Observations of young open clusters (OCs) show a bimodal distribution of rotation periods that has been difficult to explain with existing stellar spin-down models. Detailed magnetohydrodynamic (MHD) stellar wind simulations have demonstrated that surface magnetic field morphology has a strong influence on wind-driven angular momentum loss. Observations suggest that faster rotating stars store a larger fraction of their magnetic flux in higher-order multipolar components of the magnetic field. In this work, we present an entirely predictive new model for stellar spin-down that accounts for the stellar surface magnetic field configuration. We show how a magnetic complexity that evolves from complex toward simple configurations as a star spins down can explain the salient features of stellar rotation evolution, including the bimodal distribution of both slow and fast rotators seen in young OCs. Title inspired by C. L. Davis PhD Thesis Revolution evolution: tracing angular momentum during star and planetary system formation, St. Andrews University.},
  file = {/Users/Oliver/Zotero/storage/RH9HFYNI/Garraffo et al. - 2018 - The Revolution Revolution Magnetic Morphology Dri.pdf;/Users/Oliver/Zotero/storage/RVPBA6SF/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{gaulme+2016,
  title = {A {{Distant Mirror}}: {{Solar Oscillations Observed}} on {{Neptune}} by the {{Kepler K2 Mission}}},
  shorttitle = {A {{Distant Mirror}}},
  author = {Gaulme, P. and Rowe, J. F. and Bedding, T. R. and Benomar, O. and Corsaro, E. and Davies, G. R. and Hale, S. J. and Howe, R. and Garcia, R. A. and Huber, D. and Jim{\'e}nez, A. and Mathur, S. and Mosser, B. and Appourchaux, T. and Boumier, P. and Jackiewicz, J. and Leibacher, J. and Schmider, F.-X. and Hammel, H. B. and Lissauer, J. J. and Marley, M. S. and Simon, A. A. and Chaplin, W. J. and Elsworth, Y. and Guzik, J. A. and Murphy, N. and Aguirre, V. Silva},
  year = {2016},
  month = dec,
  volume = {833},
  pages = {L13},
  issn = {2041-8213},
  doi = {10.3847/2041-8213/833/1/L13},
  abstract = {Starting in December 2014, Kepler K2 observed Neptune continuously for 49 days at a 1-minute cadence. The goals consisted of studying its atmospheric dynamics (Simon et al. 2016), detecting its global acoustic oscillations (Rowe et al., submitted), and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude "nu\_max" and the mean frequency separation between mode overtones "Delta nu", is surprising as the nu\_max measured from Neptune photometry is larger than the accepted value. Compared to the usual reference nu\_max\_sun = 3100 muHz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 +/- 5.8 \% and 4.3 +/- 1.9 \% respectively. The higher nu\_max is caused by a combination of the value of nu\_max\_sun, being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 +/- 10 muHz), and the noise level of the K2 time series, being ten times larger than VIRGO's. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (SNR), we model ten overtones for degrees l=0,1,2. We compare the K2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1 sigma, except for the few peaks with lowest SNR.},
  archivePrefix = {arXiv},
  eprint = {1612.04287},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/P4BBV3NP/Gaulme et al. - 2016 - A Distant Mirror Solar Oscillations Observed on N.pdf;/Users/Oliver/Zotero/storage/SA2PS3TW/1612.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{gaulme+2016a,
  title = {Testing the {{Asteroseismic Scaling Relations}} for {{Red Giants}} with {{Eclipsing Binaries Observed}} by {{Kepler}}},
  author = {Gaulme, P. and McKeever, J. and Jackiewicz, J. and Rawls, M. L. and Corsaro, E. and Mosser, B. and Southworth, J. and Mahadevan, S. and Bender, C. and Deshpande, R.},
  year = {2016},
  month = dec,
  volume = {832},
  pages = {121},
  doi = {10.3847/0004-637X/832/2/121},
  abstract = {Given the potential of ensemble asteroseismology for understanding fundamental properties of large numbers of stars, it is critical to determine the accuracy of the scaling relations on which these measurements are based. From several powerful validation techniques, all indications so far show that stellar radius estimates from the asteroseismic scaling relations are accurate to within a few percent. Eclipsing binary systems hosting at least one star with detectable solar-like oscillations constitute the ideal test objects for validating asteroseismic radius and mass inferences. By combining radial velocity (RV) measurements and photometric time series of eclipses, it is possible to determine the masses and radii of each component of a double-lined spectroscopic binary. We report the results of a four-year RV survey performed with the \'echelle spectrometer of the Astrophysical Research Consortium's 3.5 m telescope and the APOGEE spectrometer at Apache Point Observatory. We compare the masses and radii of 10 red giants (RGs) obtained by combining radial velocities and eclipse photometry with the estimates from the asteroseismic scaling relations. We find that the asteroseismic scaling relations overestimate RG radii by about 5\% on average and masses by about 15\% for stars at various stages of RG evolution. Systematic overestimation of mass leads to underestimation of stellar age, which can have important implications for ensemble asteroseismology used for Galactic studies. As part of a second objective, where asteroseismology is used for understanding binary systems, we confirm that oscillations of RGs in close binaries can be suppressed enough to be undetectable, a hypothesis that was proposed in a previous work.},
  file = {/Users/Oliver/Zotero/storage/8RQUMSCQ/Gaulme et al. - 2016 - Testing the Asteroseismic Scaling Relations for Re.pdf;/Users/Oliver/Zotero/storage/QQFLKSQI/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{gehan+2017,
  title = {Large-Scale Measurements of the Red Giant Core Rotation through Asteroseismology},
  author = {Gehan, Charlotte and Mosser, Beno{\^i}t and Michel, Eric},
  year = {2017},
  month = oct,
  abstract = {Red giant stars are solar-like pulsators presenting mixed-modes. Such modes consist in a coupling between pressure waves propagating in the external convective envelope and gravity waves propagating in the radiative interior. Therefore, the red giant asteroseismology provides us with a direct view on their core and opens the possibility to monitor the evolution of their core rotation. Previous measurements of the mean core rotation revealed that angular momentum is efficiently transferred from the core to the envelope inside red giants, but the physical mechanisms at work are not yet fully understood. We thus need stronger observational constraints on the evolution of the red giant core rotation. In this context, we developed an automated method to determine the mean core rotation of red giant branch stars observed with Kepler. This automated method is paving the way for the future PLATO data, representing hundreds of thousands of potential red giant oscillation spectra. Results obtained for almost 1200 red giant branch stars indicate that the rate of the core rotation braking is lower than previously estimated and does not seem to depend on the stellar mass.},
  archivePrefix = {arXiv},
  eprint = {1710.05647},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/U3C2A5K9/Gehan et al. - 2017 - Large-scale measurements of the red giant core rot.pdf;/Users/Oliver/Zotero/storage/W95BZQ5I/1710.html},
  journal = {arXiv:1710.05647 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@inproceedings{gelly+1988,
  title = {Helioseismology from the {{South Pole The}} 1984/85 Campaign},
  booktitle = {Advances in {{Helio}}- and {{Asteroseismology}}},
  author = {Gelly, B. and Fossat, E. and Grec, G. and Pomerantz, M.},
  editor = {{Christensen-Dalsgaard}, J{\o}rgen and Frandsen, S{\o}ren},
  year = {1988},
  pages = {21--23},
  publisher = {{Springer Netherlands}},
  address = {{Dordrecht}},
  doi = {10.1007/978-94-009-4009-3_2},
  abstract = {More than 700 hours of full disk line of sight solar velocity have been recorded at the Geographic South Pole between late november 1984 and early february 1985. This paper presents very briefly some preliminary result of the analysis of this data.Between November 27, 1984 and February 1, 1985, almost continuous data have been recorded at the geographic south pole with our sodium cell full disk spectrophotometer, in which 704 hours have been selected for analysis. That makes a duty cycle of about 45H, which itself makes of this season a reasonably good one. A complete week of extremely good sky was missed, we could almost say as usually, as the beginning of the season before we could be ready.},
  isbn = {978-94-009-4009-3},
  keywords = {Duty Cycle,Power Spectrum,Solar Phys,South Pole,Window Function},
  language = {en},
  series = {International {{Astronomical Union}} / {{Union Astronomique Internationale}}}
}

@article{gelman+rubin1992,
  title = {Inference from {{Iterative Simulation Using Multiple Sequences}}},
  author = {Gelman, Andrew and Rubin, Donald B.},
  year = {1992},
  volume = {7},
  pages = {457--472},
  doi = {10.1214/ss/1177011136},
  abstract = {The Gibbs sampler, the algorithm of Metropolis and similar iterative simulation methods are potentially very helpful for summarizing
multivariate distributions. Used naively, however, iterative simulation can give misleading answers. Our methods are simple and generally applicable to the output of any iterative simulation; they are designed for researchers primarily interested in the science underlying the data and models they are analyzing, rather than for researchers interested in the probability theory underlying the iterative simulations themselves. Our recommended strategy is to use several independent sequences, with starting points sampled from an overdispersed distribution. At each step of the iterative simulation, we obtain, for each univariate estimand of interest, a distributional estimate and an estimate of how much sharper the distributional estimate might become if the simulations were continued indefinitely. Because our focus is on applied inference for Bayesian posterior distributions in real problems, which often tend toward normality after transformations and marginalization, we derive our results as normal-theory approximations to exact Bayesian inference, conditional on the observed simulations. The methods are illustrated on a random-effects mixture model applied to experimental measurements of reaction times of normal and schizophrenic patients.},
  file = {/Users/Oliver/Zotero/storage/VBLP3U7A/Gelman and Rubin - 1992 - Inference from Iterative Simulation Using Multiple.pdf},
  journal = {Statistical Science}
}

@article{gelman2006,
  title = {Prior Distributions for Variance Parameters in Hierarchical Models (Comment on Article by {{Browne}} and {{Draper}})},
  author = {Gelman, Andrew},
  year = {2006},
  month = sep,
  volume = {1},
  pages = {515--534},
  publisher = {{International Society for Bayesian Analysis}},
  issn = {1936-0975, 1931-6690},
  doi = {10.1214/06-BA117A},
  abstract = {Various noninformative prior distributions have been suggested for scale parameters in hierarchical models. We construct a new folded-noncentral-ttt family of conditionally conjugate priors for hierarchical standard deviation parameters, and then consider noninformative and weakly informative priors in this family. We use an example to illustrate serious problems with the inverse-gamma family of "noninformative" prior distributions. We suggest instead to use a uniform prior on the hierarchical standard deviation, using the half-ttt family when the number of groups is small and in other settings where a weakly informative prior is desired. We also illustrate the use of the half-ttt family for hierarchical modeling of multiple variance parameters such as arise in the analysis of variance.},
  file = {/Users/Oliver/Zotero/storage/2YU4JKLI/Gelman - 2006 - Prior distributions for variance parameters in hie.pdf;/Users/Oliver/Zotero/storage/H95UBQJJ/1340371048.html},
  journal = {Bayesian Analysis},
  keywords = {Bayesian inference,conditional conjugacy,folded-noncentral-$t$ distribution,half-$t$ distribution,hierarchical model,multilevel model,noninformative prior distribution,weakly informative prior distribution},
  language = {EN},
  mrnumber = {MR2221284},
  number = {3},
  zmnumber = {1331.62139}
}

@article{giammichele+2016,
  title = {Toward {{High Precision Seismic Studies}} of {{White Dwarf Stars}}: {{Parametrization}} of the {{Core}} and {{Tests}} of {{Accuracy}}},
  shorttitle = {Toward {{High Precision Seismic Studies}} of {{White Dwarf Stars}}},
  author = {Giammichele, N. and Charpinet, S. and Fontaine, G. and Brassard, P.},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/9CGF69TZ/1610.06036v1.pdf},
  journal = {arXiv preprint arXiv:1610.06036}
}

@article{giammichele+2016a,
  title = {The Potential of Asteroseismology for Probing the Core Chemical Stratification in White Dwarf Stars},
  author = {Giammichele, N. and Charpinet, S. and Brassard, P. and G and Fontaine},
  year = {2016},
  month = nov,
  abstract = {Context. The details of the C/O core structure in white dwarf stars has mostly remained inaccessible to the technique of asteroseismology, despite several attempts carried out in the past. Aims. We re-assess the potential of asteroseismology for probing the chemical stratification in white dwarf cores, in light of new highly efficient tools recently developed for that purpose. Methods. Using the forward modeling approach and a new parameterization for the core chemical stratification in ZZ Ceti stars, we test several situations typical of the usually limited constraints available, such as small numbers of observed independent modes, to carry out asteroseismology of these stars. Results. We find that, even with a limited number of modes, the core chemical stratification (in particular, the location of the steep chemical transitions expected in the oxygen profile) can be determined quite precisely due to the significant sensitivity of some confined modes to partial reflexion (trapping) effects. These effects are similar to the well known trapping induced by the shallower chemical transitions at the edge of the core and at the bottom of the H-rich envelope. We also find that success to unravel the core structure depends on the information content of the available seismic data. In some cases, it may not be possible to isolate a unique, well-defined seismic solution and the problem remains degenerate. Conclusions. Our results establish that constraining the core chemical stratification in white dwarf stars based solely on asteroseismology is possible, an opportunity that we have started to exploit.},
  archivePrefix = {arXiv},
  eprint = {1611.05071},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/XNSTH3B4/Giammichele et al. - 2016 - The potential of asteroseismology for probing the .pdf;/Users/Oliver/Zotero/storage/JETN7MVD/1611.html},
  journal = {arXiv:1611.05071 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{gillen+2016,
  title = {{{CoRoT}} 223992193: {{Investigating}} the Variability in a Low-Mass, Pre-Main Sequence Eclipsing Binary with Evidence of a Circumbinary Disk},
  shorttitle = {{{CoRoT}} 223992193},
  author = {Gillen, E. and Aigrain, S. and Terquem, C. and Bouvier, J. and Alencar, S. H. P. and Gandolfi, D. and Stauffer, J. and Cody, A. and Venuti, L. and Almeida, P. Viana and others},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/F73M5QTW/1611.05461v1.pdf},
  journal = {Astronomy \& Astrophysics}
}

@article{gillon+2017,
  title = {Seven Temperate Terrestrial Planets around the Nearby Ultracool Dwarf Star {{TRAPPIST}}-1},
  author = {Gillon, Michael and Triaud, Amaury H. M. J. and Demory, Brice-Olivier and Jehin, Emmanuel and Agol, Eric and Deck, Katherine M. and Lederer, Susan M. and {de Wit}, Julien and Burdanov, Artem and Ingalls, James G. and Bolmont, Emeline and Leconte, Jeremy and Raymond, Sean N. and Selsis, Franck and Turbet, Martin and Barkaoui, Khalid and Burgasser, Adam and Burleigh, Matthew R. and Carey, Sean J. and Chaushev, Aleksander and Copperwheat, Chris M. and Delrez, Laetitia and Fernandes, Catarina S. and Holdsworth, Daniel L. and Kotze, Enrico J. and Van Grootel, Valerie and Almleaky, Yaseen and Benkhaldoun, Zouhair and Magain, Pierre and Queloz, Didier},
  year = {2017},
  month = feb,
  volume = {542},
  pages = {456--460},
  issn = {0028-0836, 1476-4687},
  doi = {10.1038/nature21360},
  abstract = {One focus of modern astronomy is to detect temperate terrestrial exoplanets well-suited for atmospheric characterisation. A milestone was recently achieved with the detection of three Earth-sized planets transiting (i.e. passing in front of) a star just 8\% the mass of the Sun 12 parsecs away. Indeed, the transiting configuration of these planets with the Jupiter-like size of their host star - named TRAPPIST-1 - makes possible in-depth studies of their atmospheric properties with current and future astronomical facilities. Here we report the results of an intensive photometric monitoring campaign of that star from the ground and with the Spitzer Space Telescope. Our observations reveal that at least seven planets with sizes and masses similar to the Earth revolve around TRAPPIST-1. The six inner planets form a near-resonant chain such that their orbital periods (1.51, 2.42, 4.04, 6.06, 9.21, 12.35 days) are near ratios of small integers. This architecture suggests that the planets formed farther from the star and migrated inward. The seven planets have equilibrium temperatures low enough to make possible liquid water on their surfaces.},
  archivePrefix = {arXiv},
  eprint = {1703.01424},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/5IJPBB3Z/Gillon et al. - 2017 - Seven temperate terrestrial planets around the nea.pdf;/Users/Oliver/Zotero/storage/9FPZU8A7/1703.html},
  journal = {Nature},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  number = {7642}
}

@article{gilmore+2012,
  title = {The {{Gaia}}-{{ESO Public Spectroscopic Survey}}},
  author = {Gilmore, G. and Randich, S. and Asplund, M. and Binney, J. and Bonifacio, P. and Drew, J. and Feltzing, S. and Ferguson, A. and Jeffries, R. and Micela, G. and Negueruela, I. and Prusti, T. and Rix, H.-W. and Vallenari, A. and Alfaro, E. and {Allende-Prieto}, C. and Babusiaux, C. and Bensby, T. and Blomme, R. and Bragaglia, A. and Flaccomio, E. and Fran{\c c}ois, P. and Irwin, M. and Koposov, S. and Korn, A. and Lanzafame, A. and Pancino, E. and Paunzen, E. and {Recio-Blanco}, A. and Sacco, G. and Smiljanic, R. and Van Eck, S. and Walton, N. and Aden, D. and Aerts, C. and Affer, L. and Alcala, J.-M. and Altavilla, G. and Alves, J. and Antoja, T. and Arenou, F. and Argiroffi, C. and Asensio Ramos, A. and {Bailer-Jones}, C. and {Balaguer-Nunez}, L. and Bayo, A. and Barbuy, B. and Barisevicius, G. and {Barrado y Navascues}, D. and Battistini, C. and Bellas Velidis, I. and Bellazzini, M. and Belokurov, V. and Bergemann, M. and Bertelli, G. and Biazzo, K. and Bienayme, O. and {Bland-Hawthorn}, J. and Boeche, C. and Bonito, S. and Boudreault, S. and Bouvier, J. and Brandao, I. and Brown, A. and {de Bruijne}, J. and Burleigh, M. and Caballero, J. and Caffau, E. and Calura, F. and {Capuzzo-Dolcetta}, R. and Caramazza, M. and Carraro, G. and Casagrande, L. and Casewell, S. and Chapman, S. and Chiappini, C. and Chorniy, Y. and Christlieb, N. and Cignoni, M. and Cocozza, G. and Colless, M. and Collet, R. and Collins, M. and Correnti, M. and Covino, E. and Crnojevic, D. and Cropper, M. and Cunha, M. and Damiani, F. and David, M. and Delgado, A. and Duffau, S. and Edvardsson, B. and Eldridge, J. and Enke, H. and Eriksson, K. and Evans, N. W. and Eyer, L. and Famaey, B. and Fellhauer, M. and Ferreras, I. and Figueras, F. and Fiorentino, G. and Flynn, C. and Folha, D. and Franciosini, E. and Frasca, A. and Freeman, K. and Fremat, Y. and Friel, E. and Gaensicke, B. and Gameiro, J. and Garzon, F. and Geier, S. and Geisler, D. and Gerhard, O. and Gibson, B. and Gomboc, A. and Gomez, A. and {Gonzalez-Fernandez}, C. and Gonzalez Hernandez, J. and Gosset, E. and Grebel, E. and Greimel, R. and Groenewegen, M. and Grundahl, F. and Guarcello, M. and Gustafsson, B. and Hadrava, P. and Hatzidimitriou, D. and Hambly, N. and Hammersley, P. and Hansen, C. and Haywood, M. and Heber, U. and Heiter, U. and Held, E. and Helmi, A. and Hensler, G. and Herrero, A. and Hill, V. and Hodgkin, S. and Huelamo, N. and Huxor, A. and Ibata, R. and Jackson, R. and {de Jong}, R. and Jonker, P. and Jordan, S. and Jordi, C. and Jorissen, A. and Katz, D. and Kawata, D. and Keller, S. and Kharchenko, N. and Klement, R. and Klutsch, A. and Knude, J. and Koch, A. and Kochukhov, O. and Kontizas, M. and Koubsky, P. and Lallement, R. and {de Laverny}, P. and {van Leeuwen}, F. and Lemasle, B. and Lewis, G. and Lind, K. and Lindstrom, H. P. E. and Lobel, A. and Lopez Santiago, J. and Lucas, P. and Ludwig, H. and Lueftinger, T. and Magrini, L. and Maiz Apellaniz, J. and Maldonado, J. and Marconi, G. and Marino, A. and Martayan, C. and {Martinez-Valpuesta}, I. and Matijevic, G. and McMahon, R. and Messina, S. and Meyer, M. and Miglio, A. and Mikolaitis, S. and Minchev, I. and Minniti, D. and Moitinho, A. and Momany, Y. and Monaco, L. and Montalto, M. and Monteiro, M. J. and Monier, R. and Montes, D. and Mora, A. and Moraux, E. and Morel, T. and Mowlavi, N. and Mucciarelli, A. and Munari, U. and Napiwotzki, R. and Nardetto, N. and Naylor, T. and Naze, Y. and Nelemans, G. and Okamoto, S. and Ortolani, S. and Pace, G. and Palla, F. and Palous, J. and Parker, R. and Penarrubia, J. and Pillitteri, I. and Piotto, G. and Posbic, H. and Prisinzano, L. and Puzeras, E. and Quirrenbach, A. and Ragaini, S. and Read, J. and Read, M. and Reyle, C. and De Ridder, J. and Robichon, N. and Robin, A. and Roeser, S. and Romano, D. and Royer, F. and Ruchti, G. and Ruzicka, A. and Ryan, S. and Ryde, N. and Santos, N. and Sanz Forcada, J. and Sarro Baro, L. M. and Sbordone, L. and Schilbach, E. and Schmeja, S. and Schnurr, O. and Schoenrich, R. and Scholz, R.-D. and Seabroke, G. and Sharma, S. and De Silva, G. and Smith, M. and Solano, E. and Sordo, R. and Soubiran, C. and Sousa, S. and Spagna, A. and Steffen, M. and Steinmetz, M. and Stelzer, B. and Stempels, E. and Tabernero, H. and Tautvaisiene, G. and Thevenin, F. and Torra, J. and Tosi, M. and Tolstoy, E. and Turon, C. and Walker, M. and Wambsganss, J. and Worley, C. and Venn, K. and Vink, J. and Wyse, R. and Zaggia, S. and Zeilinger, W. and Zoccali, M. and Zorec, J. and Zucker, D. and Zwitter, T. and {Gaia-ESO Survey Team}},
  year = {2012},
  month = mar,
  volume = {147},
  pages = {25--31},
  issn = {0722-6691},
  abstract = {The Gaia-ESO Public Spectroscopic Survey has begun and will obtain high quality spectroscopy of some 100000 Milky Way stars, in the field and in open clusters, down to magnitude 19, systematically covering all the major components of the Milky Way. This survey will provide the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. The motivation, organisation and implementation of the Gaia-ESO Survey are described, emphasising the complementarity with the ESA Gaia mission. Spectra from the very first observing run of the survey are presented.},
  file = {/Users/Oliver/Zotero/storage/RIDREQIV/Gilmore et al. - 2012 - The Gaia-ESO Public Spectroscopic Survey.pdf},
  journal = {The Messenger}
}

@article{ginsburg+2019,
  title = {Astroquery: {{An Astronomical Web}}-Querying {{Package}} in {{Python}}},
  shorttitle = {Astroquery},
  author = {Ginsburg, Adam and Sip{\H o}cz, Brigitta M. and Brasseur, C. E. and Cowperthwaite, Philip S. and Craig, Matthew W. and Deil, Christoph and Guillochon, James and Guzman, Giannina and Liedtke, Simon and Lian Lim, Pey and Lockhart, Kelly E. and Mommert, Michael and Morris, Brett M. and Norman, Henrik and Parikh, Madhura and Persson, Magnus V. and Robitaille, Thomas P. and Segovia, Juan-Carlos and Singer, Leo P. and Tollerud, Erik J. and {de Val-Borro}, Miguel and Valtchanov, Ivan and Woillez, Julien and {Astroquery Collaboration} and {a subset of astropy Collaboration}},
  year = {2019},
  month = mar,
  volume = {157},
  pages = {98},
  issn = {0004-6256},
  doi = {10.3847/1538-3881/aafc33},
  abstract = {astroquery is a collection of tools for requesting data from databases hosted on remote servers with interfaces exposed on the internet, including those with web pages but without formal application program interfaces. These tools are built on the Python requests package, which is used to make HTTP requests, and astropy, which provides most of the data parsing functionality. astroquery modules generally attempt to replicate the web page interface provided by a given service as closely as possible, making the transition from browser-based to command-line interaction easy. astroquery has received significant contributions from throughout the astronomical community, including several from telescope archives. astroquery enables the creation of fully reproducible
workflows from data acquisition through publication. This paper
describes the philosophy, basic structure, and development model of the astroquery package. The complete documentation for astroquery can be
found at http://astroquery.readthedocs.io/.},
  file = {/Users/Oliver/Zotero/storage/DNGD7BEX/Ginsburg et al. - 2019 - astroquery An Astronomical Web-querying Package i.pdf},
  journal = {The Astronomical Journal},
  keywords = {astronomical databases: miscellaneous,virtual observatory tools}
}

@article{girardi+2012,
  title = {{{TRILEGAL}}, a {{TRIdimensional modeL}} of {{thE GALaxy}}: {{Status}} and {{Future}}},
  shorttitle = {{{TRILEGAL}}, a {{TRIdimensional modeL}} of {{thE GALaxy}}},
  author = {Girardi, L{\'e}o and Barbieri, Mauro and Groenewegen, Martin A. T. and Marigo, Paola and Bressan, Alessandro and {Rocha-Pinto}, Helio J. and Santiago, Bas{\'i}lio X. and Camargo, Julio I. B. and {da Costa}, Luiz N.},
  year = {2012},
  volume = {26},
  pages = {165},
  doi = {10.1007/978-3-642-18418-5_17},
  abstract = {We briefly describe TRILEGAL, a TRIdimensional modeL of thE GALaxy, and its more recent developments. Particularly relevant is the recent inclusion of a kinematical module to the code, and the present efforts to provide a more solid calibration of Milky Way parameters based on 2MASS and SDSS data.},
  journal = {Astrophysics and Space Science Proceedings},
  keywords = {Physics}
}

@article{girardi+2015,
  title = {The {{Expected Stellar Populations}} in the {{Kepler}} and {{CoRoT Fields}}},
  author = {Girardi, L{\'e}o and Barbieri, Mauro and Miglio, Andrea and Bossini, Diego and Bressan, Alessandro and Marigo, Paola and Rodrigues, Tha{\'i}se S.},
  year = {2015},
  volume = {39},
  pages = {125},
  address = {{eprint: arXiv:1409.2276}},
  doi = {10.1007/978-3-319-10993-0_14},
  abstract = {Using the stellar population synthesis tool TRILEGAL, we discuss the expected stellar populations in the Kepler and CoRoT fields.},
  file = {/Users/Oliver/Zotero/storage/9ZV3ZWXR/Girardi et al. - 2015 - The Expected Stellar Populations in the Kepler and.pdf},
  keywords = {Physics}
}

@article{girardi+salaris2001,
  title = {Population Effects on the Red Giant Clump Absolute Magnitude, and Distance Determinations to Nearby Galaxies},
  author = {Girardi, L{\'e}o and Salaris, Maurizio},
  year = {2001},
  month = may,
  volume = {323},
  pages = {109},
  doi = {10.1046/j.1365-8711.2001.04084.x},
  abstract = {The red giant clump has been recently argued to be a reliable distance indicator for the galaxies in the Local Group. The accuracy of distance determinations based on this method, however, depends on the possible presence of systematic magnitude differences ({$\increment$}MIRC) between the local clump revealed by the Hipparcos colour-magnitude diagram (CMD), and the clump stars observed in distant galaxies. In this paper, we re-address the problem of these systematic `population' effects. First, we present tables with the theoretically predicted I-band clump magnitude as a function of age and metallicity. Simple equations, taken from basic population synthesis theory, are provided for the easy computation of the mean clump magnitude for any given galaxy model. We use our models to explain in some detail what determines the distribution of masses, ages and metallicities of clump stars in a galaxy. Such an approach has so far been neglected in the analysis of clump data related with distance determinations. We point out that, in galaxies with recent/ongoing star formation (e.g. the discs of spirals), the age distribution of clump stars is strongly biased towards younger (\textasciitilde 1-3Gyr) ages, and hence towards higher metallicities. Obviously, this does not happen in galaxies with predominantly old stellar populations (e.g. ellipticals and bulges). We construct detailed models for the clump population in the local (Hipparcos) sample, the bulge, Magellanic Clouds and Carina dSph galaxy. In all cases, star formation rates and chemical enrichment histories are taken from the literature. The Hipparcos model is shown to produce distributions of metallicities, colours, and magnitudes, that are similar to those derived from spectroscopic and Hipparcos data. The bulge, Magellanic Clouds, and Carina dSph models are used to analyse the values of {$\increment$}MIRC for these different stellar systems. We show how the clump-RR Lyrae data from Udalski are well reproduced by the models. However, despite the similarity between the models and data, the models indicate that the linear {$\increment$}MIRC versus [Fe/H] relations that have been derived from the same data (such as by Udalski and Popowski) are not general. In fact, the distribution of clump stars has several factors hidden in it - e.g. the age-metallicity relation, the rate of past star formation - that cannot be described by such relations. The model behaviour is also supported by empirical data for open clusters by Sarajedini and Twarog et al. We argue that Udalski's data for Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) star clusters do not allow a good assessment of the age dependence of the clump magnitude. Moreover, we remark that similar analyses of cluster data should better include clump stars with ages 1-2Gyr, which turn out to be very important in determining the mean clump in galaxies with recent star formation. Finally, we provide revised clump distances to the bulge, Magellanic Clouds and Carina dSph, and further comment on their reliability. The largest {$\increment$}MIRC values are found for the Magellanic Clouds and Carina dSph, which turn out to be located at distance moduli \textasciitilde 0.2-0.3mag longer than indicated by works which ignore population effects. The Galactic bulge, instead, may be slightly closer (up to 0.1mag in distance modulus) than indicated by previous works based on the red clump, the exact result depending on the use of either scaled-solar or {$\alpha$}-enhanced stellar models.},
  file = {/Users/Oliver/Zotero/storage/QQMTKUP4/Girardi and Salaris - 2001 - Population effects on the red giant clump absolute.pdf;/Users/Oliver/Zotero/storage/PCBC8W56/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{girardi1999,
  title = {A Secondary Clump of Red Giant Stars: Why and Where},
  shorttitle = {A Secondary Clump of Red Giant Stars},
  author = {Girardi, L{\'e}o},
  year = {1999},
  month = sep,
  volume = {308},
  pages = {818},
  doi = {10.1046/j.1365-8711.1999.02746.x},
  abstract = {Based on the results of detailed population synthesis models, Girardi et al. recently claimed that the clump of red giants in the colour-magnitude diagram (CMD) of composite stellar populations should present an extension to lower luminosities, which goes down to about 0.4mag below the main clump. This feature is made of stars just massive enough to have ignited helium in non-degenerate conditions, and therefore corresponds to a limited interval of stellar masses and ages. In the present models, which include moderate convective overshooting, it corresponds to \textasciitilde 1Gyr old populations. In this paper, we go into more detail about the origin and properties of this feature. We first compare the clump theoretical models with data for clusters of different ages and metallicities, basically confirming the predicted behaviour. We then refine the previous models in order to show the following behaviour. (i) The faint extension is expected to be clearly separated from the main clump in the CMD of metal-rich populations, defining a `secondary clump' by itself. (ii) It should be present in all galactic fields containing \textasciitilde 1Gyr old stars and with mean metallicities higher than about Z=0.004. (iii) It should be particularly strong, if compared with the main red clump, in galaxies that have increased their star formation rate in the last Gyr or so of their evolution. In fact, secondary clumps similar to the model predictions are observed in the CMD of nearby stars from Hipparcos data, and in those of some Large Magellanic Cloud fields observed to date. There are also several reasons why this secondary clump may be missing or hidden in other observed CMDs of galaxy fields. For instance, it becomes indistinguishable from the main clump if the photometric errors or differential absorption are larger than about 0.2mag. None the less, this structure may provide important constraints on the star formation history of Local Group galaxies. We comment also on the intrinsic luminosity variation and dispersion of clump stars, which may limit their use as either absolute or relative distance indicators, respectively.},
  file = {/Users/Oliver/Zotero/storage/GQMTSMRG/Girardi - 1999 - A secondary clump of red giant stars why and wher.pdf;/Users/Oliver/Zotero/storage/NK6KL5UV/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{girardi2016,
  title = {Red {{Clump Stars}}},
  author = {Girardi, L{\'e}o},
  year = {2016},
  month = sep,
  volume = {54},
  pages = {95},
  doi = {10.1146/annurev-astro-081915-023354},
  abstract = {Low-mass stars in their core-helium-burning stage define the sharpest feature present in the color-magnitude diagrams of nearby galaxy systems: the red clump (RC). This feature has given rise to a series of methods aimed at measuring the distributions of stellar distances and extinctions, especially in the Magellanic Clouds and Milky Way Bulge. Because the RC is easily recognizable within the data of large spectroscopic and asteroseismic surveys, it is a useful probe of stellar densities, kinematics, and chemical abundances across the Milky Way disk; it can be applied up to larger distances than that allowed by dwarfs; and it has better accuracy than is possible with other kinds of giants. Here, we discuss the reasons for the RC narrowness in several sets of observational data, its fine structure, and the presence of systematic changes in the RC properties as regards age, metallicity, and the observed passband. These factors set the limits on the validity and accuracy of several RC methods defined in the literature.},
  file = {/Users/Oliver/Zotero/storage/8E9KHDVF/Girardi - 2016 - Red Clump Stars.pdf;/Users/Oliver/Zotero/storage/AGH9ZBDK/ui.adsabs.harvard.edu.html},
  journal = {Annual Review of Astronomy and Astrophysics},
  language = {en}
}

@article{gizis+2016,
  title = {K2 {{Ultracool Dwarfs Survey I}}: {{Photometry}} of an {{L Dwarf Superflare}}},
  shorttitle = {K2 {{Ultracool Dwarfs Survey I}}},
  author = {Gizis, John E. and Paudel, Rishi R. and Schmidt, Sarah J. and Williams, Peter K. G. and Burgasser, Adam J.},
  year = {2016},
  month = nov,
  volume = {1611},
  pages = {arXiv:1611.07080},
  abstract = {We report on K2 Campaign 8 measurements of a huge white light flare on the L1 dwarf SDSSp J005406.55-003101.8 (EPIC 220186653). The source is a typical L1 dwarf at a distance of \$\textbackslash sim50\$ pc, probably an old
hydrogen-burning star rather than a young brown dwarf. In the long (30-minute) cadence photometry, the flare peak is 21 times the flux of the stellar photosphere in the broad optical Kepler filter, which we estimate corresponds to \$\textbackslash Delta V \textbackslash approx -7.1\$. The total equivalent duration of the flare is 15.4 hr. We estimate the total bolometric energy of the flare was \$4 \textbackslash times 10\^\{33\}\$ erg, more powerful that the previously reported Kepler white light flares for the L1 dwarf WISEP J190648.47+401106.8, but weaker than the \$\textbackslash Delta V = -11\$ L0 dwarf superflare ASASSN-16ae. The initial (impulsive) cooling phase is too rapid to resolve with our 30-minute cadence data, but after one hour the gradual cooling phase has an exponential time constant of 1.8 hours. We use template fitting to estimate that the
full-time-width-at-half-amplitude of the light curve is \${$<$}10\$ minutes and that the true flare maximum reached \$\textbackslash sim70\$ times the stellar photosphere, or \$\textbackslash Delta V \textbackslash approx -8\$. This flare is comparable to the most powerful Kepler flares observed on the active M4 dwarf GJ 1243.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{gizon+2013,
  title = {Seismic Constraints on Rotation of {{Sun}}-like Star and Mass of Exoplanet},
  author = {Gizon, L. and Ballot, J. and Michel, E. and Stahn, T. and Vauclair, G. and Bruntt, H. and Quirion, P.-O. and Benomar, O. and Vauclair, S. and Appourchaux, T. and Auvergne, M. and Baglin, A. and Barban, C. and Baudin, F. and Bazot, M. and Campante, T. and Catala, C. and Chaplin, W. and Creevey, O. and Deheuvels, S. and Dolez, N. and Elsworth, Y. and Garcia, R. and Gaulme, P. and Mathis, S. and Mathur, S. and Mosser, B. and Regulo, C. and Roxburgh, I. and Salabert, D. and Samadi, R. and Sato, K. and Verner, G. and Hanasoge, S. and Sreenivasan, K. R.},
  year = {2013},
  month = aug,
  volume = {110},
  pages = {13267},
  doi = {10.1073/pnas.1303291110},
  abstract = {Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1.85 (+0.52,-0.42) M\_Jupiter, which implies that it is a planet, not a brown dwarf.},
  file = {/Users/Oliver/Zotero/storage/3W4FM3QK/Gizon et al. - 2013 - Seismic constraints on rotation of Sun-like star a.pdf;/Users/Oliver/Zotero/storage/4HBUK4TS/ui.adsabs.harvard.edu.html},
  journal = {Proceedings of the National Academy of Science},
  keywords = {Seismic rotation},
  language = {en},
  number = {33}
}

@article{gizon+2016,
  title = {Shape of a Slowly Rotating Star Measured by Asteroseismology},
  author = {Gizon, Laurent and Sekii, Takashi and Takata, Masao and Kurtz, Donald W. and Shibahashi, Hiromoto and Bazot, Michael and Benomar, Othman and Birch, Aaron C. and Sreenivasan, Katepalli R.},
  year = {2016},
  month = nov,
  volume = {2},
  pages = {e1601777-e1601777},
  issn = {2375-2548},
  doi = {10.1126/sciadv.1601777},
  abstract = {Stars are not perfectly spherically symmetric. They are deformed by rotation and magnetic fields. Until now, the study of stellar shapes has only been possible with optical interferometry for a few of the fastest-rotating nearby stars. We report an asteroseismic measurement, with much better precision than interferometry, of the asphericity of an A-type star with a rotation period of 100 days. Using the fact that different modes of oscillation probe different stellar latitudes, we infer a tiny but significant flattening of the star's shape of \$\textbackslash Delta R/R = (1.8 \textbackslash pm 0.6) \textbackslash times 10\^\{-6\}\$. For a stellar radius \$R\$ that is \$2.24\$ times the solar radius, the difference in radius between the equator and the poles is \$\textbackslash Delta R = 3 \textbackslash pm 1\$ km. Because the observed \$\textbackslash Delta R/R\$ is only one-third of the expected rotational oblateness, we conjecture the presence of a weak magnetic field on a star that does not have an extended convective envelope. This calls to question the origin of the magnetic field.},
  archivePrefix = {arXiv},
  eprint = {1611.06435},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/XZWBTH54/Gizon et al. - 2016 - Shape of a slowly rotating star measured by astero.pdf;/Users/Oliver/Zotero/storage/B4IPQ5QI/1611.html},
  journal = {Science Advances},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {11}
}

@article{gizon+solanki2003,
  title = {Determining the {{Inclination}} of the {{Rotation Axis}} of a {{Sun}}-like {{Star}}},
  author = {Gizon, L. and Solanki, S. K.},
  year = {2003},
  month = jun,
  volume = {589},
  pages = {1009},
  doi = {10.1086/374715},
  abstract = {Asteroseismology provides us with the possibility of determining the angle, i, between the direction of the rotation axis of a pulsating Sun-like star and the line of sight. A knowledge of i is important not just for obtaining improved stellar parameters, but also in order to determine the true masses of extrasolar planets detected from the radial velocity shifts of their central stars. By means of Monte Carlo simulations, we estimate the precision of the measurement of i and other stellar parameters. We find that the inclination angle can be retrieved accurately when i\>\textasciitilde 30\textsuperscript{deg} for stars that rotate at least twice as fast as the Sun.},
  file = {/Users/Oliver/Zotero/storage/8ZKH6W3K/Gizon and Solanki - 2003 - Determining the Inclination of the Rotation Axis o.pdf;/Users/Oliver/Zotero/storage/SZYG2QPE/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{goldreich+keeley1977,
  title = {Solar Seismology. {{I}} - {{The}} Stability of the Solar p-Modes},
  author = {Goldreich, P. and Keeley, D. A.},
  year = {1977},
  month = feb,
  volume = {211},
  pages = {934--942},
  issn = {0004-637X},
  doi = {10.1086/155005},
  abstract = {The stability of the radial p-modes of the sun is investigated by computing nonadiabatic eigenvalues and eigenfunctions for a solar envelope model which extends from an inner radius of about 0.3 solar radius out to an optical depth of about 0.0003. The calculations take into account in a crude fashion the response of the convective flux to the oscillation. The dynamical effect of turbulence in the convection zone is parametrized in terms of a turbulent shear viscosity. The results show that if damping by turbulent viscosity is neglected, all modes with periods longer than 6 minutes are unstable. The familiar kappa-mechanism, which operates in the H ionization-H(-) opacity region, is the dominant source of driving of the oscillations. Modes with periods shorter than 6 minutes are stabilized by radiative damping in the solar atmosphere. When turbulent dissipation of pulsational energy is included, all modes are predicted to be stable. However, the margin of stability is very small. In view of the large uncertainty that must be assigned to the estimate of turbulent damping, it is concluded that theoretical calculations cannot unequivocally resolve the question of the stability of the solar p-modes.},
  file = {/Users/Oliver/Zotero/storage/XS58Y7B2/Goldreich and Keeley - 1977 - Solar seismology. I - The stability of the solar p.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Astronomical Models,Convective Flow,Eigenvalues,Linear Equations,Nonadiabatic Conditions,Optical Thickness,Pulsed Radiation,Radiative Transfer,Seismology,Solar Atmosphere,Solar Physics,Stable Oscillations}
}

@article{goldreich+keeley1977a,
  title = {Solar Seismology. {{II}} - {{The}} Stochastic Excitation of the Solar p-Modes by Turbulent Convection},
  author = {Goldreich, P. and Keeley, D. A.},
  year = {1977},
  month = feb,
  volume = {212},
  pages = {243--251},
  issn = {0004-637X},
  doi = {10.1086/155043},
  abstract = {We test the hypothesis that the solar p-modes are stabilized by damping
due to turbulent viscosity in the convective zone. Starting from the
assumption that the modes are stable, we calculate expectation values
for the modal energies. We find that the interaction between a p-mode
and the turbulent convection is such that the modal energy tends toward
equipartition with the kinetic energy of turbulent eddies whose
lifetimes are comparable to the modal period. From the calculated values
of the modal energies, we compute rms surface velocity amplitudes. Our
predicted rms surface velocities range from 0.01 cm/sec for the
fundamental radial mode to 0.6 cm/sec for the radial mode whose period
is approximately 5 minutes. The predicted surface velocities for the low
order p-modes are much smaller than the velocities inferred from recent
observations.},
  file = {/Users/Oliver/Zotero/storage/ML63WHPT/Goldreich and Keeley - 1977 - Solar seismology. II - The stochastic excitation o.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Atmospheric Models,Atmospheric Turbulence,Convective Flow,Kinetic Energy,Modal Response,Perturbation Theory,Seismology,Solar Atmosphere,Stochastic Processes,Turbulence Effects,Vortices}
}

@article{goldreich+kumar1988,
  title = {The Interaction of Acoustic Radiation with Turbulence},
  author = {Goldreich, Peter and Kumar, Pawan},
  year = {1988},
  month = mar,
  volume = {326},
  pages = {462--478},
  issn = {0004-637X},
  doi = {10.1086/166108},
  abstract = {The authors derive expressions for the spectral emissivity and absorptivity of acoustic radiation by low Mach number turbulent fluids. They consider three types of turbulence. The first is free turbulence, that is, turbulence which is not subject to external forces. The second and third examples are special cases of forced turbulence, turbulence maintained by stirring with spoons and turbulent pseudoconvection. The resulting formulae are used to estimate the equilibrium energies and quality factors of the acoustic modes in a box which contains turbulent fluid. The scattering of acoustic radiation by the turbulent velocity and pressure fluctuations is treated and the rate at which nonlinear interactions transfer energy among the acoustic modes is evaluated. This work is a first step in the attempt to relate the excitation of the Sun's acoustic modes to the turbulence in the solar convection zone.},
  file = {/Users/Oliver/Zotero/storage/67STW4YB/Goldreich and Kumar - 1988 - The interaction of acoustic radiation with turbule.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Absorptivity,Convection,Electrodynamics,Magnetohydrodynamic Turbulence,Solar Oscillations,Sound Waves,Turbulent Flow,Wave Interaction}
}

@article{gontcharov+mosenkov2017,
  title = {On the Discrepancy between Asteroseismic and {{Gaia DR1 TGAS}} Parallaxes},
  author = {Gontcharov, George and Mosenkov, Aleksandr},
  year = {2017},
  month = sep,
  volume = {470},
  pages = {L97-L101},
  issn = {1745-3925, 1745-3933},
  doi = {10.1093/mnrasl/slx083},
  abstract = {Recently, a deviation of the Gaia TGAS parallaxes from the asteroseismic ones for giants was found. We show that for parallaxes \$\textbackslash varpi{$<$}1.5\$ mas it can be explained by a selection effect in favour of bright and luminous giants in the Tycho-2 and TGAS catalogues. Another explanation of this deviation seems to be valid for \$\textbackslash varpi{$>$}1.5\$ mas based on the best extinction estimates: the deviation may be caused not by a bias of parallax, but by an underestimation of the extinction (and, consequently, an overestimation of the calculated absolute magnitude) in the asteroseismic results. We demonstrate that the reliable estimates of the reddening and extinction (about 0.22 mag of the visual extinction for the Kepler field) better fit both the giants and main sequence stars to the PARSEC, MIST and YaPSI isochrones.},
  archivePrefix = {arXiv},
  eprint = {1705.09063},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/S69VT4WI/Gontcharov and Mosenkov - 2017 - On the discrepancy between asteroseismic and Gaia .pdf;/Users/Oliver/Zotero/storage/J47CH6QN/1705.html},
  journal = {Monthly Notices of the Royal Astronomical Society: Letters},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{gontcharov2017,
  title = {Systematic {{Error}} of the {{Gaia DR1 TGAS Parallaxes}} from {{Data}} for the {{Red Giant Clump}}},
  author = {Gontcharov, George},
  year = {2017},
  month = jun,
  doi = {10.1134/S1063773717060044},
  abstract = {Based on the Gaia DR1 TGAS parallaxes and photometry from the Tycho-2, Gaia, 2MASS, and WISE catalogues, we have produced a sample of about 100 000 clump red giants within about 800 pc of the Sun. The systematic variations of the mode of their absolute magnitude as a function of the distance, magnitude, and other parameters have been analyzed. We show that these variations reach 0.7 mag and cannot be explained by variations in the interstellar extinction or intrinsic properties of stars and by selection. The only explanation seems to be a systematic error of the Gaia DR1 TGAS parallax dependent on the square of the observed distance in kpc: \$0.18R\^2\$ mas. Allowance for this error reduces significantly the systematic dependences of the absolute magnitude mode on all parameters. This error reaches 0.1 mas within 800 pc of the Sun and allows an upper limit for the accuracy of the TGAS parallaxes to be estimated as 0.2 mas. A careful allowance for such errors is needed to use clump red giants as "standard candles". This eliminates all discrepancies between the theoretical and empirical estimates of the characteristics of these stars and allows us to obtain the first estimates of the modes of their absolute magnitudes from the Gaia parallaxes: \$mode(M\_H)=-1.49\^m\textbackslash pm0.04\^m\$, \$mode(M\_\{K\_s\})=-1.63\^m\textbackslash pm0.03\^m\$, \$mode(M\_\{W1\})=-1.67\^m\textbackslash pm0.05\^m\$, \$mode(M\_\{W2\})=-1.67\^m\textbackslash pm0.05\^m\$, \$mode(M\_\{W3\})=-1.66\^m\textbackslash pm0.02\^m\

repository: sandorkruk/malatium

repo_name: sandorkruk/malatium