text:
, J. and Salgado, J. and Salguero, E. and Sanna, N. and {Santana-Ros}, T. and Sarasso, M. and Savietto, H. and Schultheis, M. and Sciacca, E. and Segol, M. and Segovia, J. C. and S{\'e}gransan, D. and Shih, I.-C. and Siltala, L. and Silva, A. F. and Smart, R. L. and Smith, K. W. and Solano, E. and Solitro, F. and Sordo, R. and Soria Nieto, S. and Souchay, J. and Spagna, A. and Spoto, F. and Stampa, U. and Steele, I. A. and Steidelm{\"u}ller, H. and Stephenson, C. A. and Stoev, H. and Suess, F. F. and Surdej, J. and Szabados, L. and {Szegedi-Elek}, E. and Tapiador, D. and Taris, F. and Tauran, G. and Taylor, M. B. and Teixeira, R. and Terrett, D. and Teyssandier, P. and Thuillot, W. and Titarenko, A. and Torra Clotet, F. and Turon, C. and Ulla, A. and Utrilla, E. and Uzzi, S. and Vaillant, M. and Valentini, G. and Valette, V. and {van Elteren}, A. and Van Hemelryck, E. and {van Leeuwen}, M. and Vaschetto, M. and Vecchiato, A. and Veljanoski, J. and Viala, Y. and Vicente, D. and Vogt, S. and {von Essen}, C. and Voss, H. and Votruba, V. and Voutsinas, S. and Walmsley, G. and Weiler, M. and Wertz, O. and Wevers, T. and Wyrzykowski, {\L} and Yoldas, A. and {\v Z}erjal, M. and Ziaeepour, H. and Zorec, J. and Zschocke, S. and Zucker, S. and Zurbach, C. and Zwitter, T.},
  year = {2018},
  month = aug,
  volume = {616},
  pages = {A1},
  doi = {10.1051/0004-6361/201833051},
  abstract = {Context. 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. \\
 Aims: 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. \\
 Methods: The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. \\
 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\textsubscript{BP} (330-680 nm) and G\textsubscript{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 14 000 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. \\
 Conclusions: Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.},
  file = {/Users/Oliver/Zotero/storage/EBKAPVV8/Brown et al. - 2018 - Gaia Data Release 2. Summary of the contents and s.pdf;/Users/Oliver/Zotero/storage/QA6VPCW3/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{brown+gilliland1994,
  title = {Asteroseismology},
  author = {Brown, Timothy M. and Gilliland, Ronald L.},
  year = {1994},
  volume = {32},
  pages = {37--82},
  issn = {0066-4146},
  doi = {10.1146/annurev.aa.32.090194.000345},
  abstract = {Not Available},
  file = {/Users/Oliver/Zotero/storage/JPMMTED2/Asteroseismology.docx;/Users/Oliver/Zotero/storage/MVXF6UKJ/1994ARA+A__32___37B.pdf},
  journal = {Annual Review of Astronomy and Astrophysics}
}

@article{brown2017,
  title = {On the Eccentricity of {{Proxima}} b},
  author = {Brown, Robert A.},
  year = {2017},
  month = jan,
  abstract = {We apply Monte Carlo projection to the radial velocity data set that Anglada Escude et al. (2016) use for the discovery of Proxima b. They find an upper limit to the orbital eccentricity of 0.35. To investigate the eccentricity issue further, we calculate a suite of monovariate and bivariate densities o eccentricity. After discarding apparent artifacts at eccentricity = 0 and = 1, we find that eccentricity has a trimodal sampling distribution: three chimeras or types of orbit compatible with the RV data set. The three modes or peaks in the density of eccentricity are located at eccentricity = 0.25, 0.75, and 0.95, with relative weights 0.79, 0.10, and 0.11. Future RV observations will clarify which of the three chimeras represents the true eccentricity of Proxima b. The most-likely estimate is eccentricity = 0.25, and our lower limit is eccentricity = 0.025. Our strategic, long-term goal is to elevate the orbital analyses of exoplanets to meet the challenges of sometimes complex probability density distributions.},
  archivePrefix = {arXiv},
  eprint = {1701.04063},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/FBQBSQR2/Brown - 2017 - On the eccentricity of Proxima b.pdf;/Users/Oliver/Zotero/storage/C4UZMKUN/1701.html},
  journal = {arXiv:1701.04063 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{brown2018,
  title = {The {{Gaia}} Sky: Version 1.0},
  shorttitle = {The {{Gaia}} Sky},
  author = {Brown, Anthony G. A.},
  year = {2018},
  month = apr,
  volume = {330},
  pages = {13},
  doi = {10.1017/S1743921317006664},
  abstract = {In this contribution I provide a brief summary of the contents of Gaia DR1. This is followed by a discussion of studies in the literature that attempt to characterize the quality of the Tycho-Gaia Astrometric Solution parallaxes in Gaia DR1, and I point out a misconception about the handling of the known systematic errors in the Gaia DR1 parallaxes. I highlight some of the more unexpected uses of the Gaia DR1 data and close with a look ahead at the next Gaia data releases, with Gaia DR2 coming up in April 2018.},
  file = {/Users/Oliver/Zotero/storage/JD3D2DLU/Brown - 2018 - The Gaia sky version 1.0.pdf;/Users/Oliver/Zotero/storage/5Z2GV86Z/ui.adsabs.harvard.edu.html},
  journal = {Astrometry and Astrophysics in the Gaia Sky},
  language = {en}
}

@article{brun+2004,
  title = {Global-{{Scale Turbulent Convection}} and {{Magnetic Dynamo Action}} in the {{Solar Envelope}}},
  author = {Brun, Allan Sacha and Miesch, Mark S. and Toomre, Juri},
  year = {2004},
  month = oct,
  volume = {614},
  pages = {1073--1098},
  issn = {0004-637X},
  doi = {10.1086/423835},
  abstract = {The operation of the solar global dynamo appears to involve many
dynamical elements, including the generation of fields by the intense
turbulence of the deep convection zone, the transport of these fields
into the tachocline region near the base of the convection zone, the
storage and amplification of toroidal fields in the tachocline by
differential rotation, and the destabilization and emergence of such
fields due to magnetic buoyancy. Self-consistent magnetohydrodynamic
(MHD) simulations that realistically incorporate all of these processes
are not yet computationally feasible, although some elements can now be
studied with reasonable fidelity. Here we consider the manner in which
turbulent compressible convection within the bulk of the solar
convection zone can generate large-scale magnetic fields through dynamo
action. We accomplish this through a series of three-dimensional
numerical simulations of MHD convection within rotating spherical shells
using our anelastic spherical harmonic (ASH) code on massively parallel
supercomputers. Since differential rotation is a key ingredient in all
dynamo models, we also examine here the nature of the rotation profiles
that can be sustained within the deep convection zone as strong magnetic
fields are built and maintained. We find that the convection is able to
maintain a solar-like angular velocity profile despite the influence of
Maxwell stresses, which tend to oppose Reynolds stresses and thus reduce
the latitudinal angular velocity contrast throughout the convection
zone. The dynamo-generated magnetic fields exhibit a complex structure
and evolution, with radial fields concentrated in downflow lanes and
toroidal fields organized into twisted ribbons that are extended in
longitude and achieve field strengths of up to 5000 G. The flows and
fields exhibit substantial kinetic and magnetic helicity although
systematic hemispherical patterns are only apparent in the former.
Fluctuating fields dominate the magnetic energy and account for most of
the back-reaction on the flow via Lorentz forces. Mean fields are
relatively weak and do not exhibit systematic latitudinal propagation or
periodic polarity reversals as in the Sun. This may be attributed to the
absence of a tachocline, i.e., a penetrative boundary layer between the
convection zone and the deeper radiative interior possessing strong
rotational shear. The influence of such a layer will await subsequent
studies.},
  file = {/Users/Oliver/Zotero/storage/R83RKLZJ/Brun et al. - 2004 - Global-Scale Turbulent Convection and Magnetic Dyn.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Convection,Magnetohydrodynamics: MHD,Sun: Magnetic Fields,Turbulence}
}

@article{bryson+2013,
  title = {Identification of {{Background False Positives}} from {{Kepler Data}}},
  author = {Bryson, Stephen T. and Jenkins, Jon M. and Gilliland, Ronald L. and Twicken, Joseph D. and Clarke, Bruce and Rowe, Jason and Caldwell, Douglas and Batalha, Natalie and Mullally, Fergal and Haas, Michael R. and Tenenbaum, Peter},
  year = {2013},
  month = aug,
  volume = {125},
  pages = {889},
  issn = {0004-6280},
  doi = {10.1086/671767},
  abstract = {The Kepler Mission was launched on 2009 March 6 to perform a photometric survey of more than 100,000 dwarf stars to search for Earth-size planets with the transit technique. The reliability of the resulting planetary candidate list relies on the ability to identify and remove false positives. Major sources of astrophysical false positives are planetary transits and stellar eclipses on background stars. We describe several new techniques for the identification of background transit sources that are separated from their target stars, indicating an astrophysical false positive. These techniques use only Kepler photometric data. We describe the concepts and construction of these techniques in detail as well as their performance and relative merits.},
  file = {/Users/Oliver/Zotero/storage/E45BMDQU/Bryson et al. - 2013 - Identification of Background False Positives from .pdf},
  journal = {Publications of the Astronomical Society of the Pacific}
}

@article{buchhave+latham2015,
  title = {The {{Metallicities}} of {{Stars}} with and without {{Transiting Planets}}},
  author = {Buchhave, Lars A. and Latham, David W.},
  year = {2015},
  month = aug,
  volume = {808},
  pages = {187},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/808/2/187},
  abstract = {Host star metallicities have been used to infer observational constraints on planet formation throughout the history of the exoplanet field. The giant planet metallicity correlation has now been widely accepted, but questions remain as to whether the metallicity correlation extends to the small terrestrial-sized planets. Here, we report
metallicities for a sample of 518 stars in the Kepler field that have no detected transiting planets and compare their metallicity distribution to a sample of stars that hosts small planets (\{R\}p\textbackslash lt 1.7 \{R\}\textbackslash oplus ). Importantly, both samples have been analyzed in a homogeneous manner using the same set of tools (Stellar Parameters Classification tool). We find the average metallicity of the sample of stars without detected transiting planets to be
\{[\{\{m\}\}/\{\{H\}\}]\}\{SNTP,\{dwarf\}\}=-0.02+/- 0.02 \{dex\} and the sample of stars hosting small planets to be
\{[\{\{m\}\}/\{\{H\}\}]\}\{STP\}=-0.02+/- 0.02 \{dex\}. The average metallicities of the two samples are indistinguishable within the uncertainties, and the two-sample Kolmogorov-Smirnov test yields a p-value of 0.68 (0.41{$\sigma$}), indicating a failure to reject the null hypothesis that the two samples are drawn from the same parent
population. We conclude that the homogeneous analysis of the data presented here supports the hypothesis that stars hosting small planets have a metallicity similar to stars with no known transiting planets in the same area of the sky.},
  file = {/Users/Oliver/Zotero/storage/LPNPDBXQ/Buchhave and Latham - 2015 - The Metallicities of Stars with and without Transi.pdf},
  journal = {The Astrophysical Journal},
  keywords = {planetary systems,surveys,techniques: spectroscopic}
}

@article{buckley+2016,
  title = {Polarimetric Evidence of a White Dwarf Pulsar in the Binary System {{AR Scorpii}}},
  author = {Buckley, D. A. H. and Meintjes, P. J. and Potter, S. B. and Marsh, T. R. and G{\"a}nsicke, B. T.},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/DGJFAVCD/1612.03185.pdf},
  journal = {arXiv preprint arXiv:1612.03185}
}

@article{buder+2018,
  title = {The {{GALAH Survey}}: Second Data Release},
  shorttitle = {The {{GALAH Survey}}},
  author = {Buder, Sven and Asplund, Martin and Duong, Ly and Kos, Janez and Lind, Karin and Ness, Melissa K. and Sharma, Sanjib and {Bland-Hawthorn}, Joss and Casey, Andrew R. and {de Silva}, Gayandhi M. and D'Orazi, Valentina and Freeman, Ken C. and Lewis, Geraint F. and Lin, Jane and Martell, Sarah L. and Schlesinger, Katharine J. and Simpson, Jeffrey D. and Zucker, Daniel B. and Zwitter, Toma{\v z} and Amarsi, Anish M. and Anguiano, Borja and Carollo, Daniela and Casagrande, Luca and {\v C}otar, Klemen and Cottrell, Peter L. and {da Costa}, Gary and Gao, Xudong D. and Hayden, Michael R. and Horner, Jonathan and Ireland, Michael J. and Kafle, Prajwal R. and Munari, Ulisse and Nataf, David M. and Nordlander, Thomas and Stello, Dennis and Ting, Yuan-Sen and Traven, Gregor and Watson, Fred and Wittenmyer, Robert A. and Wyse, Rosemary F. G. and Yong, David and Zinn, Joel C. and {\v Z}erjal, Maru{\v s}a and {Galah Collaboration}},
  year = {2018},
  month = aug,
  volume = {478},
  pages = {4513--4552},
  issn = {0035-8711},
  doi = {10.1093/mnras/sty1281},
  abstract = {The Galactic Archaeology with HERMES (GALAH) survey is a large-scale stellar spectroscopic survey of the Milky Way, designed to deliver complementary chemical information to a large number of stars covered by the Gaia mission. We present the GALAH second public data release (GALAH DR2) containing 342 682 stars. For these stars, the GALAH collaboration provides stellar parameters and abundances for up to 23 elements to the community. Here we present the target selection, observation, data reduction, and detailed explanation of how the spectra were analysed to estimate stellar parameters and element abundances. For the stellar analysis, we have used a multistep approach. We use the physics-driven spectrum synthesis of Spectroscopy Made Easy (SME) to derive stellar labels (Teff, log g, [Fe/H], [X/Fe], vmic, vsin i, A\_\{K\_S\}) for a representative training set of stars. This information is then propagated to the whole sample with the data-driven method of The Cannon. Special care has been exercised in the spectral synthesis to only consider spectral lines that have reliable atomic input data and are little affected by blending lines. Departures from local
thermodynamic equilibrium (LTE) are considered for several key elements, including Li, O, Na, Mg, Al, Si, and Fe, using 1D MARCS stellar
atmosphere models. Validation tests including repeat observations, Gaia benchmark stars, open and globular clusters, and K2 asteroseismic targets lend confidence to our methods and results. Combining the GALAH DR2 catalogue with the kinematic information from Gaia will enable a wide range of Galactic Archaeology studies, with unprecedented detail, dimensionality, and scope.},
  file = {/Users/Oliver/Zotero/storage/X66THHH9/Buder et al. - 2018 - The GALAH Survey second data release.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {methods: data analysis,methods: observational,stars: abundances,stars: fundamental parameters,Surveys,the Galaxy}
}

@article{buldgen2019,
  title = {Global {{Helioseismology}}},
  author = {Buldgen, G.},
  year = {2019},
  month = dec,
  abstract = {Helioseismology is one of the most successful fields of astrophysics. The observation and characterization of solar oscillation has allowed solar seismologists to study the internal structure and dynamics of the Sun with unprecedented thoroughness. Ground-based networks and dedicated space missions have delivered data of exquisite quality, enabling the development of sophisticated inference techniques. The achievements of the fields count, amongst other, the determination of solar photospheric helium abundance, unacessible to spectroscopic constraints, the precise positioning of the base of the convective zone and the demonstration of the importance of microscopic diffusion in stellar radiative regions. Helioseismology played also a key role in validating the framework used to compute solar and stellar models and played an important role in the so-called solar neutrino problem. In the current era of astrophysics, with the increasing importance of asteroseismology to precisely characterize stars, the Sun still plays a crucial calibration role, acting as a benchmark for stellar models. With the revision of the solar abundances and the current discussions related to radiative opacity computations, the role of the Sun as a laboratory of fundamental physics is undisputable. In this brief review, I will discuss some of the inference techniques developed in the field of helioseismology, dedicated to the exploitation of the solar global oscillation modes.},
  archivePrefix = {arXiv},
  eprint = {1912.02003},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/K4J9PD8F/Buldgen - 2019 - Global Helioseismology.pdf;/Users/Oliver/Zotero/storage/HIHEQ2L7/1912.html},
  journal = {arXiv:1912.02003 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{buzasi+2005,
  title = {Altair: {{The Brightest}} {$\delta$} {{Scuti Star}}},
  shorttitle = {Altair},
  author = {Buzasi, D. L. and Bruntt, H. and Bedding, T. R. and Retter, A. and Kjeldsen, H. and Preston, H. L. and Mandeville, W. J. and Suarez, J. C. and Catanzarite, J. and Conrow, T. and Laher, R.},
  year = {2005},
  month = feb,
  volume = {619},
  pages = {1072--1076},
  issn = {0004-637X},
  doi = {10.1086/426704},
  abstract = {We present an analysis of observations of the bright star Altair ({$\alpha$} Aql) obtained using the star camera on the Wide Field Infrared Explorer (WIRE) satellite. Although Altair lies within the {$\delta$} Scuti instability strip, previous observations have not revealed the presence of oscillations. However, the WIRE observations show Altair to be a low-amplitude ({$\Delta$}m{$<$}1 parts per thousand [ppt]) {$\delta$} Scuti
star with at least seven modes present.},
  file = {/Users/Oliver/Zotero/storage/TAPWUQSD/Buzasi et al. - 2005 - Altair The Brightest δ Scuti Star.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Stars: Individual: Constellation Name: α Aquilae,Stars: Oscillations}
}

@article{buzasi+2015,
  title = {Serendipitous {{Science}} from the {{K2 Mission}}},
  author = {Buzasi, Derek L. and Carboneau, Lindsey and Hessler, Carly and Lezcano, Andy and Preston, Heather},
  year = {2015},
  file = {/Users/Oliver/Zotero/storage/HV3MA3ZK/1511.09069v1.pdf},
  journal = {arXiv preprint arXiv:1511.09069},
  keywords = {C3,Notes}
}

@article{buzasi2000,
  title = {Experiment {{Design}} and {{Data Reduction}} for {{Seismology}}: {{Lessons Learned}} from {{WIRE}}},
  shorttitle = {Experiment {{Design}} and {{Data Reduction}} for {{Seismology}}},
  author = {Buzasi, D. L.},
  year = {2000},
  month = apr,
  pages = {9},
  abstract = {Since June 1999, the 5 cm star camera on board the WIRE spacecraft has been used to perform asteroseismology on a variety of targets. This has provided an unusual opportunity to assess the performance of a CCD in space, and to learn firsthand some of the data reduction problems that future missions such as MONS will face. I will describe our performance characteristics and problems, and briefly summarize our results to date.},
  file = {/Users/Oliver/Zotero/storage/ZIZAZP9J/Buzasi - 2000 - Experiment Design and Data Reduction for Seismolog.pdf}
}

@article{cameron+2017,
  title = {Observing and Modeling the Poloidal and Toroidal Fields of the Solar Dynamo},
  author = {Cameron, R. H. and Duvall Jr., T. L. and Sch{\"u}ssler, M. and Schunker, H.},
  year = {2017},
  month = oct,
  abstract = {Context. The solar dynamo consists of a process that converts poloidal field to toroidal field followed by a process which creates new poloidal field from the toroidal field. Aims. Our aim is to observe the poloidal and toroidal fields relevant to the global solar dynamo and see if their evolution is captured by a Babcock-Leighton dynamo. Methods. We use synoptic maps of the surface radial field from the KPNSO/VT and SOLIS observatories to construct the poloidal field as a function of time and latitude, and Wilcox Solar Observatory and SOHO/MDI full disk images to infer the longitudinally averaged surface azimuthal field. We show that the latter is consistent with an estimate of that due to flux emergence and therefore closely related to the subsurface toroidal field. Results. We present maps of the poloidal and toroidal magnetic field of the global solar dynamo. The longitude-averaged azimuthal field observed at the surface results from flux emergence. At high latitudes this component follows the radial component of the polar fields with a short time lag (1-3 years). The lag increases at lower latitudes. The observed evolution of the poloidal and toroidal magnetic fields is described by the (updated) Babcock-Leighton dynamo model.},
  archivePrefix = {arXiv},
  eprint = {1710.07126},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/268HFPI7/Cameron et al. - 2017 - Observing and modeling the poloidal and toroidal f.pdf;/Users/Oliver/Zotero/storage/ND8SPCW3/1710.html},
  journal = {arXiv:1710.07126 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{campante+2016,
  title = {Spin-{{Orbit Alignment}} of {{Exoplanet Systems}}: {{Ensemble Analysis Using Asteroseismology}}},
  shorttitle = {Spin-{{Orbit Alignment}} of {{Exoplanet Systems}}},
  author = {Campante, T. L. and Lund, M. N. and Kuszlewicz, J. S. and Davies, G. R. and Chaplin, W. J. and Albrecht, S. and Winn, J. N. and Bedding, T. R. and Benomar, O. and Bossini, D. and Handberg, R. and Santos, A. R. G. and Van Eylen, V. and Basu, S. and {Christensen-Dalsgaard}, J. and Elsworth, Y. P. and Hekker, S. and Hirano, T. and Huber, D. and Karoff, C. and Kjeldsen, H. and Lundkvist, M. S. and North, T. S. H. and Silva Aguirre, V. and Stello, D. and White, T. R.},
  year = {2016},
  month = mar,
  volume = {819},
  pages = {85},
  doi = {10.3847/0004-637X/819/1/85},
  abstract = {The angle {$\psi$} between a planet's orbital axis and the spin axis of its parent star is an important diagnostic of planet formation, migration, and tidal evolution. We seek empirical constraints on {$\psi$} by measuring the stellar inclination I\textsubscript{s} via asteroseismology for an ensemble of 25 solar-type hosts observed with NASA's Kepler satellite. Our results for I\textsubscript{s} are consistent with alignment at the 2{$\sigma$} level for all stars in the sample, meaning that the system surrounding the red-giant star Kepler-56 remains as the only unambiguous misaligned multiple-planet system detected to date. The availability of a measurement of the projected spin-orbit angle {$\lambda$} for two of the systems allows us to estimate {$\psi$}. We find that the orbit of the hot Jupiter HAT-P-7b is likely to be retrograde (\textbackslash psi =116\textbackslash buildrel\{\textbackslash circ\}\textbackslash over\{.\} \{4\}\textsubscript{-14.7}\textsuperscript{+30.2}), whereas that of Kepler-25c seems to be well aligned with the stellar spin axis (\textbackslash psi =12\textbackslash buildrel\{\textbackslash circ\}\textbackslash over\{.\} \{6\}\textsubscript{-11.0}\textsuperscript{+6.7}). While the latter result is in apparent contradiction with a statement made previously in the literature that the multi-transiting system Kepler-25 is misaligned, we show that the results are consistent, given the large associated uncertainties. Finally, we perform a hierarchical Bayesian analysis based on the asteroseismic sample in order to recover the underlying distribution of {$\psi$}. The ensemble analysis suggests that the directions of the stellar spin and planetary orbital axes are correlated, as conveyed by a tendency of the host stars to display large values of inclination.},
  file = {/Users/Oliver/Zotero/storage/4JIH54Z8/Campante et al. - 2016 - Spin-Orbit Alignment of Exoplanet Systems Ensembl.pdf;/Users/Oliver/Zotero/storage/BDS4GLEJ/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{campante+2016a,
  title = {The {{Asteroseismic Potential}} of {{TESS}}: {{Exoplanet}}-Host {{Stars}}},
  shorttitle = {The {{Asteroseismic Potential}} of {{TESS}}},
  author = {Campante, T. L. and Schofield, M. and Kuszlewicz, J. S. and Bouma, L. and Chaplin, W. J. and Huber, D. and {Christensen-Dalsgaard}, J. and Kjeldsen, H. and Bossini, D. and North, T. S. H. and Appourchaux, T. and Latham, D. W. and Pepper, J. and Ricker, G. R. and Stassun, K. G. and Vanderspek, R. and Winn, J. N.},
  year = {2016},
  month = oct,
  volume = {830},
  pages = {138},
  doi = {10.3847/0004-637X/830/2/138},
  abstract = {New insights on stellar evolution and stellar interior physics are being made possible by asteroseismology. Throughout the course of the Kepler mission, asteroseismology has also played an important role in the characterization of exoplanet-host stars and their planetary systems. The upcoming NASA Transiting Exoplanet Survey Satellite (TESS) will be performing a near all-sky survey for planets that transit bright nearby stars. In addition, its excellent photometric precision, combined with its fine time sampling and long intervals of uninterrupted observations, will enable asteroseismology of solar-type and red-giant stars. Here we develop a simple test to estimate the detectability of solar-like oscillations in TESS photometry of any given star. Based on an all-sky stellar and planetary synthetic population, we go on to predict the asteroseismic yield of the TESS mission, placing emphasis on the yield of exoplanet-host stars for which we expect to detect solar-like oscillations. This is done for both the target stars (observed at a 2-minute cadence) and the full-frame-image stars (observed at a 30-minute cadence). A similar exercise is also conducted based on a compilation of known host stars. We predict that TESS will detect solar-like oscillations in a few dozen target hosts (mainly subgiant stars but also in a smaller number of F dwarfs), in up to 200 low-luminosity red-giant hosts, and in over 100 solar-type and red-giant known hosts, thereby leading to a threefold improvement in the asteroseismic yield of exoplanet-host stars when compared to Kepler's.},
  file = {/Users/Oliver/Zotero/storage/ZRREXA24/Campante et al. - 2016 - The Asteroseismic Potential of TESS Exoplanet-hos.pdf;/Users/Oliver/Zotero/storage/URAEXRUT/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{campante+2018,
  title = {Synergy between Asteroseismology and Exoplanet Science: An Outlook},
  shorttitle = {Synergy between Asteroseismology and Exoplanet Science},
  author = {Campante, Tiago L. and Barros, Susana C. C. and Demangeon, Olivier and {da N{\'o}brega}, Hugo J. and Kuszlewicz, James S. and Pereira, Filipe and Chaplin, William J. and Huber, Daniel},
  year = {2018},
  month = dec,
  pages = {arXiv:1812.06150},
  abstract = {Space-based asteroseismology has been playing an important role in the characterization of exoplanet-host stars and their planetary systems. The future looks even brighter, with space missions such as NASA's TESS and ESA's PLATO ready to take on this legacy. In this contribution, we provide an outlook on the synergy between asteroseismology and exoplanet science, namely, on the prospect of conducting a populational study of giant planets around oscillating evolved stars with the TESS mission.},
  file = {/Users/Oliver/Zotero/storage/6FUHCUZ8/Campante et al. - 2018 - Synergy between asteroseismology and exoplanet sci.pdf;/Users/Oliver/Zotero/storage/63BQBEPZ/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{campante+2019,
  title = {{{TESS Asteroseismology}} of the Known Red-Giant Host Stars {{HD}} 212771 and {{HD}} 203949},
  author = {Campante, Tiago L. and Corsaro, Enrico and Lund, Mikkel N. and Mosser, Beno{\^i}t and Serenelli, Aldo and Veras, Dimitri and Adibekyan, Vardan and Antia, H. M. and Ball, Warrick and Basu, Sarbani and Bedding, Timothy R. and Bossini, Diego and Davies, Guy R. and Delgado Mena, Elisa and Garc{\'i}a, Rafael A. and Handberg, Rasmus and Hon, Marc and Kane, Stephen R. and Kawaler, Steven D. and Kuszlewicz, James S. and Lucas, Miles and Mathur, Savita and Nardetto, Nicolas and Nielsen, Martin B. and Pinsonneault, Marc H. and Reffert, Sabine and Silva Aguirre, V{\'i}ctor and Stassun, Keivan G. and Stello, Dennis and Stock, Stephan and Vrard, Mathieu and Y{\i}ld{\i}z, Mutlu and Chaplin, William J. and Huber, Daniel and Bean, Jacob L. and {\c C}elik Orhan, Zeynep and Cunha, Margarida S. and {Christensen-Dalsgaard}, J{\o}rgen and Kjeldsen, Hans and Metcalfe, Travis S. and Miglio, Andrea and Monteiro, M{\'a}rio J. P. F. G. and Nsamba, Benard and {\"O}rtel, Sibel and Pereira, Filipe and Sousa, S{\'e}rgio G. and Tsantaki, Maria and Turnbull, Margaret C.},
  year = {2019},
  month = sep,
  pages = {arXiv:1909.05961},
  abstract = {The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets that transit bright stars. In addition, its excellent photometric precision enables asteroseismology of solar-type and red-giant stars, which exhibit convection-driven, solar-like oscillations. Simulations predict that TESS will detect solar-like oscillations in nearly 100 stars already known to host planets. In this paper, we present an asteroseismic analysis of the known red-giant host stars HD 212771 and HD 203949, both systems having a long-period planet detected through radial velocities. These are the first detections of oscillations in previously known exoplanet-host stars by TESS, further showcasing the mission's potential to conduct asteroseismology of red-giant stars. We estimate the fundamental properties of both stars through a grid-based modeling approach that uses global asteroseismic parameters as input. We discuss the evolutionary state of HD 203949 in depth and note the large discrepancy between its asteroseismic mass (\$M\_\textbackslash ast = 1.23 \textbackslash pm 0.15\textbackslash,\{\textbackslash rm M\}\_\textbackslash odot\$ if on the red-giant branch or \$M\_\textbackslash ast = 1.00 \textbackslash pm 0.16\textbackslash,\{\textbackslash rm M\}\_\textbackslash odot\$ if in the clump) and the mass quoted in the discovery paper (\$M\_\textbackslash ast = 2.1 \textbackslash pm 0.1\textbackslash,\{\textbackslash rm M\}\_\textbackslash odot\$), implying a change \$\>30\textbackslash,\textbackslash\%\$ in the planet's mass. Assuming HD 203949 to be in the clump, we investigate the planet's past orbital evolution and discuss how it could have avoided engulfment at the tip of the red-giant branch. Finally, HD 212771 was observed by K2 during its Campaign 3, thus allowing for a preliminary comparison of the asteroseismic performances of TESS and K2. We estimate the ratio of the observed oscillation amplitudes for this star to be \$A\_\{\textbackslash rm max\}\^\{\textbackslash rm TESS\}/A\_\{\textbackslash rm max\}\^\{\textbackslash rm K2\} = 0.75 \textbackslash pm 0.14\$, consistent with the expected ratio of \$\textbackslash sim0.85\$ due to the redder bandpass of TESS.},
  file = {/Users/Oliver/Zotero/storage/44XC2Z2L/Campante et al. - 2019 - TESS Asteroseismology of the known red-giant host .pdf;/Users/Oliver/Zotero/storage/K4XXC944/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{campante2016,
  title = {On the Detectability of Solar-like Oscillations with the {{NASA TESS}} Mission},
  author = {Campante, Tiago L.},
  year = {2016},
  month = oct,
  abstract = {The upcoming NASA TESS mission will perform an all-sky survey for planets transiting bright nearby stars. In addition, its excellent photometric precision will enable asteroseismology of solar-type and red-giant stars. We apply a newly developed detection test along a sequence of stellar evolutionary tracks in order to predict the detectability of solar-like oscillations with TESS.},
  archivePrefix = {arXiv},
  eprint = {1610.06460},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/2DJUSMBX/Campante - 2016 - On the detectability of solar-like oscillations wi.pdf;/Users/Oliver/Zotero/storage/E2JSGM99/1610.html},
  journal = {arXiv:1610.06460 [astro-ph]},
  keywords = {AR 01/11/16,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{campante2017,
  title = {{{TESS}} Asteroseismology of {{CHEOPS}} Prime Targets},
  author = {Campante, T.},
  year = {2017},
  month = jul,
  pages = {41},
  file = {/Users/Oliver/Zotero/storage/XTYVW82N/Campante - 2017 - TESS asteroseismology of CHEOPS prime targets.pdf;/Users/Oliver/Zotero/storage/LSJIC9AY/abstract.html},
  journal = {CHEOPS Fifth Science Workshop},
  language = {en}
}

@article{cannon1970,
  title = {Red Giants in Old Open Clusters.},
  author = {Cannon, R. D.},
  year = {1970},
  month = jan,
  volume = {150},
  pages = {111},
  doi = {10.1093/mnras/150.1.111},
  abstract = {A detailed comparison is made between the predictions of stellar evolution calculations and the observations of red giants in old open clusters. Colour- magnitude diagrams are presented for several such clusters, in which relative proper motions have been used to eliminate non-members. The published observations of other old clusters are suinmarized. A prominent feature of all these clusters is a' clump `of red giants, centred near Mv = + I, B-V = +i.o, which is tentatively identified with the horizontal branch found in globular clusters. Comparison with various theoretical calculations, mostly by I. Iben and J. Faulkner, supports this identification and indicates that the stars have a helium-burning core surrounded by a hydrogen-burning shell. The near constancy of the absolute magnitude of the clump is then interpreted as observational evidence for the occurrence of electron degeneracy in the cores of low mass red giants. The use of the clump for crude determinations of cluster distances and reddening, and as evidence of the internal composition of the stars, is advocated. Finally, it is suggested that a large number of field red giants may be in the helium-burning phase of evolution some of which may be used to investigate mass loss and internal mixing in evolving stars.},
  file = {/Users/Oliver/Zotero/storage/DUEAA7JA/Cannon - 1970 - Red giants in old open clusters..pdf;/Users/Oliver/Zotero/storage/R33VMZF5/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en}
}

@article{cantat-gaudin+2018,
  title = {A {{Gaia DR2}} View of the {{Open Cluster}} Population in the {{Milky Way}}},
  author = {{Cantat-Gaudin}, T. and Jordi, C. and Vallenari, A. and Bragaglia, A. and {Balaguer-N{\'u}{\~n}ez}, L. and Soubiran, C. and Bossini, D. and Moitinho, A. and {Castro-Ginard}, A. and {Krone-Martins}, A. and Casamiquela, L. and Sordo, R. and Carrera, R.},
  year = {2018},
  month = may,
  pages = {arXiv:1805.08726},
  abstract = {Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second Gaia data release contains precise astrometry at the sub-milliarcsecond level and homogeneous photometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky. In this study we aim to a establish list of members and derive mean parameters, in particular distances, for as many clusters as possible, making use of Gaia data alone. We compile a list of thousands of known or putative clusters from the literature. We then apply an unsupervised membership assignment code, UPMASK, to the Gaia DR2 data contained within the fields of those clusters. We obtained a list of members and cluster parameters for 1229 clusters. As expected, the youngest clusters are seen to be tightly distributed near the Galactic plane and to trace the spiral arms of the Milky Way, while older objects are more uniformly distributed, deviate further from the plane, and tend to be located at larger Galactocentric distances. Thanks to the quality of GaiaDR2 astrometry, the fully homogeneous parameters derived in this study are the most precise to date. Furthermore, we report on the serendipitous discovery of 60 new open clusters in the fields analysed during this study.},
  file = {/Users/Oliver/Zotero/storage/VC9UNBFN/Cantat-Gaudin et al. - 2018 - A Gaia DR2 view of the Open Cluster population in .pdf;/Users/Oliver/Zotero/storage/M2IGC9AK/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{cardelli+1989,
  title = {The Relationship between Infrared, Optical, and Ultraviolet Extinction},
  author = {Cardelli, Jason A. and Clayton, Geoffrey C. and Mathis, John S.},
  year = {1989},
  month = oct,
  volume = {345},
  pages = {245--256},
  issn = {0004-637X},
  doi = {10.1086/167900},
  abstract = {The parameterized extinction data of Fitzpatrick and Massa (1986, 1988) for the ultraviolet and various sources for the optical and
near-infrared are used to derive a meaningful average extinction law over the 3.5 micron to 0.125 wavelength range which is applicable to both diffuse and dense regions of the interstellar medium. The law depends on only one parameter R(V) = A(V)/E(B-V). An analytic formula is given for the mean extinction law which can be used to calculate color excesses or to deredden observations. The validity of the law over a large wavelength interval suggests that the processes which modify the sizes and compositions of grains are stochastic in nature and very efficient.},
  file = {/Users/Oliver/Zotero/storage/V2VTVTU3/nph-iarticle_query.pdf},
  journal = {The Astrophysical Journal},
  keywords = {C4}
}

@article{cardoso+2018,
  title = {Lightkurve: {{Kepler}} and {{TESS}} Time Series Analysis in {{Python}}},
  shorttitle = {Lightkurve},
  author = {Cardoso, Jos{\'e} Vin{\'i}cius de Miranda and {Gully-Santiago}, Michael and Saunders, Nicholas and Cody, Ann Marie and Barclay, Thomas and Hall, Oliver and Sagear, Sheila and Turtelboom, Emma and Zhang, Johnny and Tzanidakis, Andy and Mighell, Ken and Coughlin, Jeff and Bell, Keaton and {Berta-Thompson}, Zach and Williams, Peter and Dotson, Jessie and Barentsen, Geert},
  year = {2018},
  month = dec,
  pages = {ascl:1812.013},
  abstract = {Lightkurve analyzes astronomical flux time series data, in particular the pixels and light curves obtained by NASA's Kepler, K2, and TESS exoplanet missions. This community-developed Python package is designed to be user friendly to lower the barrier for students, astronomers, and citizen scientists interested in analyzing data from these missions. Lightkurve provides easy tools to download, inspect, and analyze time series data and its documentation is supported by a large syllabus of tutorials.},
  file = {/Users/Oliver/Zotero/storage/P2FB7BYD/abstract.html},
  journal = {Astrophysics Source Code Library},
  language = {en}
}

@article{carpenter+2017,
  title = {Stan: {{A Probabilistic Programming Language}}},
  shorttitle = {Stan},
  author = {Carpenter, Bob and Gelman, Andrew and Hoffman, Matthew D. and Lee, Daniel and Goodrich, Ben and Betancourt, Michael and Brubaker, Marcus and Guo, Jiqiang and Li, Peter and Riddell, Allen},
  year = {2017},
  month = jan,
  volume = {76},
  pages = {1--32},
  issn = {1548-7660},
  doi = {10.18637/jss.v076.i01},
  copyright = {Copyright (c) 2017 Bob Carpenter, Andrew Gelman, Matthew D. Hoffman, Daniel Lee, Ben Goodrich, Michael Betancourt, Marcus Brubaker, Jiqiang Guo, Peter Li, Allen Riddell},
  file = {/Users/Oliver/Zotero/storage/UFEVNAC8/Carpenter et al. - 2017 - Stan A Probabilistic Programming Language.pdf;/Users/Oliver/Zotero/storage/3EHCGMPI/v076i01.html},
  journal = {Journal of Statistical Software},
  keywords = {algorithmic differentiation,Bayesian inference,probabilistic programming,Stan},
  language = {en},
  number = {1}
}

@article{carrier+2005,
  title = {New Seismological Results on the {{G0 IV}} {$\eta$} {{Bootis}}},
  author = {Carrier, F. and Eggenberger, P. and Bouchy, F.},
  year = {2005},
  month = may,
  volume = {434},
  pages = {1085--1095},
  issn = {0004-6361},
  doi = {10.1051/0004-6361:20042140},
  abstract = {Several attempts have been made to detect solar-like oscillations in the G0 IV star {$\eta$} Boo. We present here new
observations on this star simultaneously conducted with two
spectrographs: Coralie mounted on the 1.2-m Swiss telescope at the ESO La Silla Observatory (Chile) and Elodie based on the 1.93-m telescope at the Observatoire de Haute-Provence (France). In total, 1239 spectra were collected over 13 nights. The power spectrum of the high precision velocity time series clearly presents several identifiable peaks between 0.4 and 1.0 mHz showing regularity with a large and small separation of {$\Delta\nu$} = 39.9 {$\mu$}Hz and {$\delta\nu$}02 = 3.95 {$\mu$}Hz
respectively. Twenty-two individual frequencies have been identified. Detailed models based on these measurements and non-asteroseismic observables were computed using the Geneva evolution code including shellular rotation and atomic diffusion. By combining these
seismological data with non-asteroseismic observations, we determine the following global parameters for {$\eta$} Boo: a mass of 1.57 {$\pm$} 0.07 M{$\odot$}, an age t=2.67 {$\pm$} 0.10 Gyr
and an initial metallicity (Z/X)i=0.0391 {$\pm$} 0.0070. We also show that the mass of {$\eta$} Boo is very
sensitive to the choice of the observed metallicity, while the age of {$\eta$} Boo depends on the input physics used. Indeed, a higher metallicity favours a higher mass, while non-rotating models without overshooting predict a smaller age.},
  file = {/Users/Oliver/Zotero/storage/Y6GHE3SL/Carrier et al. - 2005 - New seismological results on the G0 IV η Bootis.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {stars variables: general,stars: fundamental parameters,stars: individual: η Boo,techniques: radial velocities}
}

@article{casagrande+2014,
  title = {Str\"omgren {{Survey}} for {{Asteroseismology}} and {{Galactic Archaeology}}: {{Let}} the {{SAGA Begin}}},
  shorttitle = {Str\"omgren {{Survey}} for {{Asteroseismology}} and {{Galactic Archaeology}}},
  author = {Casagrande, L. and Silva Aguirre, V. and Stello, D. and Huber, D. and Serenelli, A. M. and Cassisi, S. and Dotter, A. and Milone, A. P. and Hodgkin, S. and Marino, A. F. and Lund, M. N. and Pietrinferni, A. and Asplund, M. and Feltzing, S. and Flynn, C. and Grundahl, F. and Nissen, P. E. and Sch{\"o}nrich, R. and Schlesinger, K. J. and Wang, W.},
  year = {2014},
  month = jun,
  volume = {787},
  pages = {110},
  doi = {10.1088/0004-637X/787/2/110},
  abstract = {Asteroseismology has the capability of precisely determining stellar properties that would otherwise be inaccessible, such as radii, masses, and thus ages of stars. When coupling this information with classical determinations of stellar parameters, such as metallicities, effective temperatures, and angular diameters, powerful new diagnostics for Galactic studies can be obtained. The ongoing Str\"omgren survey for Asteroseismology and Galactic Archaeology has the goal of transforming the Kepler field into a new benchmark for Galactic studies, similar to the solar neighborhood. Here we present the first results from a stripe centered at a Galactic longitude of 74\textdegree{} and covering latitude from about 8\textdegree{} to 20\textdegree, which includes almost 1000 K giants with seismic information and the benchmark open cluster NGC 6819. We describe the coupling of classical and seismic parameters, the accuracy as well as the caveats of the derived effective temperatures, metallicities, distances, surface gravities, masses, and radii. Confidence in the achieved precision is corroborated by the detection of the first and secondary clumps in a population of field stars with a ratio of 2 to 1 and by the negligible scatter in the seismic distances among NGC 6819 member stars. An assessment of the reliability of stellar parameters in the Kepler Input Catalog is also performed, and the impact of our results for population studies in the Milky Way is discussed, along with the importance of an all-sky Str\"omgren survey. Based on observations made with the Isaac Newton Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\'isica de Canarias.},
  file = {/Users/Oliver/Zotero/storage/4XSZN2DY/Casagrande et al. - 2014 - Strömgren Survey for Asteroseismology and Galactic.pdf;/Users/Oliver/Zotero/storage/WKE74XX2/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{casagrande+2016,
  title = {Measuring the Vertical Age Structure of the {{Galactic}} Disc Using Asteroseismology and {{SAGA}}},
  author = {Casagrande, L. and Silva Aguirre, V. and Schlesinger, K. J. and Stello, D. and Huber, D. and Serenelli, A. M. and Sch{\"o}nrich, R. and Cassisi, S. and Pietrinferni, A. and Hodgkin, S. and Milone, A. P. and Feltzing, S. and Asplund, M.},
  year = {2016},
  month = jan,
  volume = {455},
  pages = {987},
  doi = {10.1093/mnras/stv2320},
  abstract = {The existence of a vertical age gradient in the Milky Way disc has been indirectly known for long. Here, we measure it directly for the first time with seismic ages, using red giants observed by Kepler. We use Str\"omgren photometry to gauge the selection function of asteroseismic targets, and derive colour and magnitude limits where giants with measured oscillations are representative of the underlying population in the field. Limits in the 2MASS system are also derived. We lay out a method to assess and correct for target selection effects independent of Galaxy models. We find that low-mass, I.e. old red giants dominate at increasing Galactic heights, whereas closer to the Galactic plane they exhibit a wide range of ages and metallicities. Parametrizing this as a vertical gradient returns approximately 4 Gyr kpc\textsuperscript{-1} for the disc we probe, although with a large dispersion of ages at all heights. The ages of stars show a smooth distribution over the last {$\simeq$}10 Gyr, consistent with a mostly quiescent evolution for the Milky Way disc since a redshift of about 2. We also find a flat age-metallicity relation for disc stars. Finally, we show how to use secondary clump stars to estimate the present-day intrinsic metallicity spread, and suggest using their number count as a new proxy for tracing the ageing of the disc. This work highlights the power of asteroseismology for Galactic studies; however, we also emphasize the need for better constraints on stellar mass-loss, which is a major source of systematic age uncertainties in red giant stars.},
  file = {/Users/Oliver/Zotero/storage/PE7PM43D/Casagrande et al. - 2016 - Measuring the vertical age structure of the Galact.pdf;/Users/Oliver/Zotero/storage/CI53V5WI/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{casagrande+vandenberg2014,
  title = {Synthetic Stellar Photometry - {{I}}. {{General}} Considerations and New Transformations for Broad-Band Systems},
  author = {Casagrande, L. and VandenBerg, Don A.},
  year = {2014},
  month = oct,
  volume = {444},
  pages = {392},
  doi = {10.1093/mnras/stu1476},
  abstract = {After a pedagogical introduction to the main concepts of synthetic photometry, colours and bolometric corrections in the Johnson-Cousins, 2MASS, and HST-ACS/WFC3 photometric systems are generated from MARCS synthetic fluxes for various [Fe/H] and [{$\alpha$}/Fe] combinations, and virtually any value of E(B - V) {$\lessequivlnt$} 0.7. The successes and failures of model fluxes in reproducing the observed magnitudes are highlighted. Overall, extant synthetic fluxes predict quite realistic broad-band colours and bolometric corrections, especially at optical and longer wavelengths: further improvements of the predictions for the blue and ultraviolet spectral regions await the use of hydrodynamic models where the microturbulent velocity is not treated as a free parameter. We show how the morphology of the colour-magnitude diagram (CMD) changes for different values of [Fe/H] and [{$\alpha$}/Fe]; in particular, how suitable colour combinations can easily discriminate between red giant branch and lower main-sequence populations with different [{$\alpha$}/Fe], due to the concomitant loops and swings in the CMD. We also provide computer programs to produce tables of synthetic bolometric corrections as well as routines to interpolate in them. These colour-T\textsubscript{eff}-metallicity relations may be used to convert isochrones for different chemical compositions to various bandpasses assuming observed reddening values, thus bypassing the standard assumption of a constant colour excess for stars of different spectral type. We also show how such an assumption can lead to significant systematic errors. The MARCS transformations presented in this study promise to provide important constraints on our understanding of the multiple stellar populations found in globular clusters (e.g. the colours of lower main-sequence stars are predicted to depend strongly on [{$\alpha$}/Fe]) and of those located towards/in the Galactic bulge.},
  file = {/Users/Oliver/Zotero/storage/P3DJZCQ8/Casagrande and VandenBerg - 2014 - Synthetic stellar photometry - I. General consider.pdf;/Users/Oliver/Zotero/storage/7CLK3V97/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{casagrande+vandenberg2018,
  title = {Synthetic {{Stellar Photometry}} - {{II}}. {{Testing}} the Bolometric Flux Scale and Tables of Bolometric Corrections for the {{Hipparcos}}/{{Tycho}}, {{Pan}}-{{STARRS1}}, {{SkyMapper}}, and {{JWST}} Systems},
  author = {Casagrande, L. and VandenBerg, Don A.},
  year = {2018},
  month = apr,
  volume = {475},
  pages = {5023},
  doi = {10.1093/mnras/sty149},
  abstract = {We use MARCS model atmosphere fluxes to compute synthetic colours, bolometric corrections and reddening coefficients for the Hipparcos/Tycho, Pan-STARRS1, SkyMapper, and JWST systems. Tables and interpolation subroutines are provided to transform isochrones from the theoretical to various observational planes, to derive bolometric corrections, synthetic colours and colour-temperature relations at nearly any given point of the HR diagram for 2600 K {$\leq$} T\textsubscript{eff} {$\leq$} 8000 K, and different values of reddening in 85 photometric filters. We use absolute spectrophotometry from the CALSPEC library to show that bolometric fluxes can be recovered to{\~ }2 per cent from bolometric corrections in a single band, when input stellar parameters are well known for FG dwarfs at various metallicities. This sole source of uncertainty impacts interferometric T\textsubscript{eff} to {$\simeq$}0.5 per cent (or 30 K at the solar temperature). Uncertainties are halved when combining bolometric corrections in more bands, and limited by the fundamental uncertainty of the current absolute flux scale at 1 per cent. Stars in the RAVE DR5 catalogue are used to validate the quality of our MARCS synthetic photometry in selected filters across the optical and infrared range. This investigation shows that extant MARCS synthetic fluxes are able to reproduce the main features observed in stellar populations across the Galactic disc.},
  file = {/Users/Oliver/Zotero/storage/95B6NDSK/Casagrande and VandenBerg - 2018 - Synthetic Stellar Photometry - II. Testing the bol.pdf;/Users/Oliver/Zotero/storage/LHWGTFV3/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {4}
}

@article{casagrande+vandenberg2018a,
  title = {On the Use of {{Gaia}} Magnitudes and New Tables of Bolometric Corrections},
  author = {Casagrande, L. and VandenBerg, Don A.},
  year = {2018},
  month = sep,
  volume = {479},
  pages = {L102},
  doi = {10.1093/mnrasl/sly104},
  abstract = {The availability of reliable bolometric corrections and reddening estimates, rather than the quality of parallaxes, will be one of the main limiting factors in determining the luminosities of a large fraction of Gaia stars. With this goal in mind, we provide GaiaG\textsubscript{BP}, G, and G\textsubscript{RP} synthetic photometry for the entire MARCS grid and test the performance of our synthetic colours and bolometric corrections against space-borne absolute spectrophotometry. We find indication of a magnitude-dependent offset in Gaia DR2 G magnitudes, which must be taken into account in high-accuracy investigations. Our interpolation routines are easily used to derive bolometric corrections at desired stellar parameters and to explore the dependence of Gaia photometry on T\textsubscript{eff}, log g, \{[Fe/H]\}, [{$\alpha$} /\{Fe\}], and E(B - V). Gaia colours for the Sun and Vega, and T\textsubscript{eff}-dependent extinction coefficients are also provided.},
  file = {/Users/Oliver/Zotero/storage/2GVXJFTQ/Casagrande and VandenBerg - 2018 - On the use of Gaia magnitudes and new tables of bo.pdf;/Users/Oliver/Zotero/storage/XFYG4PVM/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{casagrande+vandenberg2018b,
  title = {{{BCcodes}}: {{Bolometric Corrections}} and {{Synthetic Stellar Photometry}}},
  shorttitle = {{{BCcodes}}},
  author = {Casagrande, Luca and VandenBerg, Don A.},
  year = {2018},
  month = may,
  pages = {ascl:1805.022},
  abstract = {BCcodes computes bolometric corrections and synthetic colors in up to 5 filters for input values of the stellar parameters Teff, log(g), [Fe/H], E(B-V) and [alpha/Fe].},
  file = {/Users/Oliver/Zotero/storage/RK2HU66C/ui.adsabs.harvard.edu.html},
  journal = {Astrophysics Source Code Library},
  language = {en}
}

@article{casey+2016,
  title = {The {{Gaia}}-{{ESO Survey}}: Revisiting the {{Li}}-Rich Giant Problem},
  shorttitle = {The {{Gaia}}-{{ESO Survey}}},
  author = {Casey, A. R. and Ruchti, G. and Masseron, T. and Randich, S. and Gilmore, G. and Lind, K. and Kennedy, G. M. and Koposov, S. E. and Hourihane, A. and Franciosini, E. and Lewis, J. R. and Magrini, L. and Morbidelli, L. and Sacco, G. G. and Worley, C. C. and Feltzing, S. and Jeffries, R. D. and Vallenari, A. and Bensby, T. and Bragaglia, A. and Flaccomio, E. and Francois, P. and Korn, A. J. and Lanzafame, A. and Pancino, E. and {Recio-Blanco}, A. and Smiljanic, R. and Carraro, G. and Costado, M. T. and Damiani, F. and Donati, P. and Frasca, A. and Jofr{\'e}, P. and Lardo, C. and {de Laverny}, P. and Monaco, L. and Prisinzano, L. and Sbordone, L. and Sousa, S. G. and Tautvai{\v s}ien{\.e}, G. and Zaggia, S. and Zwitter, T. and Delgado Mena, E. and Chorniy, Y. and Martell, S. L. and Silva Aguirre, V. and Miglio, A. and Chiappini, C. and Montalban, J. and Morel, T. and Valentini, M.},
  year = {2016},
  month = sep,
  volume = {461},
  pages = {3336--3352},
  issn = {0035-8711},
  doi = {10.1093/mnras/stw1512},
  abstract = {The discovery of lithium-rich giants contradicts expectations from canonical stellar evolution. Here we report on the serendipitous discovery of 20 Li-rich giants observed during the Gaia-ESO Survey, which includes the first nine Li-rich giant stars known towards the CoRoT fields. Most of our Li-rich giants have near-solar metallicities and stellar parameters consistent with being before the luminosity bump. This is difficult to reconcile with deep mixing models proposed to explain lithium enrichment, because these models can only operate at later evolutionary stages: at or past the luminosity bump. In an effort to shed light on the Li-rich phenomenon, we highlight recent evidence of the tidal destruction of close-in hot Jupiters at the sub-giant phase. We note that when coupled with models of planet accretion, the observed destruction of hot Jupiters actually predicts the existence of Li-rich giant stars, and suggests that Li-rich stars should be found early on the giant branch and occur more frequently with increasing metallicity. A comprehensive review of all known Li-rich giant stars reveals that this scenario is consistent with the data. However, more evolved or metal-poor stars are less likely to host close-in giant planets, implying that their Li-rich origin requires an alternative explanation, likely related to mixing scenarios rather than external phenomena.},
  file = {/Users/Oliver/Zotero/storage/QECJDCSR/Casey et al. - 2016 - The Gaia-ESO Survey revisiting the Li-rich giant .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {stars: abundances}
}

@article{cassisi+2011,
  title = {On the Magnitude Difference between the Main Sequence Turn off and the Red Giant Branch Bump in {{Galactic}} Globular Clusters},
  author = {Cassisi, Santi and {Marin-Franch}, Antonio and Salaris, Maurizio and Aparicio, Antonio and Monelli, Matteo and Pietrinferni, Adriano},
  year = {2011},
  month = mar,
  volume = {527},
  pages = {A59},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201016066},
  abstract = {We present new measurements of the magnitude of the main sequence turn off and the red giant branch bump in the luminosity function of a sample of Galactic globular clusters with updated estimates of [Fe/H] and [\$\textbackslash alpha\$/Fe], employing photometric data collected with the Advanced Camera for Survey on board the HST. We compare measured and predicted values of the magnitude difference between these two features, a rarely employed diagnostic of the internal structure of low-mass stars at the beginning of their red giant evolution. Our analysis discloses a clear discrepancy between theory and observations, the theoretical red giant branch bump magnitudes being too bright by on average \$\textbackslash sim0.2\$\textasciitilde mag. This corroborates results from the more widely studied magnitude difference between horizontal branch and red giant bump, avoiding the well known problems associated to the determination of the horizontal branch level from colour magnitude diagrams, and to uncertainties in the luminosity of horizontal branch stellar models. We briefly discuss several potential solutions of this discrepancy.},
  archivePrefix = {arXiv},
  eprint = {1012.0419},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/ICT26DUA/Cassisi et al. - 2011 - On the magnitude difference between the main seque.pdf;/Users/Oliver/Zotero/storage/DJSMPEGW/1012.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{castellani+2000,
  title = {The Puzzling Theoretical Predictions for the Luminosity of Clumping {{He}} Burning Stars},
  author = {Castellani, V. and Degl'Innocenti, S. and Girardi, L. and Marconi, M. and Prada Moroni, P. G. and Weiss, A.},
  year = {2000},
  month = feb,
  volume = {354},
  pages = {150},
  abstract = {This paper deals with theoretical predictions for He burning models in a range of masses covering the so-called Red Giant Branch phase transition. Taking as a guideline the observational constraints given by Hipparcos parallaxes to the predicted luminosity of models originated from Red Giant progenitors with He core undergoing electron degeneracy, we compare models by various authors as recently appeared in the literature, disclosing sensitive differences in the predicted luminosity. The ``solidity" of these theoretical predictions is investigated by exploring the effects of varying the assumptions about the efficiency of core overshooting or the amount of mass loss, giving quantitative estimates of the related uncertainties. However, one finds that theoretical predictions concerning the luminosity of the red giant clump in the Hipparcos sample is scarcely affected by these mechanisms. \{ A comparison among theoretical predictions as recently given by different authors convincingly demonstrates that the different luminosity predictions are the natural results of evolutionary codes with different - but all reasonable- input physics.\} In this context observations suggests that stellar models based on the ``most updated" input physics are possibly overestimating the luminosity of these structures, raising doubts on several current predictions concerning the luminosity of HB stars in galactic globulars.},
  file = {/Users/Oliver/Zotero/storage/RVHNMGTG/Castellani et al. - 2000 - The puzzling theoretical predictions for the lumin.pdf;/Users/Oliver/Zotero/storage/QRX58A7E/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{ceillier+2016,
  title = {Rotation Periods and Seismic Ages of {{KOIs}} - Comparison with Stars without Detected Planets from {{Kepler}} Observations},
  author = {Ceillier, T. and {van Saders}, J. and Garc{\'i}a, R. A. and Metcalfe, T. S. and Creevey, O. and Mathis, S. and Mathur, S. and Pinsonneault, M. H. and Salabert, D. and Tayar, J.},
  year = {2016},
  month = feb,
  volume = {456},
  pages = {119--125},
  issn = {0035-8711},
  doi = {10.1093/mnras/stv2622},
  abstract = {One of the most difficult properties to derive for stars is their age.
For cool main-sequence stars, gyrochronology relations can be used to
infer stellar ages from measured rotation periods and Hertzsprung
Russell diagram positions. These relations have few calibrators with
known ages for old, long rotation period stars. There is a significant
sample of old Kepler objects of interest, or KOIs, which have both
measurable surface rotation periods and precise asteroseismic
measurements from which ages can be accurately derived. In this work, we
determine the age and the rotation period of solar-like pulsating KOIs
to both compare the rotation properties of stars with and without known
planets and enlarge the gyrochronology calibration sample for old stars.
We use Kepler photometric light curves to derive the stellar surface
rotation periods while ages are obtained with asteroseismology using the
Asteroseismic Modelling Portal in which individual mode frequencies are
combined with high-resolution spectroscopic parameters. We thus
determine surface rotation periods and ages for 11 planet-hosting stars,
all over 2 Gyr old. We find that the planet-hosting stars exhibit a
rotational behaviour that is consistent with the latest age-rotation
models and similar to the rotational behaviour of stars without detected
planets. We conclude that these old KOIs can be used to test and
calibrate gyrochronology along with stars not known to host planets.},
  file = {/Users/Oliver/Zotero/storage/KMACE3ZL/Ceillier et al. - 2016 - Rotation periods and seismic ages of KOIs - compar.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {planet-star interactions,stars: evolution,stars: oscillations,stars: rotation}
}

@article{chan+bovy2019,
  title = {The \textbackslash emph\{\vphantom\}{{Gaia}}\vphantom\{\} {{DR2}} Parallax Zero Point: {{Hierarchical}} Modeling of Red Clump Stars},
  shorttitle = {The \textbackslash emph\{\vphantom\}{{Gaia}}\vphantom\{\} {{DR2}} Parallax Zero Point},
  author = {Chan, Victor C. and Bovy, Jo},
  year = {2019},
  month = oct,
  pages = {arXiv:1910.00398},
  abstract = {The systematic offset of \textbackslash emph\{Gaia\} parallaxes has been widely reported with \textbackslash emph\{Gaia\}'s second data release, and it is expected to persist in future \textbackslash emph\{Gaia\} data. In order to use \textbackslash emph\{Gaia\} parallaxes to infer distances to high precision, we develop a hierarchical probabilistic model to determine the \textbackslash emph\{Gaia\} parallax zero point offset along with the calibration of an empirical model for luminosity of red clump stars by combining astrometric and photometric measurements. Using a cross-matched sample of red clump stars from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and \textbackslash emph\{Gaia\} Data Release 2 (DR2), we report the parallax zero point offset in DR2 to be \$ \textbackslash varpi\_0 = -48 \textbackslash pm 1\textasciitilde\textbackslash mu\textbackslash text\{as\} \$. We infer the red clump absolute magnitude to be \$ -1.622 \textbackslash pm 0.004 \$ in \$ K\_s \$, \$ 0.517 \textbackslash pm 0.004 \$ in \$ G \$, \$ -1.019 \textbackslash pm 0.004 \$ in \$ J \$, and \$ -1.516 \textbackslash pm 0.004 \$ in \$ H \$. The intrinsic scatter of the red clump is \$ \textbackslash sim 0.09 \$ mag in \$ J \$, \$ H \$ and \$ K\_s \$, or \$ \textbackslash sim 0.17 \$ mag in \$ G \$. We tailor our models to accommodate more complex analyses such as investigating the variations of the parallax zero point with each source's observed magnitude, observed colour, and sky position. In particular, we find fluctuations of the zero point across the sky to be of order or less than a few 10s of \$ \textbackslash mu\textbackslash text\{as\} \$.},
  file = {/Users/Oliver/Zotero/storage/WIJ4DGAP/Chan and Bovy - 2019 - The emph Gaia DR2 parallax zero point Hierarchi.pdf;/Users/Oliver/Zotero/storage/3UUU7K92/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{chaplin+1999,
  title = {Rotation of the Solar Core from {{BiSON}} and {{LOWL}} Frequency Observations},
  author = {Chaplin, W. J. and {Christensen-Dalsgaard}, J. and Elsworth, Y. and Howe, R. and Isaak, G. R. and Larsen, R. M. and New, R. and Schou, J. and Thompson, M. J. and Tomczyk, S.},
  year = {1999},
  month = sep,
  volume = {308},
  pages = {405--414},
  issn = {0035-8711},
  doi = {10.1046/j.1365-8711.1999.02691.x},
  abstract = {Determination of the rotation of the solar core requires very accurate data on splittings for the low-degree modes which penetrate to the core, as well as for modes of higher degree to suppress the contributions from the rest of the Sun to the splittings of the low-degree modes. Here we combine low-degree data based on 32 months of observations with the BiSON network and data from the LOWL instrument. The data are analysed with a technique that specifically aims at obtaining an inference of rotation that is localized to the core. Our analysis provides what we believe is the most stringent constraint to date on the rotation of the deep solar interior.},
  file = {/Users/Oliver/Zotero/storage/UJ5BLLBA/Chaplin et al. - 1999 - Rotation of the solar core from BiSON and LOWL fre.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society}
}

@article{chaplin+2010,
  title = {The {{Asteroseismic Potential}} of {{Kepler}}: {{First Results}} for {{Solar}}-{{Type Stars}}},
  shorttitle = {The {{Asteroseismic Potential}} of {{Kepler}}},
  author = {Chaplin, W. J. and Appourchaux, T. and Elsworth, Y. and Garc{\'i}a, R. A. and Houdek, G. and Karoff, C. and Metcalfe, T. S. and {Molenda-{\.Z}akowicz}, J. and Monteiro, M. J. P. F. G. and Thompson, M. J. and Brown, T. M. and {Christensen-Dalsgaard}, J. and Gilliland, R. L. and Kjeldsen, H. and Borucki, W. J. and Koch, D. and Jenkins, J. M. and Ballot, J. and Basu, S. and Bazot, M. and Bedding, T. R. and Benomar, O. and Bonanno, A. and Brand{\~a}o, I. M. and Bruntt, H. and Campante, T. L. and Creevey, O. L. and Mauro, Di and P, M. and Do{\v g}an, G. and Dreizler, S. and Eggenberger, P. and Esch, L. and Fletcher, S. T. and Frandsen, S. and Gai, N. and Gaulme, P. and Handberg, R. and Hekker, S. and Howe, R. and Huber, D. and Korzennik, S. G. and Lebrun, J. C. and Leccia, S. and Martic, M. and Mathur, S. and Mosser, B. and New, R. and Quirion, P.-O. and R{\'e}gulo, C. and Roxburgh, I. W. and Salabert, D. and Schou, J. and Sousa, S. G. and Stello, D. and Verner, G. A. and Arentoft, T. and Barban, C. and Belkacem, K. and Benatti, S. and Biazzo, K. and Boumier, P. and Bradley, P. A. and Broomhall, A.-M. and Buzasi, D. L. and Claudi, R. U. and Cunha, M. S. and D'Antona, F. and Deheuvels, S. and Derekas, A. and Garc{\'i}a Hern{\'a}ndez, A. and Giampapa, M. S. and Goupil, M. J. and Gruberbauer, M. and Guzik, J. A. and Hale, S. J. and Ireland, M. J. and Kiss, L. L. and Kitiashvili, I. N. and Kolenberg, K. and Korhonen, H. and Kosovichev, A. G. and Kupka, F. and Lebreton, Y. and Leroy, B. and Ludwig, H.-G. and Mathis, S. and Michel, E. and Miglio, A. and Montalb{\'a}n, J. and Moya, A. and Noels, A. and Noyes, R. W. and Pall{\'e}, P. L. and Piau, L. and Preston, H. L. and Roca Cort{\'e}s, T. and Roth, M. and Sato, K. H. and Schmitt, J. and Serenelli, A. M. and Silva Aguirre, V. and Stevens, I. R. and Su{\'a}rez, J. C. and Suran, M. D. and Trampedach, R. and {Turck-Chi{\`e}ze}, S. and Uytterhoeven, K. and Ventura, R. and Wilson, P. A.},
  year = {2010},
  month = apr,
  volume = {713},
  pages = {L169},
  doi = {10.1088/2041-8205/713/2/L169},
  abstract = {We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: about 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses, and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe.},
  file = {/Users/Oliver/Zotero/storage/TQFUPGMS/Chaplin et al. - 2010 - The Asteroseismic Potential of Kepler First Resul.pdf;/Users/Oliver/Zotero/storage/CHXY5EHN/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{chaplin+2011,
  title = {Ensemble {{Asteroseismology}} of {{Solar}}-{{Type Stars}} with the {{NASA Kepler Mission}}},
  author = {Chaplin, W. J. and Kjeldsen, H. and {Christensen-Dalsgaard}, J. and Basu, S. and Miglio, A. and Appourchaux, T. and Bedding, T. R. and Elsworth, Y. and Garc{\'i}a, R. A. and Gilliland, R. L. and Girardi, L. and Houdek, G. and Karoff, C. and Kawaler, S. D. and Metcalfe, T. S. and {Molenda-{\.Z}akowicz}, J. and Monteiro, M. J. P. F. G. and Thompson, M. J. and Verner, G. A. and Ballot, J. and Bonanno, A. and Brand{\~a}o, I. M. and Broomhall, A.-M. and Bruntt, H. and Campante, T. L. and Corsaro, E. and Creevey, O. L. and Do{\u g}an, G. and Esch, L. and Gai, N. and Gaulme, P. and Hale, S. J. and Handberg, R. and Hekker, S. and Huber, D. and Jim{\'e}nez, A. and Mathur, S. and Mazumdar, A. and Mosser, B. and New, R. and Pinsonneault, M. H. and Pricopi, D. and Quirion, P.-O. and R{\'e}gulo, C. and Salabert, D. and Serenelli, A. M. and Silva Aguirre, V. and Sousa, S. G. and Stello, D. and Stevens, I. R. and Suran, M. D. and Uytterhoeven, K. and White, T. R. and Borucki, W. J. and Brown, T. M. and Jenkins, J. M. and Kinemuchi, K. and Van Cleve, J. and Klaus, T. C.},
  year = {2011},
  month = apr,
  volume = {332},
  pages = {213},
  doi = {10.1126/science.1201827},
  abstract = {In addition to its search for extrasolar planets, the NASA Kepler mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solar-type stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius, and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy.},
  file = {/Users/Oliver/Zotero/storage/5KXBIB99/Chaplin et al. - 2011 - Ensemble Asteroseismology of Solar-Type Stars with.pdf;/Users/Oliver/Zotero/storage/QLM5T3GK/ui.adsabs.harvard.edu.html},
  journal = {Science},
  language = {en},
  number = {6026}
}

@article{chaplin+2013,
  title = {Asteroseismic {{Determination}} of {{Obliquities}} of the {{Exoplanet Systems Kepler}}-50 and {{Kepler}}-65},
  author = {Chaplin, W. J. and {Sanchis-Ojeda}, R. and Campante, T. L. and Handberg, R. and Stello, D. and Winn, J. N. and Basu, S. and {Christensen-Dalsgaard}, J. and Davies, G. R. and Metcalfe, T. S. and Buchhave, L. A. and Fischer, D. A. and Bedding, T. R. and Cochran, W. D. and Elsworth, Y. and Gilliland, R. L. and Hekker, S. and Huber, D. and Isaacson, H. and Karoff, C. and Kawaler, S. D. and Kjeldsen, H. and Latham, D. W. and Lund, M. N. and Lundkvist, M. and Marcy, G. W. and Miglio, A. and Barclay, T. and Lissauer, J. J.},
  year = {2013},
  month = apr,
  volume = {766},
  pages = {101},
  doi = {10.1088/0004-637X/766/2/101},
  abstract = {Results on the obliquity of exoplanet host stars\textemdash the angle between the stellar spin axis and the planetary orbital axis\textemdash provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1{$\sigma$} level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated.},
  file = {/Users/Oliver/Zotero/storage/45DFIP57/Chaplin et al. - 2013 - Asteroseismic Determination of Obliquities of the .pdf;/Users/Oliver/Zotero/storage/VXNCQVR5/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  keywords = {Seismic rotation},
  language = {en},
  number = {2}
}

@article{chaplin+2014,
  title = {Super-{{Nyquist}} Asteroseismology of Solar-like Oscillators with {{Kepler}} and {{K2}} - Expanding the Asteroseismic Cohort at the Base of the Red-Giant Branch},
  author = {Chaplin, W. J. and Elsworth, Y. and Davies, G. R. and Campante, T. L. and Handberg, R. and Miglio, A. and Basu, S.},
  year = {2014},
  month = nov,
  volume = {445},
  pages = {946--954},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stu1811},
  abstract = {We consider the prospects for detecting solar-like oscillations in the "super-Nyquist" regime of long-cadence (LC) Kepler photometry, i.e., above the associated Nyquist frequency of approximately 283 \{\textbackslash mu\}Hz. Targets of interest are cool, evolved subgiants and stars lying at the base of the red-giant branch. These stars would ordinarily be studied using the short-cadence (SC) data, since the associated SC Nyquist frequency lies well above the frequencies of the detectable oscillations. However, the number of available SC target slots is quite limited. This imposes a severe restriction on the size of the ensemble available for SC asteroseismic study.We find that archival Kepler LC data from the nominal Mission may be utilized for asteroseismic studies of targets whose dominant oscillation frequencies lie as high as approximately 500 \{\textbackslash mu\}Hz, i.e., about 1.75- times the LC Nyquist frequency. The frequency detection threshold for the shorter-duration science campaigns of the re-purposed Kepler Mission, K2, is lower. The maximum threshold will probably lie somewhere between approximately 400 and 450 \{\textbackslash mu\}Hz. The potential to exploit the archival Kepler and K2 LC data in this manner opens the door to increasing significantly the number of subgiant and low-luminosity red-giant targets amenable to asteroseismic analysis, overcoming target limitations imposed by the small number of SC slots.We estimate that around 400 such targets are now available for study in the Kepler LC archive. That number could potentially be a lot higher for K2, since there will be a new target list for each of its campaigns.},
  archivePrefix = {arXiv},
  eprint = {1409.0696},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/99APSRAJ/Chaplin et al. - 2014 - Super-Nyquist asteroseismology of solar-like oscil.pdf;/Users/Oliver/Zotero/storage/XN9REZV2/1409.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{chaplin+2014a,
  title = {Asteroseismic {{Fundamental Properties}} of {{Solar}}-Type {{Stars Observed}} by the {{NASA Kepler Mission}}},
  author = {Chaplin, W. J. and Basu, S. and Huber, D. and Serenelli, A. and Casagrande, L. and Silva Aguirre, V. and Ball, W. H. and Creevey, O. L. and Gizon, L. and Handberg, R. and Karoff, C. and Lutz, R. and Marques, J. P. and Miglio, A. and Stello, D. and Suran, M. D. and Pricopi, D. and Metcalfe, T. S. and Monteiro, M. J. P. F. G. and {Molenda-{\.Z}akowicz}, J. and Appourchaux, T. and {Christensen-Dalsgaard}, J. and Elsworth, Y. and Garc{\'i}a, R. A. and Houdek, G. and Kjeldsen, H. and Bonanno, A. and Campante, T. L. and Corsaro, E. and Gaulme, P. and Hekker, S. and Mathur, S. and Mosser, B. and R{\'e}gulo, C. and Salabert, D.},
  year = {2014},
  month = jan,
  volume = {210},
  pages = {1},
  doi = {10.1088/0067-0049/210/1/1},
  abstract = {We use asteroseismic data obtained by the NASA Kepler mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures, T \textsubscript{eff}, were available for the entire ensemble from complementary photometry; spectroscopic estimates of T \textsubscript{eff} and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. We adopt a grid-based analysis, coupling six pipeline codes to 11 stellar evolutionary grids. Through use of these different grid-pipeline combinations we allow implicitly for the impact on the results of stellar model dependencies from commonly used grids, and differences in adopted pipeline methodologies. By using just two global parameters as the seismic inputs we are able to perform a homogenous analysis of all solar-type stars in the asteroseismic cohort, including many targets for which it would not be possible to provide robust estimates of individual oscillation frequencies (due to a combination of low signal-to-noise ratio and short dataset lengths). The median final quoted uncertainties from consolidation of the grid-based analyses are for the full ensemble (spectroscopic subset) approximately 10.8\% (5.4\%) in mass, 4.4\% (2.2\%) in radius, 0.017 dex (0.010 dex) in log g, and 4.3\% (2.8\%) in mean density. Around 36\% (57\%) of the stars have final age uncertainties smaller than 1 Gyr. These ages will be useful for ensemble studies, but should be treated carefully on a star-by-star basis. Future analyses using individual oscillation frequencies will offer significant improvements on up to 150 stars, in particular for estimates of the ages, where having the individual frequency data is most important.},
  file = {/Users/Oliver/Zotero/storage/SWSWJSKH/Chaplin et al. - 2014 - Asteroseismic Fundamental Properties of Solar-type.pdf;/Users/Oliver/Zotero/storage/KP9V6J2L/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{chaplin+2015,
  title = {Asteroseismology of Solar-Type Stars with {{K2}}},
  author = {Chaplin, W. J. and Lund, M. N. and Handberg, R. and Basu, S. and Buchhave, L. A. and Campante, T. L. and Davies, G. R. and Huber, D. and Latham, D. W. and Latham, C. A. and Serenelli, A. and Antia, H. M. and Appourchaux, T. and Ball, W. H. and Benomar, O. and Casagrande, L. and {Christensen-Dalsgaard}, J. and Coelho, H. R. and Creevey, O. L. and Elsworth, Y. and Garc, R. A. and Gaulme, P. and Hekker, S. and Kallinger, T. and Karoff, C. and Kawaler, S. D. and Kjeldsen, H. and Lundkvist, M. S. and Marcadon, F. and Mathur, S. and Miglio, A. and Mosser, B. and R, C. and Roxburgh, I. W. and Aguirre, V. Silva and Stello, D. and Verma, K. and White, T. R. and Bedding, T. R. and Barclay, T. and Buzasi, D. L. and Deheuvels, S. and Gizon, L. and Houdek, G. and Howell, S. B. and Salabert, D. and Soderblom, D. R.},
  year = {2015},
  month = oct,
  volume = {127},
  pages = {1038--1044},
  issn = {00046280, 15383873},
  doi = {10.1086/683103},
  abstract = {We present the first detections by the NASA K2 Mission of oscillations in solar-type stars, using short-cadence data collected during K2 Campaign 1 (C1). We understand the asteroseismic detection thresholds for C1-like levels of photometric performance, and we can detect oscillations in subgiants having dominant oscillation frequencies around 1000 \textmu Hz. Changes to the operation of the fine-guidance sensors are expected to give significant improvements in the high-frequency performance from C3 onwards. A reduction in the excess highfrequency noise by a factor of two-and-a-half in amplitude would bring mainsequence stars with dominant oscillation frequencies as high as {$\simeq$} 2500 \textmu Hz into play as potential asteroseismic targets for K2.},
  archivePrefix = {arXiv},
  eprint = {1507.01827},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/YE3NFI6W/Chaplin et al. - 2015 - Asteroseismology of solar-type stars with K2.pdf},
  journal = {Publications of the Astronomical Society of the Pacific},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  number = {956}
}

@article{chaplin+2020,
  title = {Age Dating of an Early {{Milky Way}} Merger via Asteroseismology of the Naked-Eye Star \$\textbackslash nu\$ {{Indi}}},
  author = {Chaplin, William J. and Serenelli, Aldo M. and Miglio, Andrea and Morel, Thierry and Mackereth, J. Ted and Vincenzo, Fiorenzo and Basu, Hans Kjeldsen Sarbani and Ball, Warrick H. and Stokholm, Amalie and Verma, Kuldeep and Mosumgaard, Jakob R{\o}rsted and Aguirre, Victor Silva and Mazumdar, Anwesh and Ranadive, Pritesh and Antia, H. M. and Lebreton, Yveline and Ong, Joel and Appourchaux, Thierry and Bedding, Timothy R. and {Christensen-Dalsgaard}, J{\o}rgen and Creevey, Orlagh and Garc{\'i}a, Rafael A. and Handberg, Rasmus and Huber, Daniel and Kawaler, Steven D. and Lund, Mikkel N. and Metcalfe, Travis S. and Stassun, Keivan G. and Bazot, Mich{\"a}el and Beck, Paul and Bell, Keaton J. and Bergemann, Maria and Buzasi, Derek L. and Benomar, Othman and Bossini, Diego and Bugnet, Lisa and Campante, Tiago L. and Orhan, Zeynep {\c C}elik and Corsaro, Enrico and {Gonz{\'a}lez-Cuesta}, Luc{\'i}a and Davies, Guy R. and Di Mauro, Maria Pia and Egeland, Ricky and Elsworth, Yvonne P. and Gaulme, Patrick and Ghasemi, Hamed and Guo, Zhao and Hall, Oliver J. and Hasanzadeh, Amir and Hekker, Saskia and Howe, Rachel and Jenkins, Jon M. and Jim{\'e}nez, Antonio and Kiefer, Ren{\'e} and Kuszlewicz, James S. and Kallinger, Thomas and Latham, David W. and Lundkvist, Mia S. and Mathur, Savita and Montalb{\'a}n, Josefina and Mosser, Benoit and Bed{\'o}n, Andres Moya and Nielsen, Martin Bo and {\"O}rtel, Sibel and Rendle, Ben M. and Ricker, George R. and Rodrigues, Tha{\'i}se S. and Roxburgh, Ian W. and Safari, Hossein and Schofield, Mathew and Seager, Sara and Smalley, Barry and Stello, Dennis and Szab{\'o}, R{\'o}bert and Tayar, Jamie and Theme{\ss}l, Nathalie and Thomas, Alexandra E. L. and Vanderspek, Roland K. and {van Rossem}, Walter E. and Vrard, Mathieu and Weiss, Achim and White, Timothy R. and Winn, Joshua N. and Y{\i}ld{\i}z, Mutlu},
  year = {2020},
  month = jan,
  issn = {2397-3366},
  doi = {10.1038/s41550-019-0975-9},
  abstract = {Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies. While these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to precisely date the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called \textbackslash textit\{Gaia\}-Enceladus, leading to a substantial pollution of the chemical and dynamical properties of the Milky Way. Here, we identify the very bright, naked-eye star \$\textbackslash nu\$\textbackslash,Indi as a probe of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric, and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be \$11.0 \textbackslash pm 0.7\$ (stat) \$\textbackslash pm 0.8\$ (sys)\$\textbackslash,\textbackslash rm Gyr\$. The star bears hallmarks consistent with it having been kinematically heated by the \textbackslash textit\{Gaia\}-Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 Gyr ago at 68 and 95\% confidence, respectively. Input from computations based on hierarchical cosmological models tightens (i.e. reduces) slightly the above limits.},
  archivePrefix = {arXiv},
  eprint = {2001.04653},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/4NXPKVDF/Chaplin et al. - 2020 - Age dating of an early Milky Way merger via astero.pdf},
  journal = {Nature Astronomy},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  language = {en}
}

@article{chaplin+basu2008,
  title = {Perspectives in {{Global Helioseismology}}, and the {{Road Ahead}}},
  author = {Chaplin, William J. and Basu, Sarbani},
  year = {2008},
  month = sep,
  volume = {251},
  pages = {53--75},
  issn = {0038-0938, 1573-093X},
  doi = {10.1007/s11207-008-9136-5},
  abstract = {We review the impact of global helioseismology on key questions concerning the internal structure and dynamics of the Sun, and consider the exciting challenges the field faces as it enters a fourth decade of science exploitation. We do so with an eye on the past, looking at the perspectives global helioseismology offered in its earlier phases, in particular the mid-to-late 1970s and the 1980s. We look at how modern, higher-quality, longer datasets coupled with new developments in analysis, have altered, refined, and changed some of those perspectives, and opened others that were not previously available for study. We finish by discussing outstanding challenges and questions for the field.},
  archivePrefix = {arXiv},
  eprint = {0801.4213},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/NV2VHXST/Chaplin and Basu - 2008 - Perspectives in Global Helioseismology, and the Ro.pdf;/Users/Oliver/Zotero/storage/28SMZRXH/0801.html},
  journal = {Solar Physics},
  keywords = {Astrophysics},
  number = {1-2}
}

@article{chaplin+basu2014,
  title = {Inferences on {{Stellar Activity}} and {{Stellar Cycles}} from {{Asteroseismology}}},
  author = {Chaplin, William J. and Basu, Sarbani},
  year = {2014},
  month = dec,
  volume = {186},
  pages = {437--456},
  issn = {0038-6308, 1572-9672},
  doi = {10.1007/s11214-014-0090-2},
  abstract = {The solar activity cycle can be studied using many different types of observations, such as counting sunspots, measuring emission in the Ca II H\&K lines, magnetograms, radio emissions, etc. One of the more recent ways of studying solar activity is to use the changing properties of solar oscillations. Stellar activity cycles are generally studied using the Ca II lines, or sometimes using photometry. Asteroseismology is potentially an exciting means of studying these cycles. In this article we examine whether or not asteroseismic data can be used for this purpose, and what the asteroseismic signatures of stellar activity are. We also examine how asteroseismology may help in more indirect ways.},
  file = {/Users/Oliver/Zotero/storage/QAEJNID6/Chaplin and Basu - 2014 - Inferences on Stellar Activity and Stellar Cycles .pdf;/Users/Oliver/Zotero/storage/E6K8GHER/10.html},
  journal = {Space Science Reviews},
  language = {en},
  number = {1-4}
}

@book{chaplin+basu2017,
  title = {Asteroseismic {{Data Analysis}}: {{Foundations}} and {{Techniques}}},
  author = {Chaplin, W. J. and Basu},
  year = {2017},
  edition = {1st},
  publisher = {{Princeton University Press}},
  address = {{Princeton, New Jersey}},
  isbn = {978-0-691-16292-8}
}

@article{chaplin+miglio2013,
  title = {Asteroseismology of {{Solar}}-{{Type}} and {{Red}}-{{Giant Stars}}},
  author = {Chaplin, William J. and Miglio, Andrea},
  year = {2013},
  month = aug,
  volume = {51},
  pages = {353},
  doi = {10.1146/annurev-astro-082812-140938},
  abstract = {We are entering a golden era for stellar physics driven by satellite and telescope observations of unprecedented quality and scope. New insights on stellar evolution and stellar interiors physics are being made possible by asteroseismology, the study of stars by the observation of natural, resonant oscillations. Asteroseismology is proving to be particularly significant for the study of solar-type and red-giant stars. These stars show rich spectra of solar-like oscillations, which are excited and intrinsically damped by turbulence in the outermost layers of the convective envelopes. In this review we discuss the current state of the field, with a particular emphasis on recent advances provided by the Kepler and COROT (Convection, Rotation \& Planetary Transits) space missions and the wider significance to astronomy of the results from asteroseismology, such as stellar populations studies and exoplanet studies.},
  file = {/Users/Oliver/Zotero/storage/QP66FFAV/Chaplin and Miglio - 2013 - Asteroseismology of Solar-Type and Red-Giant Stars.pdf;/Users/Oliver/Zotero/storage/4RUV4AMH/abstract.html},
  journal = {Annual Review of Astronomy and Astrophysics},
  language = {en},
  number = {1}
}

@article{chen+2017,
  title = {Absolute {{Magnitudes}} of {{Seismic Red Clumps}} in the {{Kepler Field}} and {{SAGA}}: {{The Age Dependency}} of the {{Distance Scale}}},
  shorttitle = {Absolute {{Magnitudes}} of {{Seismic Red Clumps}} in the {{Kepler Field}} and {{SAGA}}},
  author = {Chen, Y. Q. and Casagrande, L. and Zhao, G. and Bovy, J. and Silva Aguirre, V. and Zhao, J. K. and Jia, Y. P.},
  year = {2017},
  month = may,
  volume = {840},
  pages = {77},
  doi = {10.3847/1538-4357/aa6d0f},
  abstract = {Red clump stars are fundamental distance indicators in astrophysics, although theoretical stellar models predict a dependence of absolute magnitudes with age. This effect is particularly strong below{\~ }2 Gyr, but even above this limit a mild age dependence is still expected. We use seismically identified red clump stars in the Kepler field for which we have reliable distances, masses, and ages from the SAGA survey, to first explore this effect. By excluding red clump stars with masses larger than 1.6 \{M\}\textsubscript{{$\Sun$} } (corresponding to ages younger than 2 Gyr), we derive robust calibrations linking intrinsic colors to absolute magnitudes in the following photometric systems: Str\"omgren by, Johnson BV, Sloan griz, 2MASS JHK \textsubscript{ s }, and WISE W1W2W3. With the precision achieved we also detect a slope of absolute magnitudes{\~ } 0.020+/- 0.003 \{mag\} \{\{Gyr\}\}\textsuperscript{-1} in the infrared, implying that distance calibrations of clump stars can be off by up to{\~ } 0.2 \{mag\} in the infrared (over the range from 2 to 12 Gyr) if their ages are unknown. Even larger uncertainties affect optical bands, because of the stronger interdependency of absolute magnitudes on colors and age. Our distance calibrations are ultimately based on asteroseismology, and we show how the distance scale can be used to test the accuracy of seismic scaling relations. Within the uncertainties our calibrations are in agreement with those built upon local red clumps with Hipparcos parallaxes, although we find a tension, which, if confirmed, would imply that scaling relations overestimate the radii of red clump stars by 2 {$\pm$} 2\%. Data releases post Gaia DR1 will provide an important testbed for our results.},
  file = {/Users/Oliver/Zotero/storage/WR6JQFKB/Chen et al. - 2017 - Absolute Magnitudes of Seismic Red Clumps in the K.pdf;/Users/Oliver/Zotero/storage/7BPBXRZ5/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{chiavassa+2017,
  title = {Asymmetries on Red Giant Branch Surfaces from {{CHARA}}/{{MIRC}} Optical Interferometry},
  author = {Chiavassa, A. and Norris, R. and Montarg{\`e}s, M. and Ligi, R. and Fossati, L. and Bigot, L. and Baron, F. and Kervella, P. and Monnier, J. D. and Mourard, D. and Nardetto, N. and Perrin, G. and Schaefer, G. H. and ten Brummelaar, T. A. and Magic, Z. and Collet, R. and Asplund, M.},
  year = {2017},
  month = mar,
  abstract = {Context. Red giant branch (RGB) stars are very bright objects in galaxies and are often used as standard candles. Interferometry is the ideal tool to characterize the dynamics and morphology of their atmospheres. Aims. We aim at precisely characterising the surface dynamics of a sample of RGB stars. Methods. We obtained interferometric observations for three RGB stars with the MIRC instrument mounted at the CHARA interfer- ometer. We looked for asymmetries on the stellar surfaces using limb-darkening models. Results. We measured the apparent diameters of HD197989 (Epsilon Cyg) = 4.61+-0.02 mas, HD189276 (HR7633) = 2.95+-0.01 mas, and HD161096 (Beta Oph) = 4.43+-0.01 mas. We detected departures from the centrosymmetric case for all three stars with the tendency of a greater effect for lower logg of the sample. We explored the causes of this signal and conclude that a possible explanation to the interferometric signal is the convection-related and/or the magnetic-related surface activity. However, it is necessary to monitor these stars with new observations, possibly coupled with spectroscopy, in order to firmly establish the cause.},
  archivePrefix = {arXiv},
  eprint = {1703.02406},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/XVG7PS98/Chiavassa et al. - 2017 - Asymmetries on red giant branch surfaces from CHAR.pdf;/Users/Oliver/Zotero/storage/MS5NEDZZ/1703.html},
  journal = {arXiv:1703.02406 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{choi+2018,
  title = {On the {{Red Giant Branch}}: {{Ambiguity}} in the {{Surface Boundary Condition Leads}} to \textasciitilde 100 {{K Uncertainty}} in {{Model Effective Temperatures}}},
  shorttitle = {On the {{Red Giant Branch}}},
  author = {Choi, Jieun and Dotter, Aaron and Conroy, Charlie and Ting, Yuan-Sen},
  year = {2018},
  month = may,
  abstract = {The effective temperature (Teff) distribution of stellar evolution models along the red giant branch (RGB) is sensitive to a number of parameters including the overall metallicity, elemental abundance patterns, the efficiency of convection, and the treatment of the surface boundary condition. Recently there has been interest in using observational estimates of the RGB Teff to place constraints on the mixing length parameter, a\_MLT, and possible variation with metallicity. Here we use 1D MESA stellar evolution models to explore the sensitivity of the RGB Teff to the treatment of the surface boundary condition. We find that different surface boundary conditions can lead to +/- 100 K metallicity-dependent offsets on the RGB relative to one another in spite of the fact that all models can reproduce the properties of the Sun. Moreover, for a given atmosphere T-tau relation, we find that the RGB Teff is also sensitive to the optical depth at which the surface boundary condition is applied in the stellar model. Nearly all models adopt the photosphere as the location of the surface boundary condition but this choice is somewhat arbitrary. We compare our models to stellar parameters derived from the APOGEE-Kepler sample of first ascent red giants and find that systematic uncertainties in the models due to treatment of the surface boundary condition place a limit of \textasciitilde 100 K below which it is not possible to make firm conclusions regarding the fidelity of the current generation of stellar models.},
  archivePrefix = {arXiv},
  eprint = {1805.04112},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/SFHF7PY8/Choi et al. - 2018 - On the Red Giant Branch Ambiguity in the Surface .pdf;/Users/Oliver/Zotero/storage/4SLNQUGQ/1805.html},
  journal = {arXiv:1805.04112 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{christensen-dalsgaard+1985,
  title = {Speed of Sound in the Solar Interior},
  author = {{Christensen-Dalsgaard}, J. and Duvall, Jr., T. L. and Gough, D. O. and Harvey, J. W. and Rhodes, Jr., E. J.},
  year = {1985},
  month = may,
  volume = {315},
  pages = {378--382},
  issn = {0028-0836},
  doi = {10.1038/315378a0},
  abstract = {The sound speed of the solar interior is directly determinable on the basis of the frequencies of solar 5-min oscillations, irrespective of solar model, and relying only on a simple asymptotic description of the oscillations in terms of trapped acoustic waves. It is plausible that, by using this asymptotic determination as an initial trial in a more accurate inversion, and imposing constraints of smoothness on the solution resulting from the iteration, a good model representing the large scale structure of the sun which satisfies the observed
frequencies may be determined.},
  journal = {Nature},
  keywords = {Acoustic Velocity,Asymptotic Methods,Differential Equations,Doppler Effect,Helioseismology,Photosphere,Solar Interior,Solar Oscillations,Wave Propagation}
}

@article{christensen-dalsgaard+1988,
  title = {Solar Oscillation Frequencies and the Equation of State},
  author = {{Christensen-Dalsgaard}, J. and Dappen, W. and Lebreton, Y.},
  year = {1988},
  month = dec,
  volume = {336},
  pages = {634},
  issn = {0028-0836},
  doi = {10.1038/336634a0},
  abstract = {Observed oscillation frequencies of the Sun can be used to investigate the properties of matter under conditions that cannot be achieved on Earth. In particular the frequencies are sensitive to the equation of state. A recently developed treatment of the partition functions leads to a substantial improvement in the agreement between the observed and the computed frequencies.},
  file = {/Users/Oliver/Zotero/storage/3U2L47WH/ui.adsabs.harvard.edu.html},
  journal = {Nature},
  language = {en},
  number = {6200}
}

@article{christensen-dalsgaard+1991,
  title = {The Depth of the Solar Convection Zone},
  author = {{Christensen-Dalsgaard}, J. and Gough, D. O. and Thompson, M. J.},
  year = {1991},
  month = sep,
  volume = {378},
  pages = {413--437},
  issn = {0004-637X},
  doi = {10.1086/170441},
  abstract = {The transition of the temperature gradient between being subadiabatic and adiabatic at the base of the solar convection zone gives rise to a clear signature in the sound speed. Helioseismic measurements of the sound speed therefore permit a determination of the location of the base of the convection zone. Two techniques were tested by applying them to artifical data, obtained by adding simulated noise to frequencies computed from two different solar models. The determinations appear to be relatively insensitive to uncertainties of the physics of the solar interior. From an analysis of observed frequencies of solar oscillation it is concluded that the depth of the solar convection zone is (0.287 + or - 0.003) solar radii.},
  file = {/Users/Oliver/Zotero/storage/R2FSYXS4/Christensen-Dalsgaard et al. - 1991 - The depth of the solar convection zone.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Acoustic Velocity,Convective Flow,Helioseismology,Reynolds Number,Solar Interior,Solar Oscillations,Sound Propagation,Stellar Composition,Temperature Gradients}
}

@article{christensen-dalsgaard+1996,
  title = {The {{Current State}} of {{Solar Modeling}}},
  author = {{Christensen-Dalsgaard}, J. and Dappen, W. and Ajukov, S. V. and Anderson, E. R. and Antia, H. M. and Basu, S. and Baturin, V. A. and Berthomieu, G. and Chaboyer, B. and Chitre, S. M. and Cox, A. N. and Demarque, P. and Donatowicz, J. and Dziembowski, W. A. and Gabriel, M. and Gough, D. O. and Guenther, D. B. and Guzik, J. A. and Harvey, J. W. and Hill, F. and Houdek, G. and Iglesias, C. A. and Kosovichev, A. G. and Leibacher, J. W. and Morel, P. and Proffitt, C. R. and Provost, J. and Reiter, J. and Rhodes, Jr., E. J. and Rogers, F. J. and Roxburgh, I. W. and Thompson, M. J. and Ulrich, R. K.},
  year = {1996},
  month = may,
  volume = {272},
  pages = {1286--1292},
  issn = {0036-8075},
  doi = {10.1126/science.272.5266.1286},
  abstract = {Data from the Global Oscillation Network Group (GONG) project and other helioseismic experiments provide a test for models of stellar interiors and for the thermodynamic and radiative properties, on which the models depend, of matter under the extreme conditions found in the sun. Current models are in agreement with the helioseismic inferences, which
suggests, for example, that the disagreement between the predicted and observed fluxes of neutrinos from the sun is not caused by errors in the models. However, the GONG data reveal subtle errors in the models, such as an excess in sound speed just beneath the convection zone. These discrepancies indicate effects that have so far not been correctly accounted for; for example, it is plausible that the sound-speed differences reflect weak mixing in stellar interiors, of potential importance to the overall evolution of stars and ultimately to estimates of the age of the galaxy based on stellar evolution calculations.},
  journal = {Science}
}

@article{christensen-dalsgaard+2010,
  title = {Asteroseismic {{Investigation}} of {{Known Planet Hosts}} in the {{Kepler Field}}},
  author = {{Christensen-Dalsgaard}, J. and Kjeldsen, H. and Brown, T. M. and Gilliland, R. L. and Arentoft, T. and Frandsen, S. and Quirion, P.-O. and Borucki, W. J. and Koch, D. and Jenkins, J. M.},
  year = {2010},
  month = apr,
  volume = {713},
  pages = {L164},
  doi = {10.1088/2041-8205/713/2/L164},
  abstract = {In addition to its great potential for characterizing extra-solar planetary systems, the Kepler Mission is providing unique data on stellar oscillations. A key aspect of Kepler asteroseismology is the application to solar-like oscillations of main-sequence stars. As an example, we here consider an initial analysis of data for three stars in the Kepler field for which planetary transits were known from ground-based observations. For one of these, HAT-P-7, we obtain a detailed frequency spectrum and hence strong constraints on the stellar properties. The remaining two stars show definite evidence for solar-like oscillations, yielding a preliminary estimate of their mean densities.},
  file = {/Users/Oliver/Zotero/storage/VJEV73N8/Christensen-Dalsgaard et al. - 2010 - Asteroseismic Investigation of Known Planet Hosts .pdf;/Users/Oliver/Zotero/storage/JIVFZPWI/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{christensen-dalsgaard2002,
  title = {Helioseismology},
  author = {{Christensen-Dalsgaard}, J{\o}rgen},
  year = {2002},
  month = nov,
  volume = {74},
  pages = {1073--1129},
  issn = {0034-6861},
  doi = {10.1103/RevModPhys.74.1073},
  abstract = {Oscillations detected on the solar surface provide a unique opportunity for investigations of the interior properties of a star. Through major observational efforts, including extensive observations from space, as well as through the development of sophisticated tools for the analysis and interpretation of the data, we have been able to infer the
large-scale structure and rotation of the solar interior with
substantial accuracy. In addition, information is emerging about the complex subsurface structure and dynamics of sunspot regions, which dominate the magnetic activity in the solar atmosphere and beyond. The results provide a detailed test of the modeling of stellar structure and evolution, and hence of the physical properties of matter assumed in the models. In this way the basis for using stellar modeling in other branches of science is substantially strengthened; an important example is the use of observations of solar neutrinos to constrain the
properties of the neutrino.},
  file = {/Users/Oliver/Zotero/storage/ZFTPCY2Z/Christensen-Dalsgaard - 2002 - Helioseismology.pdf},
  journal = {Reviews of Modern Physics},
  keywords = {Electric and magnetic fields solar magnetism,Helioseismology pulsations and shock waves,Particle emission solar wind,Solar interior,Solar neutrinos}
}

@article{christensen-dalsgaard2008,
  title = {{{ASTEC}}\textemdash the {{Aarhus STellar Evolution Code}}},
  author = {{Christensen-Dalsgaard}, J{\o}rgen},
  year = {2008},
  month = aug,
  volume = {316},
  pages = {13},
  issn = {0004-640X},
  doi = {10.1007/s10509-007-9675-5},
  abstract = {The Aarhus code is the result of a long development, starting in 1974, and still ongoing. A novel feature is the integration of the computation of adiabatic oscillations for specified models as part of the code. It offers substantial flexibility in terms of microphysics and has been carefully tested for the computation of solar models. However, considerable development is still required in the treatment of nuclear reactions, diffusion and convective mixing.},
  file = {/Users/Oliver/Zotero/storage/BKHCZNGS/Christensen-Dalsgaard - 2008 - ASTEC—the Aarhus STellar Evolution Code.pdf;/Users/Oliver/Zotero/storage/S53V4VAX/abstract.html},
  journal = {Astrophysics and Space Science},
  language = {en},
  number = {1-4}
}

@article{claytor+2019,
  title = {Chemical {{Evolution}} in the {{Milky Way}}: {{Rotation}}-Based Ages for {{APOGEE}}-{{Kepler}} Cool Dwarf Stars},
  shorttitle = {Chemical {{Evolution}} in the {{Milky Way}}},
  author = {Claytor, Zachary R. and {van Saders}, Jennifer L. and Santos, Angela R. G. and Garcia, Rafael A. and Mathur, Savita and Tayar, Jamie and Pinsonneault, Marc H. and Shetrone, Matthew},
  year = {2019},
  month = nov,
  pages = {arXiv:1911.04518},
  abstract = {We use models of stellar angular momentum evolution to determine ages for \$\textbackslash sim500\$ stars in the APOGEE-\textbackslash textit\{Kepler\} Cool Dwarfs sample. We focus on lower main-sequence stars, where other age-dating tools become ineffective. Our age distributions are compared to those derived from asteroseismic and giant samples and solar analogs. We are able to recover gyrochronological ages for old, lower-main-sequence stars, a remarkable improvement over prior work in hotter stars. Under our model assumptions, our ages have a median relative uncertainty of \$14\textbackslash\%\$, comparable to the age precision inferred for more massive stars using traditional methods. We investigate trends of galactic \$\textbackslash alpha\$-enhancement with age, finding evidence of a detection threshold between the age of the oldest \$\textbackslash alpha\$-poor stars and that of the bulk \$\textbackslash alpha\$-rich population. We argue that gyrochronology is an effective tool reaching ages of 10--12 Gyr in K- and early M-dwarfs. Finally, we present the first effort to quantify the impact of detailed abundance patterns on rotational evolution. We estimate a \$\textbackslash sim15\textbackslash\%\$ bias in age for cool, \$\textbackslash alpha\$-enhanced (+ 0.4 dex) stars when standard solar-abundance-pattern rotational models are used for age inference, rather than models that appropriately account for \$\textbackslash alpha\$-enrichment.},
  file = {/Users/Oliver/Zotero/storage/WV7JP6EE/Claytor et al. - 2019 - Chemical Evolution in the Milky Way Rotation-base.pdf;/Users/Oliver/Zotero/storage/YU7NMBSV/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{coleman+2019,
  title = {Maximum {{Entropy Estimation}} of the {{Galactic Bulge Morphology}} via the {{VVV Red Clump}}},
  author = {Coleman, Brendan and Paterson, Dylan and Gordon, Chris and Macias, Oscar and Ploeg, Harrison},
  year = {2019},
  month = nov,
  abstract = {The abundance and narrow magnitude dispersion of Red Clump (RC) stars make them a popular candidate for mapping the morphology of the bulge region of the Milky Way. Using a semi-analytic derivation of the RC's intrinsic luminosity function, we extracted the three-dimensional density distribution of the RC from deep photometric catalogues of the VISTA Variables in the Via Lactea (VVV) survey. We employed a joint approach of parametric modelling and maximum entropy based non-parametric deconvolution to extract the spatial distribution of the bulge from Ks-band star counts. Assuming two-fold symmetry over the Galactic plane, we obtained our non-parametric model of the bulge over the inner 40 by 4

repository: sandorkruk/malatium

repo_name: sandorkruk/malatium