text:
0 degrees squared region centred on the Galactic centre with curvature minimising inpainting overcrowded and high extinction regions. Our reconstruction also naturally matches onto a parametric fit to the bulge outside the VVV region. We incorporated into our background model an apparent feature behind the bar previously observed in the VVV survey. We found a range of bulge properties consistent with other recent investigations based on the VVV data. However, our base model does have less dense X-arms than previous analysis and also retains an asymmetry between the near and far arms of the X-bulge. Studies of the Fermi Large Area Telescope (LAT) gamma-ray Galactic centre excess suggest that the excess may be traced by Galactic Bulge distributed sources. Building on the view that the RC sufficiently traces the Galactic bulge morphology, we applied our deconvolved density in a template fitting analysis of this Fermi-LAT GeV excess and found an improvement in the fit compared to previous parametric based templates.},
  archivePrefix = {arXiv},
  eprint = {1911.04714},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8QEPMXLE/Coleman et al. - 2019 - Maximum Entropy Estimation of the Galactic Bulge M.pdf;/Users/Oliver/Zotero/storage/4HJKTZNQ/1911.html},
  journal = {arXiv:1911.04714 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - High Energy Astrophysical Phenomena,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{collaboration+2018,
  title = {The {{Astropy Project}}: {{Building}} an {{Open}}-Science {{Project}} and {{Status}} of the v2.0 {{Core Package}}},
  shorttitle = {The {{Astropy Project}}},
  author = {Collaboration, Astropy and {Price-Whelan}, A. M. and Sip{\H o}cz, B. M. and G{\"u}nther, H. M. and Lim, P. L. and Crawford, S. M. and Conseil, S. and Shupe, D. L. and Craig, M. W. and Dencheva, N. and Ginsburg, A. and VanderPlas, J. T. and Bradley, L. D. and {P{\'e}rez-Su{\'a}rez}, D. and {de Val-Borro}, M. and Aldcroft, T. L. and Cruz, K. L. and Robitaille, T. P. and Tollerud, E. J. and Ardelean, C. and Babej, T. and Bach, Y. P. and Bachetti, M. and Bakanov, A. V. and Bamford, S. P. and Barentsen, G. and Barmby, P. and Baumbach, A. and Berry, K. L. and Biscani, F. and Boquien, M. and Bostroem, K. A. and Bouma, L. G. and Brammer, G. B. and Bray, E. M. and Breytenbach, H. and Buddelmeijer, H. and Burke, D. J. and Calderone, G. and Cano Rodr{\'i}guez, J. L. and Cara, M. and Cardoso, J. V. M. and Cheedella, S. and Copin, Y. and Corrales, L. and Crichton, D. and D'Avella, D. and Deil, C. and Depagne, {\'E} and Dietrich, J. P. and Donath, A. and Droettboom, M. and Earl, N. and Erben, T. and Fabbro, S. and Ferreira, L. A. and Finethy, T. and Fox, R. T. and Garrison, L. H. and Gibbons, S. L. J. and Goldstein, D. A. and Gommers, R. and Greco, J. P. and Greenfield, P. and Groener, A. M. and Grollier, F. and Hagen, A. and Hirst, P. and Homeier, D. and Horton, A. J. and Hosseinzadeh, G. and Hu, L. and Hunkeler, J. S. and Ivezi{\'c}, {\v Z} and Jain, A. and Jenness, T. and Kanarek, G. and Kendrew, S. and Kern, N. S. and Kerzendorf, W. E. and Khvalko, A. and King, J. and Kirkby, D. and Kulkarni, A. M. and Kumar, A. and Lee, A. and Lenz, D. and Littlefair, S. P. and Ma, Z. and Macleod, D. M. and Mastropietro, M. and McCully, C. and Montagnac, S. and Morris, B. M. and Mueller, M. and Mumford, S. J. and Muna, D. and Murphy, N. A. and Nelson, S. and Nguyen, G. H. and Ninan, J. P. and N{\"o}the, M. and Ogaz, S. and Oh, S. and Parejko, J. K. and Parley, N. and Pascual, S. and Patil, R. and Patil, A. A. and Plunkett, A. L. and Prochaska, J. X. and Rastogi, T. and Reddy Janga, V. and Sabater, J. and Sakurikar, P. and Seifert, M. and Sherbert, L. E. and {Sherwood-Taylor}, H. and Shih, A. Y. and Sick, J. and Silbiger, M. T. and Singanamalla, S. and Singer, L. P. and Sladen, P. H. and Sooley, K. A. and Sornarajah, S. and Streicher, O. and Teuben, P. and Thomas, S. W. and Tremblay, G. R. and Turner, J. E. H. and Terr{\'o}n, V. and {van Kerkwijk}, M. H. and {de la Vega}, A. and Watkins, L. L. and Weaver, B. A. and Whitmore, J. B. and Woillez, J. and Zabalza, V. and Contributors, Astropy},
  year = {2018},
  month = sep,
  volume = {156},
  pages = {123},
  doi = {10.3847/1538-3881/aabc4f},
  abstract = {The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project. .},
  file = {/Users/Oliver/Zotero/storage/7CRTTY3I/Collaboration et al. - 2018 - The Astropy Project Building an Open-science Proj.pdf;/Users/Oliver/Zotero/storage/E6HZVM6M/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {3}
}

@article{collins+2017,
  title = {{{AstroImageJ}}: {{Image Processing}} and {{Photometric Extraction}} for {{Ultra}}-{{Precise Astronomical Light Curves}} ({{Expanded Edition}})},
  shorttitle = {{{AstroImageJ}}},
  author = {Collins, Karen A. and Kielkopf, John F. and Stassun, Keivan G. and Hessman, Frederic V.},
  year = {2017},
  file = {/Users/Oliver/Zotero/storage/8NF695GD/1701.04817.pdf},
  journal = {arXiv preprint arXiv:1701.04817}
}

@article{colman+2017,
  title = {Evidence for Compact Binary Systems around \${{Kepler}}\$ Red Giants},
  author = {Colman, Isabel L. and Huber, Daniel and Bedding, Timothy R. and Kuszlewicz, James S. and Yu, Jie and Beck, Paul G. and Elsworth, Yvonne and Garc{\'i}a, Rafael A. and Kawaler, Steven D. and Mathur, Savita and Stello, Dennis and White, Timothy R.},
  year = {2017},
  month = may,
  abstract = {We present an analysis of 168 oscillating red giants from NASA's \$Kepler\$ mission that exhibit anomalous peaks in their Fourier amplitude spectra. These peaks result from ellipsoidal variations which are indicative of binary star systems, at frequencies such that the orbit of any stellar companion would be within the convective envelope of the red giant. Alternatively, the observed phenomenon may be due to a close binary orbiting a red giant in a triple system, or chance alignments of foreground or background binary systems contaminating the target pixel aperture. We identify 87 stars in the sample as chance alignments using a combination of pixel Fourier analysis and difference imaging. We find that in the remaining 81 cases the anomalous peaks are indistinguishable from the target star to within 4\$''\$, suggesting a physical association. We examine a Galaxia model of the \$Kepler\$ field of view to estimate background star counts and find that it is highly unlikely that all targets can be explained by chance alignments. From this, we conclude that these stars may comprise a population of physically associated systems.},
  archivePrefix = {arXiv},
  eprint = {1705.00621},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/93UJZ6EZ/Colman et al. - 2017 - Evidence for compact binary systems around $Kepler.pdf;/Users/Oliver/Zotero/storage/WMDK362U/1705.html},
  journal = {arXiv:1705.00621 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{corsaro+2017,
  title = {Spin Alignment of Stars in Old Open Clusters},
  author = {Corsaro, Enrico and Lee, Yueh-Ning and Garc{\'i}a, Rafael A. and Hennebelle, Patrick and Mathur, Savita and Beck, Paul G. and Mathis, Stephane and Stello, Dennis and Bouvier, J{\'e}r{\^o}me},
  year = {2017},
  month = mar,
  volume = {1},
  pages = {0064},
  issn = {2397-3366},
  doi = {10.1038/s41550-017-0064},
  abstract = {Using asteroseismology to measure the spin axes of stars in two old open star clusters, Corsaro et al. find alignment between significant numbers of stars. It is thought that this is an imprint of the original angular momentum of the parent molecular cloud.},
  copyright = {\textcopyright{} 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved.},
  file = {/Users/Oliver/Zotero/storage/GU23KI3U/s41550-017-0064.pdf;/Users/Oliver/Zotero/storage/X4KWT9HK/s41550-017-0064.html},
  journal = {Nature Astronomy},
  language = {en}
}

@article{corsaro+deridder2015,
  title = {{{DIAMONDS}}: A New {{Bayesian}} Nested Sampling Tool},
  shorttitle = {{{DIAMONDS}}},
  author = {Corsaro, Enrico and De Ridder, Joris},
  year = {2015},
  month = sep,
  volume = {101},
  pages = {06019},
  address = {{eprint: arXiv:1509.08311}},
  doi = {10.1051/epjconf/201510106019},
  abstract = {In the context of high-quality asteroseismic data provided by the NASA Kepler Mission, we developed a new code, termed DIAMONDS
(high-DImensional And multi-MOdal NesteD Sampling), for fast Bayesian parameter estimation and model comparison by means of the Nested Sampling Monte Carlo (NSMC) algorithm, an efficient and powerful method very suitable for high-dimensional problems (like the peak bagging analysis of solar-like oscillations) and multi-modal problems (i.e. problems that show multiple solutions). We applied the code to the peak bagging analysis of solar-like oscillations observed in a
challenging F-type star. By means of DIAMONDS one is able to detect the different backgrounds in the power spectrum of the star (e.g. stellar granulation and faculae activity) and to understand whether one or two oscillation peaks can be identified or not. In addition, we demonstrate a novel approach to peak bagging based on multi-modality, which is able to reduce significantly the number of free parameters involved in the peak bagging model. This novel approach is therefore of great interest for possible future automatization of the entire analysis technique.

Software package available at the DIAMONDS code website: http://https://fys.kuleuven.be/ster/Software/Diamonds/.},
  file = {/Users/Oliver/Zotero/storage/ELEL4BMC/Corsaro and De Ridder - 2015 - DIAMONDS a new Bayesian nested sampling tool.pdf}
}

@article{corsico2017,
  title = {Pulsating White Dwarf Stars and Asteroseismology},
  author = {C{\'o}rsico, Alejandro H.},
  year = {2017},
  month = mar,
  abstract = {At present, a large number of pulsating white dwarf (WD) stars is being discovered either from Earth-based surveys such as the Sloan Digital Sky Survey, or through observations from space (e.g., the Kepler mission). The asteroseismological techniques allow us to infer details of internal chemical stratification, the total mass, and even the stellar rotation profile. In this paper, we first describe the basic properties of WD stars and their pulsations, as well as the different sub-types of these variables known so far. Subsequently, we describe some recent findings about pulsating low-mass WDs.},
  archivePrefix = {arXiv},
  eprint = {1703.00934},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8VN8TJ78/Córsico - 2017 - Pulsating white dwarf stars and asteroseismology.pdf;/Users/Oliver/Zotero/storage/2UT975MJ/1703.html},
  journal = {arXiv:1703.00934 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{couvidat+2003,
  title = {Solar {{Seismic Models}} and the {{Neutrino Predictions}}},
  author = {Couvidat, S. and {Turck-Chi{\`e}ze}, S. and Kosovichev, A. G.},
  year = {2003},
  month = dec,
  volume = {599},
  pages = {1434--1448},
  issn = {0004-637X},
  doi = {10.1086/379604},
  abstract = {This paper focuses on the solar neutrino fluxes, the g-mode predictions, and the possible impact of the magnetic fields on the neutrino emission and transport. The Solar and Heliospheric Observatory (SOHO) spacecraft has allowed astrophysicists to achieve a major breakthrough in the knowledge of the solar core. Both GOLF and MDI instruments on SOHO have significantly improved the accuracy of the sound speed profile, mainly by the detection of low-degree low-order p-modes. Our study
(Turck-Chi\`eze and coworkers) has lead to precise neutrino
predictions through constructing a seismic solar model that is in good agreement with the sound speed profile inferred by helioseismology in the radiative interior of the Sun. In this paper we present the details of this study and investigate new solar models validated by the acoustic modes. These new models are primarily used to derive the emitted neutrino fluxes. We show that these fluxes do not depend strongly on the modified physics as far as the model is consistent with the helioseismic observations in the core. We also show that an internal large-scale magnetic field cannot exceed a maximum strength of
\textasciitilde =3\texttimes 107 G in the radiative zone and may increase the
emitted 8B neutrino flux only by \textasciitilde =2\%. All the neutrino predictions here are compatible with the Sudbury Neutrino Observatory results, assuming three neutrino flavors. We deduce the electron and neutron radial densities that are needed to calculate the neutrino oscillation properties. Finally, we discuss how the magnetic fields may influence the neutrino transport through the RSFP process, for different values of {$\Delta$}m2.},
  file = {/Users/Oliver/Zotero/storage/NKD5BL7S/Couvidat et al. - 2003 - Solar Seismic Models and the Neutrino Predictions.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Instrumentation: Miscellaneous,Magnetic Fields,Neutrinos- Sun: Helioseismology,Sun: Interior,Sun: Oscillations}
}

@article{couvidat+2003a,
  title = {The {{Search}} for the {{Solar Core Dynamics}} with {{SoHO}}/{{GOLF}}},
  author = {Couvidat, S. and {Turck-Chieze}, S. and Gracia, R. A. and Corbard, T.},
  year = {2003},
  volume = {293},
  pages = {276},
  abstract = {We present the rotation profile we derive from the GOLF (plus LOWL) data. This profile shows the onset of a decrease in the rotation rate of the solar core. If confirmed, it will be useful to constrain some dynamic effects in the radiative interior and demonstrate the efficiency of angular momentum transport by gravity waves. We also present the search for gravity modes on the GOLF data. Detection of such oscillation modes will be a great breakthrough for the knowledge of the structure of the core, and the dynamic processes that occur in the deep layers. The search for both the rotation profile and gravity modes is strongly related to the dynamics of the core.},
  file = {/Users/Oliver/Zotero/storage/Z7ERD4KJ/Couvidat et al. - 2003 - The Search for the Solar Core Dynamics with SoHOG.pdf}
}

@article{cox1980,
  title = {Theory of Stellar Pulsation},
  author = {Cox, John P.},
  year = {1980},
  abstract = {Important time scales considered include the pulsation period, the
'free-fall' time, the Kelvin time, and the 'nuclear' time. Some
observational and basic theoretical considerations are discussed, taking
into account classical Cepheids and the period-luminosity relation, more
recently recognized types of variable stars, the empirical determination
of radii of pulsating stars, limb darkening and radial velocity,
Eulerian and Lagrangian descriptions, the gravitational field, and the
energy conservation theorem for a self-gravitating system. Radial
oscillations of stars are described, giving attention to spherically
symmetric radial motion, linearized equations, linear adiabatic radial
oscillations, the pulsational stability of actual stars, the phase lag,
and simple models of stellar pulsation. Nonradial oscillations of stars
are studied, taking into account the general nonlinear partial
differential equation, the hermiticity of the linear adiabatic wave
equation, the growth or decay of small nonradial oscillations, and
linear nonradial oscillations of spherical stars.},
  journal = {Research supported by the National Science Foundation Princeton, NJ, Princeton University Press, 1980. 393 p.},
  keywords = {Adiabatic Conditions,Astrophysics,Conservation Equations,Nonadiabatic Conditions,Radial Velocity,Stellar Gravitation,Stellar Luminosity,Stellar Models,Stellar Oscillations,Variable Stars,Wave Equations}
}

@article{creevey+2017,
  title = {Seismic Inference of 57 Stars Using Full-Length {{Kepler}} Data Sets},
  author = {Creevey, Orlagh and Metcalfe, Travis and Salabert, David and Mathur, Savita and Schultheis, Mathias and Garc{\'i}a, Rafael A. and Th{\'e}venin, Fr{\'e}d{\'e}ric and Bazot, Micha{\"e}l and Xu, Haiying},
  year = {2017},
  month = mar,
  abstract = {We present stellar properties (mass, age, radius, distances) of 57 stars from a seismic inference using full-length data sets from Kepler. These stars comprise active stars, planet-hosts, solar-analogs, and binary systems. We validate the distances derived from the astrometric Gaia-Tycho solution. Ensemble analysis of the stellar properties reveals a trend of mixing-length parameter with the surface gravity and effective temperature. We derive a linear relationship with the seismic quantity \$\textbackslash langle r\_\{02\} \textbackslash rangle\$ to estimate the stellar age. Finally, we define the stellar regimes where the Kjeldsen et al (2008) empirical surface correction for 1D model frequencies is valid.},
  archivePrefix = {arXiv},
  eprint = {1703.01084},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/ZDHQSGGA/Creevey et al. - 2017 - Seismic inference of 57 stars using full-length Ke.pdf;/Users/Oliver/Zotero/storage/DAA6DFGR/1703.html},
  journal = {arXiv:1703.01084 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Instrumentation and Methods for Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{creevey+2017a,
  title = {Characterizing Solar-Type Stars from Full-Length {{Kepler}} Data Sets Using the {{Asteroseismic Modeling Portal}}},
  author = {Creevey, O. L. and Metcalfe, T. S. and Schultheis, M. and Salabert, D. and Bazot, M. and Th{\'e}venin, F. and Mathur, S. and Xu, H. and Garc{\'i}a, R. A.},
  year = {2017},
  month = may,
  volume = {601},
  pages = {A67},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201629496},
  abstract = {The Kepler space telescope yielded unprecedented data for the study of
solar-like oscillations in other stars. The large samples of multi-year
observations posed an enormous data analysis challenge that has only
recently been surmounted. Asteroseismic modeling has become more
sophisticated over time, with better methods gradually developing
alongside the extended observations and improved data analysis
techniques. We apply the latest version of the Asteroseismic Modeling
Portal (AMP) to the full-length Kepler data sets for 57 stars,
comprising planetary hosts, binaries, solar-analogs, active stars, and
for validation purposes, the Sun. From an analysis of the derived
stellar properties for the full sample, we identify a variation of the
mixing-length parameter with atmospheric properties. We also derive a
linear relation between the stellar age and a characteristic frequency
separation ratio. In addition, we find that the empirical correction for
surface effects suggested by Kjeldsen and coworkers is adequate for
solar-type stars that are not much hotter (Teff{$\lessequivlnt$}6200 K)
or significantly more evolved (log g{$\greaterequivlnt$}4.2, {$\langle$} {$\Delta\nu$}
{$\rangle\greaterequivlnt$}80 {$\mu$}Hz) than the Sun. Precise parallaxes from the Gaia
mission and future observations from TESS and PLATO promise to improve
the reliability of stellar properties derived from asteroseismology.

Tables A.1-A.3 are also available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A67},
  file = {/Users/Oliver/Zotero/storage/24KJXU8I/Creevey et al. - 2017 - Characterizing solar-type stars from full-length K.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {asteroseismology,methods: numerical,stars: fundamental parameters,stars: interiors,stars: oscillations}
}

@article{crossfield+2017,
  title = {Two {{Small Transiting Planets}} and a {{Third Body Orbiting HD}} 106315},
  author = {Crossfield, Ian J. M. and Ciardi, David R. and Isaacson, Howard and Howard, Andrew W. and Petigura, Erik A. and Weiss, Lauren M. and Fulton, Benjamin J. and Sinukoff, Evan and Schlieder, Joshua E. and Mawet, Dimitri and Ruane, Garreth and {de Pater}, Imke and {de Kleer}, Katherine and Davies, Ashley G. and Christiansen, Jessie L. and Dressing, Courtney D. and Hirsch, Lea and Benneke, Bj{\"o}rn and Crepp, Justin R. and Kosiarek, Molly and Livingston, John and Gonzales, Erica and Beichman, Charles A. and Knutson, Heather A.},
  year = {2017},
  month = jan,
  abstract = {The masses, atmospheric makeups, spin-orbit alignments, and system architectures of extrasolar planets can be best studied when the planets orbit bright stars. We report the discovery of three bodies orbiting HD 106315, a bright (V = 8.97 mag) F5 dwarf targeted by our K2 survey for transiting exoplanets. Two small, transiting planets have radii of 2.23 (+0.30/-0.25) R\_Earth and 3.95 (+0.42/-0.39) R\_Earth and orbital periods of 9.55 d and 21.06 d, respectively. A radial velocity (RV) trend of 3.55 +/- 0.10 m/s/day indicates the presence of a third body orbiting HD 106315 with period {$>$}80 d and mass {$>$}M\_Jup. Transits of this object would have depths of \textasciitilde 1\% and are definitively ruled out. Though the star has v sin i=13.2 km/s, it exhibits short-timescale RV variability of just 6.4 m/s, and so is a good target for RV measurements of the mass and density of the inner two planets and the outer object's orbit and mass. Furthermore, the combination of RV jitter and moderate v sin i makes HD 106315 a valuable laboratory for studying the spin-orbit alignment of small planets through the Rossiter-McLaughlin effect. Space-based atmospheric characterization of the two transiting planets via transit and eclipse spectroscopy should also be feasible. This discovery demonstrates again the power of K2 to find compelling exoplanets worthy of future study.},
  archivePrefix = {arXiv},
  eprint = {1701.03811},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/3PQS8JGW/Crossfield et al. - 2017 - Two Small Transiting Planets and a Third Body Orbi.pdf;/Users/Oliver/Zotero/storage/3TJHRHRT/1701.html},
  journal = {arXiv:1701.03811 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{curtis+2019,
  title = {A {{Temporary Epoch}} of {{Stalled Spin}}-{{Down}} for {{Low}}-{{Mass Stars}}: {{Insights}} from {{NGC}} 6811 with {{Gaia}} and {{Kepler}}},
  shorttitle = {A {{Temporary Epoch}} of {{Stalled Spin}}-{{Down}} for {{Low}}-{{Mass Stars}}},
  author = {Curtis, Jason Lee and Ag{\"u}eros, Marcel A. and Douglas, Stephanie T. and Meibom, S{\o}ren},
  year = {2019},
  month = jul,
  volume = {879},
  pages = {49},
  issn = {1538-4357},
  doi = {10.3847/1538-4357/ab2393},
  abstract = {Stellar rotation was proposed as a potential age diagnostic that is precise, simple, and applicable to a broad range of low-mass stars (\$\textbackslash leq\$1 \$M\_\textbackslash odot\$). Unfortunately, rotation period \$(P\_\{\textbackslash rm rot\})\$ measurements of low-mass members of open clusters have undermined the idea that stars spin down with a common age dependence (i.e., \$P\_\{\textbackslash rm rot\} \textbackslash propto \textbackslash sqrt\{\textbackslash rm age\}\$): K dwarfs appear to spin down more slowly than F and G dwarfs. Ag\textbackslash "ueros et al. (2018) interpreted data for the \$\textbackslash approx\$1.4-Gyr-old cluster NGC 752 differently, proposing that after having converged onto a slow-rotating sequence in their first 600-700 Myr (by the age of Praesepe), K dwarf \$P\_\{\textbackslash rm rot\}\$ stall on that sequence for an extended period of time. We use data from Gaia DR2 to identify likely single-star members of the \$\textbackslash approx\$1-Gyr-old cluster NGC 6811 with Kepler light curves. We measure \$P\_\{\textbackslash rm rot\}\$ for 171 members, more than doubling the sample relative to the existing catalog and extending the mass limit from \$\textbackslash approx\$0.8 to \$\textbackslash approx\$0.6 \$M\_\textbackslash odot\$. We then apply a gyrochronology formula calibrated with Praesepe and the Sun to 27 single G dwarfs in NGC 6811 to derive a precise gyrochronological age for the cluster of 1.04\$\textbackslash pm\$0.07 Gyr. However, when our new low-mass rotators are included, NGC 6811's color-\$P\_\{\textbackslash rm rot\}\$ sequence deviates away from the naive 1 Gyr projection down to \$T\_\{\textbackslash rm eff\} \textbackslash approx 4295\$ K (K5V, 0.7 \$M\_\textbackslash odot\$), where it clearly overlaps with Praesepe's. Combining these data with \$P\_\{\textbackslash rm rot\}\$ for other clusters, we conclude that the assumption that mass and age are separable dependencies is invalid. Furthermore, the cluster data show definitively that stars experience a temporary epoch of reduced braking efficiency where \$P\_\{\textbackslash rm rot\}\$ stall, and that the duration of this epoch lasts longer for lower-mass stars.},
  archivePrefix = {arXiv},
  eprint = {1905.06869},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/P5X2TPSQ/Curtis et al. - 2019 - A Temporary Epoch of Stalled Spin-Down for Low-Mas.pdf;/Users/Oliver/Zotero/storage/P8DXMSDA/1905.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{dalba+2016,
  title = {Kepler {{Transit Depths Contaminated}} by a {{Phantom Star}}},
  author = {Dalba, Paul A. and Muirhead, Philip S. and Croll, Bryce and Kempton, Eliza M.-R.},
  year = {2016},
  month = dec,
  abstract = {We present ground-based observations from the Discovery Channel Telescope (DCT) of three transits of Kepler-445c---a supposed super-Earth exoplanet with properties resembling GJ 1214b---and demonstrate that the transit depth is approximately 50 percent shallower than the depth previously inferred from Kepler Spacecraft data. The resulting decrease in planetary radius significantly alters the interpretation of the exoplanet's bulk composition. Despite the faintness of the M4 dwarf host star, our ground-based photometry clearly recovers each transit and achieves repeatable 1-sigma precision of approximately 0.2 percent (2 millimags). The transit parameters estimated from the DCT data are discrepant with those inferred from the Kepler data to at least 17-sigma confidence. This inconsistency is due to a subtle miscalculation of the stellar crowding metric during the Kepler pre-search data conditioning (PDC). The crowding metric, or CROWDSAP, is contaminated by a non-existent "phantom star" originating in the USNO-B1 catalog and inherited by the Kepler Input Catalog (KIC). Phantom stars in the KIC are likely rare, but they have the potential to affect statistical studies of Kepler targets that use the PDC transit depths for a large number of exoplanets where individual follow-up observation of each is not possible. The miscalculation of Kepler-445c's transit depth emphasizes the importance of stellar crowding in the Kepler data, and provides a cautionary tale for the analysis of data from the Transiting Exoplanet Survey Satellite (TESS), which will have even larger pixels than Kepler.},
  archivePrefix = {arXiv},
  eprint = {1612.02432},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/BHUCNVDQ/Dalba et al. - 2016 - Kepler Transit Depths Contaminated by a Phantom St.pdf;/Users/Oliver/Zotero/storage/5DD59CVC/1612.html},
  journal = {arXiv:1612.02432 [astro-ph]},
  keywords = {C3,Notes},
  primaryClass = {astro-ph}
}

@article{dalton+2014,
  title = {Project Overview and Update on {{WEAVE}}: The next Generation Wide-Field Spectroscopy Facility for the {{William Herschel Telescope}}},
  shorttitle = {Project Overview and Update on {{WEAVE}}},
  author = {Dalton, Gavin and Trager, Scott and Abrams, Don Carlos and Bonifacio, Piercarlo and L{\'o}pez Aguerri, J. Alfonso and Middleton, Kevin and Benn, Chris and Dee, Kevin and Say{\`e}de, Fr{\'e}d{\'e}ric and Lewis, Ian and Pragt, Johan and Pico, Sergio and Walton, Nic and Rey, Juerg and Allende Prieto, Carlos and Pe{\~n}ate, Jos{\'e} and Lhome, Emilie and Ag{\'o}cs, Tibor and Alonso, Jos{\'e} and Terrett, David and Brock, Matthew and Gilbert, James and Ridings, Andy and Guinouard, Isabelle and Verheijen, Marc and Tosh, Ian and Rogers, Kevin and Steele, Iain and Stuik, Remko and Tromp, Neils and Jasko, Attila and Kragt, Jan and Lesman, Dirk and Mottram, Chris and Bates, Stuart and Gribbin, Frank and Fernando Rodriguez, Luis and Delgado, Jos{\'e} M. and Martin, Carlos and Cano, Diego and Navarro, Ram{\'o}n and Irwin, Mike and Lewis, Jim and Gonzalez Solares, Eduardo and O'Mahony, Neil and Bianco, Andrea and Zurita, Christina and {ter Horst}, Rik and Molinari, Emilio and Lodi, Marcello and Guerra, Jos{\'e} and Vallenari, Antonella and Baruffolo, Andrea},
  year = {2014},
  month = jul,
  volume = {9147},
  pages = {91470L},
  address = {{eprint: arXiv:1412.0843}},
  doi = {10.1117/12.2055132},
  abstract = {We present an overview of and status report on the WEAVE next-generation
spectroscopy facility for the William Herschel Telescope (WHT). WEAVE
principally targets optical ground-based follow up of upcoming
ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a
multi-object and multi-IFU facility utilizing a new 2-degree prime focus
field of view at the WHT, with a buffered pick-and-place positioner
system hosting 1000 multi-object (MOS) fibres, 20 integral field units,
or a single large IFU for each observation. The fibres are fed to a
single spectrograph, with a pair of 8k(spectral) x 6k (spatial) pixel
cameras, located within the WHT GHRIL enclosure on the telescope Nasmyth
platform, supporting observations at R\textasciitilde 5000 over the full 370-1000nm
wavelength range in a single exposure, or a high resolution mode with
limited coverage in each arm at R\textasciitilde 20000. The project is now in the final
design and early procurement phase, with commissioning at the telescope
expected in 2017.},
  file = {/Users/Oliver/Zotero/storage/ES9I846X/Dalton et al. - 2014 - Project overview and update on WEAVE the next gen.pdf}
}

@article{datta+2015,
  title = {Automated Determination of G-Mode Period Spacing of Red Giant Stars},
  author = {Datta, Abhisek and Mazumdar, Anwesh and Gupta, Umang and Hekker, Saskia},
  year = {2015},
  month = feb,
  volume = {447},
  pages = {1935},
  doi = {10.1093/mnras/stu2499},
  abstract = {The Kepler satellite has provided photometric timeseries data of unprecedented length, duty cycle and precision. To fully analyse these data for the tens of thousands of stars observed by Kepler, automated methods are a prerequisite. Here, we present an automated procedure to determine the period spacing of gravity modes in red giant stars ascending the red giant branch. The gravity modes reside in a cavity in the deep interior of the stars and provide information on the conditions in the stellar core. However, for red giants the gravity modes are not directly observable on the surface, hence this method is based on the pressure-gravity mixed modes that present observable features in the Fourier power spectrum. The method presented here is based on the vertical alignment and symmetry of these mixed modes in a period echelle diagram. We find that we can obtain reliable results for both model frequencies and observed frequencies. Additionally, we carried out Monte Carlo tests to obtain realistic uncertainties on the period spacings with different set of oscillation modes (for the models) and uncertainties on the frequencies. Furthermore, this method has been used to improve mode detection and identification of the observed frequencies in an iterative manner.},
  file = {/Users/Oliver/Zotero/storage/HN85K84T/Datta et al. - 2015 - Automated determination of g-mode period spacing o.pdf;/Users/Oliver/Zotero/storage/BRBGQJVF/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{davenport+2019,
  title = {The {{Evolution}} of {{Flare Activity}} with {{Stellar Age}}},
  author = {Davenport, James R. A. and Covey, Kevin R. and Clarke, Riley W. and Boeck, Austin C. and Cornet, Jonathan and Hawley, Suzanne L.},
  year = {2019},
  month = feb,
  volume = {871},
  pages = {241},
  doi = {10.3847/1538-4357/aafb76},
  abstract = {Using a recent census of flare stars from the Kepler survey, we have explored how flare activity evolves across stellar main-sequence lifetimes. We utilize a sample of 347 stars with robust flare activity detections and which have rotation periods measured via starspot modulations in their Kepler light curves. We consider three separate methods for quantifying flare activity from optical light curves and compare their utility for comparing flare activity between stars of differing ages and luminosities. These metrics include the fractional luminosity emitted in flares, the specific rate of flares emitted at a given energy, and a model for the entire flare frequency distribution (FFD). With all three approaches, we find that flare activity decreases for all low-mass stars as they spin down, and thus with age. Most striking is the evolution of the flare occurrence frequency distributions, which show no significant change in the power-law slope with age. Since our sample is preferentially constructed of younger, more active stars, our model overpredicts the superflare rate previously estimated for the Sun. Finally, we parameterize our best-fit model of the FFD for ease in predicting the rates of flares and their associated impacts on planet habitability and detection.},
  file = {/Users/Oliver/Zotero/storage/MK3FFJDC/Davenport et al. - 2019 - The Evolution of Flare Activity with Stellar Age.pdf;/Users/Oliver/Zotero/storage/PZ2YHNM2/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{davenport+covey2018,
  title = {Rotating {{Stars}} from {{Kepler Observed}} with {{Gaia DR2}}},
  author = {Davenport, James R. A. and Covey, Kevin R.},
  year = {2018},
  month = jul,
  pages = {arXiv:1807.09841},
  abstract = {We have matched the astrometric data from Gaia Data Release 2 to the sample of stars with measured rotation periods from Kepler. Using 30,305 stars with good distance estimates, we select 16,248 as being likely main sequence single stars centered within a 0.5 mag region about a 1 Gyr isochrone, removing many sub-giants and unresolved binary stars from the sample. The rotation period bimodality, originally discovered by McQuillan et al. (2013), is clearly recovered for stars out to 525pc, but is not detectable at further distances. This bimodality correlates with Galactic height as well, dropping strongly for stars above Z\>90 pc. We also find a significant width in the stellar main sequence of \$\textbackslash Delta M\_G\$ \textasciitilde 0.25 mag, as well as a coherent gradient of increasing rotation periods orthogonal to the main sequence. We interpret this as a signature of stellar angular momentum loss over time, implying a corresponding diagonal age gradient across the main sequence. Stellar evolution models predict changes in color and luminosity that are consistent in amplitude, but not in direction, with those required to produce the gradient we have detected. This rotation gradient suggests that main sequence evolution produces offsets in color-magnitude space that are significantly more orthogonal to the zero-age main sequence than models currently predict, and may provide new tests for both stellar evolution and gyrochronology models.},
  file = {/Users/Oliver/Zotero/storage/EF6HSUWR/Davenport and Covey - 2018 - Rotating Stars from Kepler Observed with Gaia DR2.pdf;/Users/Oliver/Zotero/storage/Y5YW99QR/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{davies+2014,
  title = {{{BiSON}} Data Preparation: A Correction for Differential Extinction and the Weighted Averaging of Contemporaneous Data},
  shorttitle = {{{BiSON}} Data Preparation},
  author = {Davies, G. R. and Chaplin, W. J. and Elsworth, Y. and Hale, S. J.},
  year = {2014},
  month = jul,
  volume = {441},
  pages = {3009--3017},
  issn = {0035-8711},
  doi = {10.1093/mnras/stu803},
  abstract = {The Birmingham Solar Oscillations Network (BiSON) has provided
high-quality high-cadence observations from as far back in time as 1978.
These data must be calibrated from the raw observations into radial
velocity and the quality of the calibration has a large impact on the
signal-to-noise ratio of the final time series. The aim of this work is
to maximize the potential science that can be performed with the BiSON
data set by optimizing the calibration procedure. To achieve better
levels of signal-to-noise ratio, we perform two key steps in the
calibration process: we attempt a correction for terrestrial atmospheric
differential extinction; and the resulting improvement in the
calibration allows us to perform weighted averaging of contemporaneous
data from different BiSON stations. The improvements listed produce
significant improvement in the signal-to-noise ratio of the BiSON
frequency-power spectrum across all frequency ranges. The reduction of
noise in the power spectrum will allow future work to provide greater
constraint on changes in the oscillation spectrum with solar activity.
In addition, the analysis of the low-frequency region suggests that we
have achieved a noise level that may allow us to improve estimates of
the upper limit of g-mode amplitudes.},
  file = {/Users/Oliver/Zotero/storage/EYPY3LD3/Davies et al. - 2014 - BiSON data preparation a correction for different.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {methods: data analysis,Sun: helioseismology,Sun: oscillations}
}

@article{davies+2014a,
  title = {The {{Long}}-{{Term Dynamical Evolution}} of {{Planetary Systems}}},
  author = {Davies, Melvyn B. and Adams, Fred C. and Armitage, Philip and Chambers, John and Ford, Eric and Morbidelli, Alessandro and Raymond, Sean N. and Veras, Dimitri},
  year = {2014},
  doi = {\{10.2458/azu_uapress_9780816531240-ch034\}},
  abstract = {This chapter concerns the long-term dynamical evolution of planetary systems from both theoretical and observational perspectives. We begin by discussing the planet-planet interactions that take place within our own Solar System. We then describe such interactions in more tightly-packed planetary systems. As planet-planet interactions build up, some systems become dynamically unstable, leading to strong encounters and ultimately either ejections or collisions of planets. After discussing the basic physical processes involved, we consider how these interactions apply to extrasolar planetary systems and explore the constraints provided by observed systems. The presence of a residual planetesimal disc can lead to planetary migration and hence cause instabilities induced by resonance crossing; however, such discs can also stabilise planetary systems. The crowded birth environment of a planetary system can have a significant impact: close encounters and binary companions can act to destabilise systems, or sculpt their properties. In the case of binaries, the Kozai mechanism can place planets on extremely eccentric orbits which may later circularise to produce hot Jupiters.},
  archivePrefix = {arXiv},
  eprint = {1311.6816},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/C2V3T94F/Davies et al. - 2014 - The Long-Term Dynamical Evolution of Planetary Sys.pdf;/Users/Oliver/Zotero/storage/5Q6Q69WJ/1311.html},
  journal = {arXiv:1311.6816 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{davies+2014b,
  title = {Low-Frequency, Low-Degree Solar p-Mode Properties from 22 Years of {{Birmingham Solar Oscillations Network}} Data},
  author = {Davies, G. R. and Broomhall, A. M. and Chaplin, W. J. and Elsworth, Y. and Hale, S. J.},
  year = {2014},
  month = apr,
  volume = {439},
  pages = {2025--2032},
  issn = {0035-8711},
  doi = {10.1093/mnras/stu080},
  abstract = {The solar low-degree low-frequency modes of oscillation are of
particular interest as their frequencies can be measured with very high
precision and hence provide good constraints on seismic models. Here we
detect and characterize these valuable measures of the solar interior
from a 22 yr Birmingham Solar Oscillations Network data set. We report
mode frequencies, line widths, heights, amplitudes, and rotational
splitting, all with robust uncertainties. The new values of frequency,
rotational splitting, amplitude, and line width we provide will help
place new constraints on hydrostatic and rotational structure, plus
diagnostics of near-surface convection. Further to this, by assuming
simple power laws, we extrapolate mode properties to lower frequencies.
We demonstrate that the low-l low-frequency p modes have a low
signal-to-noise ratio and that this cannot be overcome simply by
continued observation. It will be necessary to observe the Sun in novel
ways to `beat' the intrinsic granulation noise.},
  file = {/Users/Oliver/Zotero/storage/HRSSS5JR/Davies et al. - 2014 - Low-frequency, low-degree solar p-mode properties .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {methods: data analysis,Sun: helioseismology,Sun: oscillations}
}

@article{davies+2015,
  title = {Asteroseismic Inference on Rotation, Gyrochronology and Planetary System Dynamics of 16 {{Cygni}}},
  author = {Davies, G. R. and Chaplin, W. J. and Farr, W. M. and Garc{\'i}a, R. A. and Lund, M. N. and Mathis, S. and Metcalfe, T. S. and Appourchaux, T. and Basu, S. and Benomar, O. and Campante, T. L. and Ceillier, T. and Elsworth, Y. and Handberg, R. and Salabert, D. and Stello, D.},
  year = {2015},
  month = jan,
  volume = {446},
  pages = {2959},
  doi = {10.1093/mnras/stu2331},
  abstract = {The solar analogues 16 Cyg A and B are excellent asteroseismic targets in the Kepler field of view and together with a red dwarf and a Jovian planet form an interesting system. For these more evolved Sun-like stars we cannot detect surface rotation with the current Kepler data but instead use the technique of asteroseimology to determine rotational properties of both 16 Cyg A and B. We find the rotation periods to be 23.8\^\{+1.5\}\_\{-1.8\} and 23.2\^\{+11.5\}\_\{-3.2\} d, and the angles of inclination to be 56\^\{+6\}\_\{-5\}\textdegree{} and 36\^\{+17\}\_\{-7\}\textdegree, for A and B, respectively. Together with these results we use the published mass and age to suggest that, under the assumption of a solar-like rotation profile, 16 Cyg A could be used when calibrating gyrochronology relations. In addition, we discuss the known 16 Cyg B star-planet eccentricity and measured low obliquity which is consistent with Kozai cycling and tidal theory.},
  file = {/Users/Oliver/Zotero/storage/EI56XGG3/Davies et al. - 2015 - Asteroseismic inference on rotation, gyrochronolog.pdf;/Users/Oliver/Zotero/storage/X6XA2END/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Core Gyrochronology,Seismic Age,Seismic rotation},
  language = {en},
  number = {3}
}

@article{davies+2016,
  title = {Oscillation Frequencies for 35 {{Kepler}} Solar-Type Planet-Hosting Stars Using {{Bayesian}} Techniques and Machine Learning},
  author = {Davies, G. R. and Silva Aguirre, V. and Bedding, T. R. and Handberg, R. and Lund, M. N. and Chaplin, W. J. and Huber, D. and White, T. R. and Benomar, O. and Hekker, S. and Basu, S. and Campante, T. L. and {Christensen-Dalsgaard}, J. and Elsworth, Y. and Karoff, C. and Kjeldsen, H. and Lundkvist, M. S. and Metcalfe, T. S. and Stello, D.},
  year = {2016},
  month = feb,
  volume = {456},
  pages = {2183},
  doi = {10.1093/mnras/stv2593},
  abstract = {Kepler has revolutionized our understanding of both exoplanets and their host stars. Asteroseismology is a valuable tool in the characterization of stars and Kepler is an excellent observing facility to perform asteroseismology. Here we select a sample of 35 Kepler solar-type stars which host transiting exoplanets (or planet candidates) with detected solar-like oscillations. Using available Kepler short cadence data up to Quarter 16 we create power spectra optimized for asteroseismology of solar-type stars. We identify modes of oscillation and estimate mode frequencies by `peak bagging' using a Bayesian Markov Chain Monte Carlo framework. In addition, we expand the methodology of quality assurance using a Bayesian unsupervised machine learning approach. We report the measured frequencies of the modes of oscillation for all 35 stars and frequency ratios commonly used in detailed asteroseismic modelling. Due to the high correlations associated with frequency ratios we report the covariance matrix of all frequencies measured and frequency ratios calculated. These frequencies, frequency ratios, and covariance matrices can be used to obtain tight constraint on the fundamental parameters of these planet-hosting stars.},
  file = {/Users/Oliver/Zotero/storage/HMQ3CKLP/Davies et al. - 2016 - Oscillation frequencies for 35 Kepler solar-type p.pdf;/Users/Oliver/Zotero/storage/GXAL99HX/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{davies+2017,
  title = {Using Red Clump Stars to Correct the {{Gaia DR1}} Parallaxes},
  author = {Davies, Guy R. and Lund, Mikkel N. and Miglio, Andrea and Elsworth, Yvonne and Kuszlewicz, James S. and North, Thomas S. H. and Rendle, Ben and Chaplin, William J. and Rodrigues, Tha{\'i}se S. and Campante, Tiago L. and Girardi, L{\'e}o and Hale, Steven J. and Hall, Oliver and Jones, Caitlin D. and Kawaler, Steven D. and Roxburgh, Ian and Schofield, Mathew},
  year = {2017},
  month = feb,
  volume = {598},
  pages = {L4},
  doi = {10.1051/0004-6361/201630066},
  abstract = {Recent results have suggested that there is tension between the Gaia DR1 TGAS distances and the distances obtained using luminosities determined by eclipsing binaries or asteroseismology on red giant stars. We use the K\textsubscript{s}-band luminosities of red clump stars, identified and characterized by asteroseismology, to make independent distance estimates. Our results suggest that Gaia TGAS distances contain a systematic error that decreases with increasing distance. We propose a correction to mitigate this offset as a function of parallax that is valid for the Kepler field and values of parallax that are less than 1.6 mas. For parallaxes greater than this, we find agreement with previously published values. We note that the TGAS distances to the red clump stars of the open cluster M67 show a high level of disagreement that is difficult to correct for.},
  file = {/Users/Oliver/Zotero/storage/8VHY875U/Davies et al. - 2017 - Using red clump stars to correct the Gaia DR1 para.pdf;/Users/Oliver/Zotero/storage/ALZ85KWN/abstract.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{davies+miglio2016,
  title = {Asteroseismology of Red Giants: {{From}} Analysing Light Curves to Estimating Ages},
  shorttitle = {Asteroseismology of Red Giants},
  author = {Davies, G. R. and Miglio, A.},
  year = {2016},
  month = sep,
  volume = {337},
  pages = {774},
  doi = {10.1002/asna.201612371},
  abstract = {Asteroseismology has started to provide constraints on stellar properties that will be essential to accurately reconstruct the history of the Milky Way. Here we look at the information content in data sets representing current and future space missions (CoRoT, Kepler, K2, TESS, and PLATO) for red giant stars. We describe techniques for extracting the information in the frequency power spectrum and apply these techniques to Kepler data sets of different observing length to represent the different space missions. We demonstrate that for KIC 12008916, a low-luminosity red giant branch star, we can extract useful information from all data sets, and for all but the shortest data set we obtain good constraint on the g-mode period spacing and core rotation rates. We discuss how the high precision in these parameters will constrain the stellar properties of stellar radius, distance, mass and age. We show that high precision can be achieved in mass and hence age when values of the g-mode period spacing are available. We caution that tests to establish the accuracy of asteroseismic masses and ages are still ``work in progress''.},
  file = {/Users/Oliver/Zotero/storage/LYPC3VZU/Davies and Miglio - 2016 - Asteroseismology of red giants From analysing lig.pdf;/Users/Oliver/Zotero/storage/W5JVCII2/ui.adsabs.harvard.edu.html},
  journal = {Astronomische Nachrichten},
  language = {en},
  number = {8-9}
}

@article{deal+2017,
  title = {Asteroseismology of the Exoplanet-Host {{F}}-Type Star 94 {{Ceti}} : Impact of Atomic Diffusion on the Stellar Parameters},
  shorttitle = {Asteroseismology of the Exoplanet-Host {{F}}-Type Star 94 {{Ceti}}},
  author = {Deal, M. and Escobar, M. E. and Vauclair, S. and Vauclair, G. and {Hui-Bon-Hoa}, A. and Richard, O.},
  year = {2017},
  month = feb,
  abstract = {A precision of order one percent is needed on the parameters of exoplanet-hosts stars in order to correctly characterize the planets themselves. This will be achieved by asteroseismology. It is important in this context to test the influence on the derived parameters of introducing atomic diffusion with radiative accelerations in the models. In this paper, we begin this study with the case of the star 94 Ceti A. We performed a complete asteroseismic analysis of the exoplanet-host F-type star 94 Ceti A, from the first radial-velocity observations with HARPS up to the final computed best models. This star is hot enough to suffer from important effects of atomic diffusion, including radiative accelerations. We tested the influence of such effects on the computed frequencies and on the determined stellar parameters. We also tested the effect of including a complete atmosphere in the stellar models. The radial velocity observations were done with HARPS in 2007. The low degree modes were derived and identified using classical methods and compared with the results obtained from stellar models computed with the Toulouse Geneva Evolution Code (TGEC). We obtained precise parameters for the star 94 Ceti A. We showed that including atomic diffusion with radiative accelerations can modify the age by a few percents, whereas adding a complete atmosphere does not change the results by more than one percent.},
  archivePrefix = {arXiv},
  eprint = {1702.03170},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/PJVTWKV8/Deal et al. - 2017 - Asteroseismology of the exoplanet-host F-type star.pdf;/Users/Oliver/Zotero/storage/HK8GEPV6/1702.html},
  journal = {arXiv:1702.03170 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{deheuvels+2012,
  title = {Seismic {{Evidence}} for a {{Rapidly Rotating Core}} in a {{Lower}}-Giant-Branch {{Star Observed}} with {{Kepler}}},
  author = {Deheuvels, S. and Garc{\'i}a, R. A. and Chaplin, W. J. and Basu, S. and Antia, H. M. and Appourchaux, T. and Benomar, O. and Davies, G. R. and Elsworth, Y. and Gizon, L. and Goupil, M. J. and Reese, D. R. and Regulo, C. and Schou, J. and Stahn, T. and Casagrande, L. and {Christensen-Dalsgaard}, J. and Fischer, D. and Hekker, S. and Kjeldsen, H. and Mathur, S. and Mosser, B. and Pinsonneault, M. and Valenti, J. and Christiansen, J. L. and Kinemuchi, K. and Mullally, F.},
  year = {2012},
  month = sep,
  volume = {756},
  pages = {19},
  doi = {10.1088/0004-637X/756/1/19},
  abstract = {Rotation is expected to have an important influence on the structure and the evolution of stars. However, the mechanisms of angular momentum transport in stars remain theoretically uncertain and very complex to take into account in stellar models. To achieve a better understanding of these processes, we desperately need observational constraints on the internal rotation of stars, which until very recently was restricted to the Sun. In this paper, we report the detection of mixed modes\textemdash i.e., modes that behave both as g modes in the core and as p modes in the envelope\textemdash in the spectrum of the early red giant KIC 7341231, which was observed during one year with the Kepler spacecraft. By performing an analysis of the oscillation spectrum of the star, we show that its non-radial modes are clearly split by stellar rotation and we are able to determine precisely the rotational splittings of 18 modes. We then find a stellar model that reproduces very well the observed atmospheric and seismic properties of the star. We use this model to perform inversions of the internal rotation profile of the star, which enables us to show that the core of the star is rotating at least five times faster than the envelope. This will shed new light on the processes of transport of angular momentum in stars. In particular, this result can be used to place constraints on the angular momentum coupling between the core and the envelope of early red giants, which could help us discriminate between the theories that have been proposed over the last few decades.},
  file = {/Users/Oliver/Zotero/storage/DVSUNXET/Deheuvels et al. - 2012 - Seismic Evidence for a Rapidly Rotating Core in a .pdf;/Users/Oliver/Zotero/storage/VCCB5QXW/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{deheuvels+2014,
  title = {Seismic Constraints on the Radial Dependence of the Internal Rotation Profiles of Six {{Kepler}} Subgiants and Young Red Giants},
  author = {Deheuvels, S. and Do{\u g}an, G. and Goupil, M. J. and Appourchaux, T. and Benomar, O. and Bruntt, H. and Campante, T. L. and Casagrande, L. and Ceillier, T. and Davies, G. R. and De Cat, P. and Fu, J. N. and Garc{\'i}a, R. A. and Lobel, A. and Mosser, B. and Reese, D. R. and Regulo, C. and Schou, J. and Stahn, T. and Thygesen, A. O. and Yang, X. H. and Chaplin, W. J. and {Christensen-Dalsgaard}, J. and Eggenberger, P. and Gizon, L. and Mathis, S. and {Molenda-{\.Z}akowicz}, J. and Pinsonneault, M.},
  year = {2014},
  month = apr,
  volume = {564},
  pages = {A27},
  doi = {10.1051/0004-6361/201322779},
  abstract = {Context. We still do not understand which physical mechanisms are responsible for the transport of angular momentum inside stars. The recent detection of mixed modes that contain the clear signature of rotation in the spectra of Kepler subgiants and red giants gives us the opportunity to make progress on this question. \\
 Aims: Our aim is to probe the radial dependence of the rotation profiles for a sample of Kepler targets. For this purpose, subgiants and early red giants are particularly interesting targets because their rotational splittings are more sensitive to the rotation outside the deeper core than is the case for their more evolved counterparts. \\
 Methods: We first extracted the rotational splittings and frequencies of the modes for six young Kepler red giants. We then performed a seismic modeling of these stars using the evolutionary codes Cesam2k and astec. By using the observed splittings and the rotational kernels of the optimal models, we inverted the internal rotation profiles of the six stars. \\
 Results: We obtain estimates of the core rotation rates for these stars, and upper limits to the rotation in their convective envelope. We show that the rotation contrast between the core and the envelope increases during the subgiant branch. Our results also suggest that the core of subgiants spins up with time, while their envelope spins down. For two of the stars, we show that a discontinuous rotation profile with a deep discontinuity reproduces the observed splittings significantly better than a smooth rotation profile. Interestingly, the depths that are found to be most probable for the discontinuities roughly coincide with the location of the H-burning shell, which separates the layers that contract from those that expand. \\
 Conclusions: We characterized the differential rotation pattern of six young giants with a range of metallicities, and with both radiative and convective cores on the main sequence. This will bring observational constraints to the scenarios of angular momentum transport in stars. Moreover, if the existence of sharp gradients in the rotation profiles of young red giants is confirmed, it is expected to help in distinguishing between the physical processes that could transport angular momentum in the subgiant and red giant branches. Appendices and Tables 3-9 are available in electronic form at \href{http://www.aanda.org/10.1051/0004-6361/201322779/olm}{http://www.aanda.org}},
  file = {/Users/Oliver/Zotero/storage/2VTAJ2F3/Deheuvels et al. - 2014 - Seismic constraints on the radial dependence of th.pdf;/Users/Oliver/Zotero/storage/VXUVKCTK/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{dejong+2014,
  title = {{{4MOST}}: 4-Metre {{Multi}}-{{Object Spectroscopic Telescope}}},
  shorttitle = {{{4MOST}}},
  author = {{de Jong}, Roelof S. and Barden, Sam and {Bellido-Tirado}, Olga and Brynnel, Joar and Chiappini, Cristina and Depagne, {\'E}ric and Haynes, Roger and Johl, Diana and Phillips, Daniel P. and Schnurr, Olivier and Schwope, Axel D. and Walcher, Jakob and Bauer, Svend M. and Cescutti, Gabriele and Cioni, Maria-Rosa L. and Dionies, Frank and Enke, Harry and Haynes, Dionne M. and Kelz, Andreas and Kitaura, Francisco S. and Lamer, Georg and Minchev, Ivan and M{\"u}ller, Volker and Nuza, Sebasti{\'a}n. E. and Olaya, Jean-Christophe and Piffl, Tilmann and Popow, Emil and Saviauk, Allar and Steinmetz, Matthias and Ural, U{\v g}ur and Valentini, Monica and Winkler, Roland and Wisotzki, Lutz and Ansorge, Wolfgang R. and Banerji, Manda and Gonzalez Solares, Eduardo and Irwin, Mike and Kennicutt, Robert C. and King, David M. P. and McMahon, Richard and Koposov, Sergey and Parry, Ian R. and Sun, Xiaowei and Walton, Nicholas A. and Finger, Gert and Iwert, Olaf and Krumpe, Mirko and Lizon, Jean-Louis and Mainieri, Vincenzo and Amans, Jean-Philippe and Bonifacio, Piercarlo and Cohen, Matthieu and Fran{\c c}ois, Patrick and Jagourel, Pascal and Mignot, Shan B. and Royer, Fr{\'e}d{\'e}ric and Sartoretti, Paola and Bender, Ralf and Hess, Hans-Joachim and {Lang-Bardl}, Florian and Muschielok, Bernard and Schlichter, J{\"o}rg and B{\"o}hringer, Hans and Boller, Thomas and Bongiorno, Angela and Brusa, Marcella and Dwelly, Tom and Merloni, Andrea and Nandra, Kirpal and Salvato, Mara and Pragt, Johannes H. and Navarro, Ram{\'o}n and Gerlofsma, Gerrit and Roelfsema, Ronald and Dalton, Gavin B. and Middleton, Kevin F. and Tosh, Ian A. and Boeche, Corrado and Caffau, Elisabetta and Christlieb, Norbert and Grebel, Eva K. and Hansen, Camilla J. and Koch, Andreas and Ludwig, Hans-G. and Mandel, Holger and Quirrenbach, Andreas and Sbordone, Luca and Seifert, Walter and Thimm, Guido and Helmi, Amina and {trager}, Scott C. and Bensby, Thomas and Feltzing, Sofia and Ruchti, Gregory and Edvardsson, Bengt and Korn, Andreas and Lind, Karin and Boland, Wilfried and Colless, Matthew and Frost, Gabriella and Gilbert, James and Gillingham, Peter and Lawrence, Jon and Legg, Neville and Saunders, Will and Sheinis, Andrew and Driver, Simon and Robotham, Aaron and Bacon, Roland and Caillier, Patrick and Kosmalski, Johan and Laurent, Florence and Richard, Johan},
  year = {2014},
  month = jul,
  volume = {9147},
  pages = {91470M},
  doi = {10.1117/12.2055826},
  abstract = {4MOST is a wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of the European Southern Observatory (ESO). Its main science drivers are in the fields of galactic archeology, high-energy physics, galaxy evolution and
cosmology. 4MOST will in particular provide the spectroscopic
complements to the large area surveys coming from space missions like Gaia, eROSITA, Euclid, and PLATO and from ground-based facilities like VISTA, VST, DES, LSST and SKA. The 4MOST baseline concept features a 2.5 degree diameter field-of-view with \textasciitilde 2400 fibres in the focal surface that are configured by a fibre positioner based on the tilting spine principle. The fibres feed two types of spectrographs; \textasciitilde 1600 fibres go to two spectrographs with resolution R{$<$}5000 ({$\lambda\sptilde$}390-930 nm) and
\textasciitilde 800 fibres to a spectrograph with R{$>$}18,000 ({$\lambda\sptilde$}392-437 nm and
515-572 nm and 605-675 nm). Both types of spectrographs are
fixed-configuration, three-channel spectrographs. 4MOST will have an unique operations concept in which 5 year public surveys from both the consortium and the ESO community will be combined and observed in parallel during each exposure, resulting in more than 25 million spectra of targets spread over a large fraction of the southern sky. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing concept. 4MOST has been accepted for implementation by ESO with operations expected to start by the end of 2020. This paper provides a top-level overview of the 4MOST facility, while other papers in these proceedings provide more detailed descriptions of the
instrument concept[1], the instrument requirements development[2], the systems engineering implementation[3], the instrument model[4], the fibre positioner concepts[5], the fibre feed[6], and the
spectrographs[7].},
  file = {/Users/Oliver/Zotero/storage/B6P8QS8A/de Jong et al. - 2014 - 4MOST 4-metre Multi-Object Spectroscopic Telescop.pdf}
}

@article{deming+seager2017,
  title = {Illusion and {{Reality}} in the {{Atmospheres}} of {{Exoplanets}}},
  author = {Deming, Drake and Seager, Sara},
  year = {2017},
  month = jan,
  abstract = {The atmospheres of exoplanets reveal all their properties beyond mass, radius, and orbit. Based on bulk densities, we know that exoplanets larger than 1.5 Earth radii must have gaseous envelopes, hence atmospheres. We discuss contemporary techniques for characterization of exoplanetary atmospheres. The measurements are difficult, because - even in current favorable cases - the signals can be as small as 0.001-percent of the host star's flux. Consequently, some early results have been illusory, and not confirmed by subsequent investigations. Prominent illusions to date include polarized scattered light, temperature inversions, and the existence of carbon planets. The field moves from the first tentative and often incorrect conclusions, converging to the reality of exoplanetary atmospheres. That reality is revealed using transits for close-in exoplanets, and direct imaging for young or massive exoplanets in distant orbits. Several atomic and molecular constituents have now been robustly detected in exoplanets as small as Neptune. In our current observations, the effects of clouds and haze appear ubiquitous. Topics at the current frontier include the measurement of heavy element abundances in giant planets, detection of carbon-based molecules, measurement of atmospheric temperature profiles, definition of heat circulation efficiencies for tidally locked planets, and the push to detect and characterize the atmospheres of super-Earths. Future observatories for this quest include the James Webb Space Telescope, and the new generation of Extremely Large Telescopes on the ground. On a more distant horizon, NASA's concepts for the HabEx and LUVOIR missions could extend the study of exoplanetary atmospheres to true twins of Earth.},
  archivePrefix = {arXiv},
  eprint = {1701.00493},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/5XG5KU77/Deming and Seager - 2017 - Illusion and Reality in the Atmospheres of Exoplan.pdf;/Users/Oliver/Zotero/storage/HV3JEQC4/1701.html},
  journal = {arXiv:1701.00493 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{deng+2012,
  title = {{{LAMOST Experiment}} for {{Galactic Understanding}} and {{Exploration}} ({{LEGUE}}) \textemdash{} {{The}} Survey's Science Plan},
  author = {Deng, Li-Cai and Newberg, Heidi Jo and Liu, Chao and Carlin, Jeffrey L. and Beers, Timothy C. and Chen, Li and Chen, Yu-Qin and Christlieb, Norbert and Grillmair, Carl J. and Guhathakurta, Puragra and Han, Zhan-Wen and Hou, Jin-Liang and Lee, Hsu-Tai and L{\'e}pine, S{\'e}bastien and Li, Jing and Liu, Xiao-Wei and Pan, Kai-Ke and Sellwood, J. A. and Wang, Bo and Wang, Hong-Chi and Yang, Fan and Yanny, Brian and Zhang, Hao-Tong and Zhang, Yue-Yang and Zheng, Zheng and Zhu, Zi},
  year = {2012},
  month = jul,
  volume = {12},
  pages = {735--754},
  issn = {1674-4527},
  doi = {10.1088/1674-4527/12/7/003},
  abstract = {We describe the current plans for a spectroscopic survey of millions of
stars in the Milky Way galaxy using the Guo Shou Jing Telescope (GSJT,
formerly called the Large sky Area Multi-Object fiber Spectroscopic
Telescope \textemdash{} LAMOST). The survey will obtain spectra for 2.5
million stars brighter than r {$<$} 19 during dark/grey time, and 5
million stars brighter than r {$<$} 17 or J {$<$} 16 on nights that are
moonlit or have low transparency. The survey will begin in the fall of
2012, and will run for at least four years. The telescope's design
constrains the optimal declination range for observations to 10\textdegree{}
{$<$} {$\delta$} {$<$} 50\textdegree, and site conditions lead to an emphasis on
stars in the direction of the Galactic anticenter. The survey is divided
into three parts with different target selection strategies: disk,
anticenter, and spheroid. The resulting dataset will be used to study
the merger history of the Milky Way, the substructure and evolution of
the disks, the nature of the first generation of stars through
identification of the lowest metallicity stars, and star formation
through study of open clusters and OB associations. Detailed design of
the LAMOST Experiment for Galactic Understanding and Exploration (LEGUE)
survey will be completed in summer 2012, after a review of the results
of the pilot survey.},
  file = {/Users/Oliver/Zotero/storage/AIBT2V4M/Deng et al. - 2012 - LAMOST Experiment for Galactic Understanding and E.pdf},
  journal = {Research in Astronomy and Astrophysics}
}

@article{deridder+2009,
  title = {Non-Radial Oscillation Modes with Long Lifetimes in Giant Stars},
  author = {De Ridder, Joris and Barban, Caroline and Baudin, Fr{\'e}d{\'e}ric and Carrier, Fabien and Hatzes, Artie P. and Hekker, Saskia and Kallinger, Thomas and Weiss, Werner W. and Baglin, Annie and Auvergne, Michel and Samadi, R{\'e}za and Barge, Pierre and Deleuil, Magali},
  year = {2009},
  month = may,
  volume = {459},
  pages = {398--400},
  issn = {0028-0836},
  doi = {10.1038/nature08022},
  abstract = {Towards the end of their lives, stars like the Sun greatly expand to become red giant stars. Such evolved stars could provide stringent tests of stellar theory, as many uncertainties of the internal stellar structure accumulate with age. Important examples are convective overshooting and rotational mixing during the central hydrogen-burning phase, which determine the mass of the helium core, but which are not well understood. In principle, analysis of radial and non-radial stellar oscillations can be used to constrain the mass of the helium core. Although all giants are expected to oscillate, it has hitherto been unclear whether non-radial modes are observable at all in red giants, or whether the oscillation modes have a short or a long mode lifetime, which determines the observational precision of the frequencies. Here we report the presence of radial and non-radial oscillations in more than 300 giant stars. For at least some of the giants, the mode lifetimes are of the order of a month. We observe giant stars with equally spaced frequency peaks in the Fourier spectrum of the time series, as well as giants for which the spectrum seems to be more complex. No satisfactory theoretical explanation currently exists for our observations.},
  journal = {Nature}
}

@article{deridder+2016,
  title = {Asteroseismic versus {{Gaia}} Distances: {{A}} First Comparison},
  shorttitle = {Asteroseismic versus {{Gaia}} Distances},
  author = {De Ridder, J. and Molenberghs, G. and Eyer, L. and Aerts, C.},
  year = {2016},
  month = oct,
  volume = {595},
  pages = {L3},
  doi = {10.1051/0004-6361/201629799},
  abstract = {Context. The Kepler space mission led to a large number of high-precision time series of solar-like oscillators. Using a Bayesian analysis that combines asteroseismic techniques and additional ground-based observations, the mass, radius, luminosity, and distance of these stars can be estimated with good precision. This has given a new impetus to the research field of galactic archeology. \\
 Aims: The first data release of the Gaia space mission contains the Tycho-Gaia Astrometric Solution (TGAS) catalogue with parallax estimates for more than 2 million stars, including many of the Kepler targets. Our goal is to make a first proper comparison of asteroseismic and astrometric parallaxes of a selection of dwarfs, subgiants, and red giants observed by Kepler for which asteroseismic distances were published. \\
 Methods: We compare asteroseismic and astrometric distances of solar-like pulsators using an appropriate statistical errors-in-variables model on a linear and on a logarithmic scale. \\
 Results: For a sample of 22 dwarf and subgiant solar-like oscillators, the TGAS parallaxes considerably improved on the Hipparcos data, yet the excellent agreement between asteroseismic and astrometric distances still holds. For a sample of 938 Kepler pulsating red giants, the TGAS parallaxes are much more uncertain than the asteroseismic ones, making it worthwhile to validate the former with the latter. From errors-in-variables modelling we find a significant discrepancy between the TGAS parallaxes and the asteroseismic values. \\
 Conclusions: For the sample of dwarfs and subgiants, the comparison between astrometric and asteroseismic parallaxes does not require a revision of the stellar models on the basis of TGAS. For the sample of red giants, we identify possible causes of the discrepancy, which we will likely be able to resolve with the more precise Gaia parallaxes in the upcoming releases.},
  file = {/Users/Oliver/Zotero/storage/9XSTILXH/De Ridder et al. - 2016 - Asteroseismic versus Gaia distances A first compa.pdf;/Users/Oliver/Zotero/storage/NN6PZ77Z/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{deubner+gough1984,
  title = {Helioseismology: {{Oscillations}} as a {{Diagnostic}} of the {{Solar Interior}}},
  shorttitle = {Helioseismology},
  author = {Deubner, Franz-Ludwig and Gough, Douglas},
  year = {1984},
  volume = {22},
  pages = {593--619},
  issn = {0066-4146},
  doi = {10.1146/annurev.aa.22.090184.003113},
  abstract = {Contents: (1) Introduction. (2) Resonant cavities in the Sun. (3) Observational methods. (4) High-degree modes: Solar structure.
Subphotospheric velocities. (5) Low-degree modes: High-order p modes. Gravity modes. Solar structure. (6) Five-minute modes of intermediate degree. (7) Limb observations. (8) Problems for the immediate future. Appendix: Classification of stellar oscillations.},
  file = {/Users/Oliver/Zotero/storage/6PVFEPHK/Deubner and Gough - 1984 - Helioseismology Oscillations as a Diagnostic of t.pdf},
  journal = {Annual Review of Astronomy and Astrophysics}
}

@article{deubner1975,
  title = {Observations of Low Wavenumber Nonradial Eigenmodes of the Sun},
  author = {Deubner, F.-L.},
  year = {1975},
  month = nov,
  volume = {44},
  pages = {371--375},
  issn = {0004-6361},
  abstract = {Photoelectric observations of the photospheric velocity field with high resolution in horizontal wavenumber and frequency have been carried out in the C I 5380-A line. Three or four discrete stable modes of the five-minute oscillations are resolved in the wavenumber-frequency diagram, which agree in many respects with the predicted fundamental modes of subphotospheric standing acoustic waves. Some interesting aspects of the confirmation of a 'global' excitation mechanism of the five-minute oscillations are pointed out. Several apparently discordant details of previous observations are rediscussed, and it is shown that they can be reconciled with the present results.},
  file = {/Users/Oliver/Zotero/storage/UP6T9JKV/Deubner - 1975 - Observations of low wavenumber nonradial eigenmode.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {Astronomical Models,Photoelectric Emission,Photosphere,Solar Atmosphere,Sound Waves,Spatial Distribution,Standing Waves,Velocity Distribution}
}

@article{digennaro+2019,
  title = {Evidence for a {{Merger}}-Induced {{Shock Wave}} in {{ZwCl}} 0008.8+5215 with {{Chandra}} and {{Suzaku}}},
  author = {Di Gennaro, G. and {van Weeren}, R. J. and {Andrade-Santos}, F. and Akamatsu, H. and Randall, S. W. and Forman, W. and Kraft, R. P. and Brunetti, G. and Dawson, W. A. and Golovich, N. and Jones, C.},
  year = {2019},
  month = mar,
  volume = {873},
  pages = {64},
  doi = {10.3847/1538-4357/ab03cd},
  abstract = {We present the results from new deep Chandra ({$\sim$}410 ks) and Suzaku ({$\sim$}180 ks) observations of the merging galaxy cluster ZwCl 0008.8+5215 (z = 0.104). Previous radio observations revealed the presence of a double radio relic located diametrically west and east of the cluster center. Using our new Chandra data, we find evidence for the presence of a shock at the location of the western relic, RW, with a Mach number \{\{ \textbackslash mathcal M \}\}\textsubscript{\{S\vphantom\}}\textsubscript{X}\vphantom\{\}=\{1.48\}\textsubscript{-0.32}\textsuperscript{+0.50} from the density jump. We also measure \{\{ \textbackslash mathcal M \}\}\textsubscript{\{T\vphantom\}}\textsubscript{X}\vphantom\{\}=\{2.35\}\textsubscript{-0.55}\textsuperscript{+0.74} and \{\{ \textbackslash mathcal M \}\}\textsubscript{\{T\vphantom\}}\textsubscript{X}\vphantom\{\}=\{2.02\}\textsubscript{-0.47}\textsuperscript{+0.74} from the temperature jump, with Chandra and Suzaku, respectively. These values are consistent with the Mach number estimate from a previous study of the radio spectral index, under the assumption of diffusive shock acceleration (\{\{ \textbackslash mathcal M \}\}\textsubscript{RW}\vphantom\{\}=\{2.4\}\textsubscript{-0.2}\textsuperscript{+0.4}). Interestingly, the western radio relic does not entirely trace the X-ray shock. A possible explanation is that the relic traces fossil plasma from nearby radio galaxies that is reaccelerated at the shock. For the eastern relic we do not detect an X-ray surface brightness discontinuity, despite the fact that radio observations suggest a shock with \{\{ \textbackslash mathcal M \}\}\textsubscript{RE}\vphantom\{\}=\{2.2\}\textsubscript{-0.1}\textsuperscript{+0.2}. The low surface brightness and reduced integration time for this region might have prevented the detection. The Chandra surface brightness profile suggests \{ \textbackslash mathcal M \}{$\lessequivlnt$} 1.5, while the Suzaku temperature measurements found \{\{ \textbackslash mathcal M \}\}\textsubscript{\{T\vphantom\}}\textsubscript{X}\vphantom\{\}=\{1.54\}\textsubscript{-0.47}\textsuperscript{+0.65}. Finally, we also detect a merger-induced cold front on the western side of the cluster, behind the shock that traces the western relic.},
  file = {/Users/Oliver/Zotero/storage/NQAQCZQJ/Di Gennaro et al. - 2019 - Evidence for a Merger-induced Shock Wave in ZwCl 0.pdf;/Users/Oliver/Zotero/storage/8YACI245/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{distefano+2017,
  title = {Activity Cycles in Members of Young Loose Stellar Associations},
  author = {Distefano, E. and Lanzafame, A. C. and Lanza, A. and Messina, S. and Spada, F.},
  year = {2017},
  month = jun,
  abstract = {Magnetic cycles have been detected in tens of solar-like stars. The relationship between the cycle properties and global stellar parameters is not fully understood yet. We searched for activity cycles in 90 solar-like stars with ages between 4 and 95 Myr aiming to investigate the properties of activity cycles in this age range. We measured the length \$P\_\{ cyc\}\$ of a given cycle by analyzing the long-term time-series of three activity indexes. For each star, we computed also the global magnetic activity index  that is proportional to the amplitude of the rotational modulation and is a proxy of the mean level of the surface magnetic activity. We detected activity cycles in 67 stars. Secondary cycles were also detected in 32 stars. The lack of correlation between \$P\_\{ cyc\}\$ and \$P\_\{ rot\}\$ suggest that these stars belong to the Transitional Branch and that the dynamo acting in these stars is different from the solar one. This statement is also supported by the analysis of the butterfly diagrams. We computed the Spearman correlation coefficient \$r\_\{ S\}\$ between \$P\_\{ cyc\}\$,  and different stellar parameters. We found that \$P\_\{ cyc\}\$ is uncorrelated with all the investigated parameters. The  index is positively correlated with the convective turn-over time-scale, the magnetic diffusivity time-scale \$\textbackslash tau\_\{ diff\}\$, and the dynamo number \$D\_\{ N\}\$, whereas it is anti-correlated with the effective temperature \$T\_\{ eff\}\$, the photometric shear \$\textbackslash Delta\textbackslash Omega\_\{\textbackslash rm phot\}\$ and the radius \$R\_\{ C\}\$ at which the convective zone is located. We found that \$P\_\{ cyc\}\$ is about constant and that  decreases with the stellare age in the range 4-95 Myr. We investigated the magnetic activity of AB Dor A by merging ASAS time-series with previous long-term photometric data. We estimated the length of the AB Dor A primary cycle as \$P\_\{ cyc\} = 16.78 \textbackslash pm 2 \textbackslash rm yr\$.},
  archivePrefix = {arXiv},
  eprint = {1706.07938},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/ERNJC6NI/Distefano et al. - 2017 - Activity cycles in members of young loose stellar .pdf;/Users/Oliver/Zotero/storage/4CM8NBF9/1706.html},
  journal = {arXiv:1706.07938 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{domingo+1995,
  title = {The {{SOHO}} Mission: {{An}} Overview},
  shorttitle = {The {{SOHO}} Mission},
  author = {Domingo, V. and Fleck, B. and Poland, A. I.},
  year = {1995},
  month = dec,
  volume = {162},
  pages = {1--37},
  issn = {1573-093X},
  doi = {10.1007/BF00733425},
  abstract = {The Solar and Heliospheric Observatory (SOHO) is a space mission that forms part of the Solar-Terrestrial Science Program (STSP), developed in a collaborative effort by the European Space Agency (ESA) and the National Aeronautics and Space Administration (NASA). The STSP constitutes the first ``cornerstone'' of ESA's long-term programme known as ``Space Science \textemdash{} Horizon 2000''. The principal scientific objectives of the SOHO mission are a) to reach a better understanding of the structure and dynamics of the solar interior using techniques of helioseismology, and b) to gain better insight into the physical processes that form and heat the Sun's corona, maintain it and give rise to its acceleration into the solar wind. To achieve these goals, SOHO carries a payload consisting of 12 sets of complementary instruments. SOHO is a three-axis stabilized spacecraft with a total mass of 1850 kg; 1150 W of power will be provided by the solar panels. The payload weighs about 640 kg and will consume 450 W in orbit. SOHO will be launched by an ATLAS II-AS and will be placed in a halo orbit around the Sun-Earth L1 Lagrangian point where it will be continuously pointing to Sun centre with an accuracy of 10 arcsec. Pointing stability will be better than 1 arcsec over 15 min intervals. The SOHO payload produces a continuous science data stream of 40 kbits/s which will be increased by 160 kbits/s whenever the solar oscillations imaging instrument is operated in its highrate mode. Telemetry will be received by NASA's Deep Space Network (DSN). Planning, coordination and operation of the spacecraft and the scientific payload will be conducted from the Experiment Operations Facility (EOF) at NASA's Goddard Space Flight Center (GSFC).},
  journal = {Solar Physics},
  language = {en},
  number = {1}
}

@inproceedings{donascimentojr+2015,
  title = {A {{New Light}} on the {{Relation Between Rotation Periods}} and {{Cycle Lengths}} of {{Stellar Activity}}},
  booktitle = {18th {{Cambridge Workshop}} on {{Cool Stars}}, {{Stellar Systems}}, and the {{Sun}}},
  author = {{do Nascimento Jr}, Jos{\'e}-Dias and Saar, Steven H. and Anthony, Francys},
  year = {2015},
  volume = {18},
  pages = {59--64},
  file = {/Users/Oliver/Zotero/storage/P3NKWXZC/004-do_Nascimento_Jr.+_CS18.pdf}
}

@article{douglas+2014,
  title = {The {{Factory}} and the {{Beehive}}. {{II}}. {{Activity}} and {{Rotation}} in {{Praesepe}} and the {{Hyades}}},
  author = {Douglas, S. T. and Ag{\"u}eros, M. A. and Covey, K. R. and Bowsher, E. C. and Bochanski, J. J. and Cargile, P. A. and Kraus, A. and Law, N. M. and Lemonias, J. J. and Arce, H. G. and Fierroz, D. F. and Kundert, A.},
  year = {2014},
  month = nov,
  volume = {795},
  pages = {161},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/795/2/161},
  abstract = {Open clusters are collections of stars with a single, well-determined
age, and can be used to investigate the connections between
angular-momentum evolution and magnetic activity over a star's lifetime.
We present the results of a comparative study of the relationship
between stellar rotation and activity in two benchmark open clusters:
Praesepe and the Hyades. As they have the same age and roughly solar
metallicity, these clusters serve as an ideal laboratory for testing the
agreement between theoretical and empirical rotation-activity relations
at {$\approx$}600 Myr. We have compiled a sample of 720 spectra\textemdash more than
half of which are new observations\textemdash for 516 high-confidence members
of Praesepe; we have also obtained 139 new spectra for 130
high-confidence Hyads. We have also collected rotation periods (P
rot) for 135 Praesepe members and 87 Hyads. To compare
H{$\alpha$} emission, an indicator of chromospheric activity, as a function
of color, mass, and Rossby number Ro , we first calculate an
expanded set of {$\chi$} values, with which we can obtain the H{$\alpha$} to
bolometric luminosity ratio, L H{$\alpha$}/L bol,
even when spectra are not flux-calibrated and/or stars lack reliable
distances. Our {$\chi$} values cover a broader range of stellar masses and
colors (roughly equivalent to spectral types from K0 to M9), and exhibit
better agreement between independent calculations, than existing values.
Unlike previous authors, we find no difference between the two clusters
in their H{$\alpha$} equivalent width or L H{$\alpha$}/L
bol distributions, and therefore take the merged H{$\alpha$} and
P rot data to be representative of 600 Myr old stars. Our
analysis shows that H{$\alpha$} activity in these stars is saturated for
\{R\_o\}{$\leq$} 0.11+0.02-0.03. Above that value
activity declines as a power-law with slope {$\beta$}
=-0.73+0.16-0.12, before dropping off rapidly at
Ro {$\approx$} 0.4. These data provide a useful anchor for
calibrating the age-activity-rotation relation beyond 600 Myr.},
  file = {/Users/Oliver/Zotero/storage/LFCTH7CF/Douglas et al. - 2014 - The Factory and the Beehive. II. Activity and Rota.pdf},
  journal = {The Astrophysical Journal},
  keywords = {stars: activity,stars: chromospheres,stars: coronae,stars: evolution,stars: late-type,stars: rotation}
}

@article{douglas+2019,
  title = {K2 Rotation Periods for Low-Mass {{Hyads}} and a Quantitative Comparison of the Distribution of Slow Rotators in the {{Hyades}} and {{Praesepe}}},
  author = {Douglas, S. T. and Curtis, J. L. and Ag{\"u}eros, M. A. and Cargile, P. A. and Brewer, J. M. and Meibom, S. and Jansen, T.},
  year = {2019},
  month = may,
  abstract = {We analyze K2 light curves for 132 low-mass (\$1\textbackslash{} \textbackslash gtrsim\textbackslash{} M\_*\textbackslash{} \textbackslash gtrsim\textbackslash{} 0.1\$\textasciitilde\$\{M\_\{\textbackslash odot\}\}\$) members of the 600--800\textasciitilde Myr-old Hyades cluster and measure rotation periods (\$P\_\{rot\}\$) for 116 of these stars. These include 93 stars with no prior \$P\_\{rot\}\$ measurement; the total number of Hyads with known \$P\_\{rot\}\$ is now 232. We then combine literature binary data with Gaia DR2 photometry and astrometry to select single star sequences in the Hyades and its roughly coeval Praesepe open cluster, and derive a new reddening value of \$A\_V = 0.035\$\$\textbackslash pm\$\$0.011\$ for Praesepe. Comparing the effective temperature--\$P\_\{rot\}\$ distributions for the Hyades and Praesepe, we find that solar-type Hyads rotate, on average, 0.4\textasciitilde d slower than their Praesepe counterparts. This \$P\_\{rot\}\$ difference indicates that the Hyades is slightly older than Praesepe: we apply a new gyrochronology model tuned with Praesepe and the Sun, and find an age difference between the two clusters of 57\textasciitilde Myr. However, this \$P\_\{rot\}\$ difference decreases and eventually disappears for lower-mass stars. This provides further evidence for stalling in the rotational evolution of these stars, and highlights the need for more detailed analysis of angular-momentum evolution for stars of different masses and ages.},
  archivePrefix = {arXiv},
  eprint = {1905.06736},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/AFVMX2PB/Douglas et al. - 2019 - K2 rotation periods for low-mass Hyads and a quant.pdf;/Users/Oliver/Zotero/storage/K2VRUE63/1905.html},
  journal = {arXiv:1905.06736 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{doyle+2014,
  title = {Determining Stellar Macroturbulence Using Asteroseismic Rotational Velocities from {{Kepler}}},
  author = {Doyle, Amanda P. and Davies, Guy R. and Smalley, Barry and Chaplin, William J. and Elsworth, Yvonne},
  year = {2014},
  month = nov,
  volume = {444},
  pages = {3592--3602},
  issn = {0035-8711},
  doi = {10.1093/mnras/stu1692},
  abstract = {The Rossiter-McLaughlin effect observed for transiting exoplanets often
requires prior knowledge of the stellar projected equatorial rotational
velocity (v sin i). This is usually provided by measuring the broadening
of spectral lines, however this method has uncertainties as lines are
also broadened by velocity fields in the stellar photosphere known as
macroturbulence (vmac). We have estimated accurate v sin i
values from asteroseismic analyses of main-sequence stars observed by
Kepler. The rotational frequency splittings of the detected solar-like
oscillations of these stars are determined largely by the near-surface
rotation. These estimates have been used to infer the vmac
values for 28 Kepler stars. Out of this sample, 26 stars were used along
with the Sun to obtain a new calibration between vmac,
effective temperature and surface gravity. The new calibration is valid
for the temperature range 5200 to 6400 K and the gravity range 4.0 to
4.6 dex. A comparison is also provided with previous vmac
calibrations. As a result of this work, vmac, and thus v sin
i, can now be determined with confidence for stars that do not have
asteroseismic data available. We present new spectroscopic v sin i
values for the WASP planet host stars, using high-resolution HARPS
spectra.},
  file = {/Users/Oliver/Zotero/storage/PY94K7CJ/Doyle et al. - 2014 - Determining stellar macroturbulence using asterose.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,line: profiles,planets and satellites: fundamental parameters,stars: rotation}
}

@article{dressing+2017,
  title = {Characterizing {{K2 Candidate Planetary Systems Orbiting Low}}-{{Mass Stars I}}: {{Classifying Low}}-Mass {{Host Stars Observed During Campaigns}} 1-7},
  shorttitle = {Characterizing {{K2 Candidate Planetary Systems Orbiting Low}}-{{Mass Stars I}}},
  author = {Dressing, Courtney D. and Newton, Elisabeth R. and Schlieder, Joshua E. and Charbonneau, David and Knutson, Heather A. and Vanderburg, Andrew},
  year = {2017},
  month = jan,
  abstract = {We present near-infrared spectra for 144 candidate planetary systems identified during Campaigns 1-7 of the NASA K2 Mission. The goal of the survey was to characterize planets orbiting low-mass stars, but our IRTF/SpeX and Palomar/TripleSpec spectroscopic observations revealed that 49\% of our targets were actually giant stars or hotter dwarfs reddened by interstellar extinction. For the 72 stars with spectra consistent with classification as cool dwarfs (spectral types K3 - M4), we refined their stellar properties by applying empirical relations based on stars with interferometric radius measurements. Although our revised temperatures are generally consistent with those reported in the Ecliptic Plane Input Catalog (EPIC), our revised stellar radii are typically 0.13 solar radii (39\%) larger than the EPIC values, which were based on model isochrones that have been shown to underestimate the radii of cool dwarfs. Our improved stellar characterizations will enable more efficient prioritization of K2 targets for follow-up studies.},
  archivePrefix = {arXiv},
  eprint = {1701.00586},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/6ZS9VJMK/1701.00586v1.pdf;/Users/Oliver/Zotero/storage/SXW5F2SB/1701.html},
  journal = {arXiv:1701.00586 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{duez+2010,
  title = {On the {{Stability}} of {{Non}}-Force-Free {{Magnetic Equilibria}} in {{Stars}}},
  author = {Duez, V. and Braithwaite, J. and Mathis, S.},
  year = {2010},
  month = nov,
  volume = {724},
  pages = {L34-L38},
  issn = {0004-637X},
  doi = {10.1088/2041-8205/724/1/L34},
  abstract = {The existence of stable magnetic configurations in white dwarfs, neutron stars, and various non-convective stellar regions is now well
recognized. It has recently been shown numerically that various families of equilibria, including axisymmetric mixed poloidal-toroidal
configurations, are stable. Here we test the stability of an
analytically derived non-force-free magnetic equilibrium resulting from an initial relaxation (self-organization) process, using
three-dimensional magnetohydrodynamic simulations: the obtained mixed configuration is compared with the dynamical evolution of its purely poloidal and purely toroidal components, both known to be unstable. The mixed equilibrium shows no sign of instability under white noise perturbations. This configuration therefore provides a good description of magnetic equilibrium topology inside non-convective stellar objects and will be useful to initialize magneto-rotational transport in stellar evolution codes and in multi-dimensional magnetohydrodynamic
simulations.},
  file = {/Users/Oliver/Zotero/storage/57T3UG85/Duez et al. - 2010 - On the Stability of Non-force-free Magnetic Equili.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {magnetohydrodynamics: MHD,stars: interiors,stars: magnetic field,stars: neutron,Sun: magnetic topology,white dwarfs}
}

@article{duvall+1993,
  title = {Time-Distance Helioseismology},
  author = {Duvall, Jr., T. L. and Jefferies, S. M. and Harvey, J. W. and Pomerantz, M. A.},
  year = {1993},
  month = apr,
  volume = {362},
  pages = {430--432},
  issn = {0028-0836},
  doi = {10.1038/362430a0},
  abstract = {It is shown here that it is possible to extract time-distance information from temporal cross-correlations of the intensity
fluctuation on the solar surface. This approach opens the way for seismic studies of local solar phenomena such subsurface inhomogeneities near sunspots and should help to refine global models of the internal velocity stratification in the sun.},
  file = {/Users/Oliver/Zotero/storage/F77AG88R/Duvall et al. - 1993 - Time-distance helioseismology.pdf},
  journal = {Nature},
  keywords = {Cross Correlation,Distance,Helioseismology,Solar Interior,Solar Oscillations,Time Measurement,Vibration Mode}
}

@article{eff-darwich+2008,
  title = {Analysis of the {{Sensitivity}} of {{Solar Rotation}} to {{Helioseismic Data}} from {{GONG}}, {{GOLF}}, and {{MDI Observations}}},
  author = {{Eff-Darwich}, A. and Korzennik, S. G. and {Jim{\'e}nez-Reyes}, S. J. and Garc{\'i}a, R. A.},
  year = {2008},
  month = jun,
  volume = {679},
  pages = {1636--1643},
  issn = {0004-637X},
  doi = {10.1086/586724},
  abstract = {Accurate determination of the rotation rate in the radiative zone of the
Sun from helioseismic observations requires rotational frequency
splittings of exceptional quality as well as reliable inversion
techniques. Here we present inferences based on mode parameters
calculated from 2088 day MDI, GONG, and GOLF time series that were
fitted to estimate very low frequency rotational splittings ({$\nu$} {$<$}
1.7 mHz). These low-frequency modes provide data of exceptional quality,
since the width of the mode peaks is much smaller than the rotational
splitting, and hence it is much easier to separate the rotational
splittings from the effects caused by the finite lifetime and the
stochastic excitation of the modes. We have also implemented a new
inversion methodology that allows us to infer the rotation rate of the
radiative interior from mode sets that span l = 1 to 25. Our results are
compatible with the Sun rotating like a rigid solid in most of the
radiative zone, and slowing down in the core (r/R{$\odot$} {$<$}
0.2). A resolution analysis of the inversion was carried out for the
solar rotation inverse problem. This analysis effectively establishes a
direct relationship between the mode set included in the inversion and
the sensitivity and information content of the resulting inferences. We
show that such an approach allows us to determine the effect of adding
low-frequency and low-degree p-modes, high-frequency and low-degree
p-modes, and some g-modes on the derived rotation rate in the solar
radiative zone, and in particular the solar core. We conclude that the
level of uncertainty that is needed to infer the dynamical conditions in
the core when only p-modes are included is unlikely to be reached in the
near future, and hence sustained efforts are needed toward the detection
and characterization of g-modes.},
  file = {/Users/Oliver/Zotero/storage/TU6EMZW8/Eff-Darwich et al. - 2008 - Analysis of the Sensitivity of Solar Rotation to H.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Sun: interior,Sun: rotation}
}

@article{eggenberger+2010,
  title = {Effects of Rotation and Magnetic Fields on the Lithium Abundance and Asteroseismic Properties of Exoplanet-Host Stars},
  author = {Eggenberger, P. and Maeder, A. and Meynet, G.},
  year = {2010},
  month = sep,
  volume = {519},
  pages = {L2},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201014939},
  abstract = {Context. Recent spectroscopic observations indicate lower lithium
abundances of exoplanet-host stars compared to solar-type stars without
detected exoplanets. Moreover, studies based on the distribution of
rotational periods of solar-type stars suggest a possible link between
lithium depletion and the rotational history of exoplanet-host stars.
 Aims: The effects of rotation and magnetic fields on the surface
abundances of solar-type stars are studied in order to investigate
whether the reported difference in lithium content of exoplanet-host
stars can be related to their rotational history. Moreover, the
asteroseismic properties predicted for stars with and without exoplanets
are compared to determine how such a scenario, which relates the lithium
abundances and the rotational history of the star, can be further
challenged by observations of solar-like oscillations. Methods:
Based on observations of rotational periods of solar-type stars, slow
rotators on the zero age main sequence (ZAMS) are modelled with a
comprehensive treatment of only the shellular rotation, while fast
rotators are modelled including both shellular rotation and magnetic
fields. Assuming a possible link between low rotation rates on the ZAMS
and the presence of planets as a result of a longer disc-locking phase
during the pre-main sequence (PMS), we compare the surface abundances
and asteroseismic properties of slow and fast rotating models, which
correspond to exoplanet-host stars and stars without detected planets,
respectively. Results: We confirm previous suggestions that the
difference in the lithium content of stars with and without detected
planets can be related to their different rotational history. The larger
efficiency of rotational mixing predicted in exoplanet-host stars
explains their lithium depletion and also leads to changes in the
structure and chemical composition of the central stellar layers.
Asteroseismic observations can reveal these changes and can help us
distinguish between different possible explanations for the lower
lithium content of exoplanet-host stars.},
  file = {/Users/Oliver/Zotero/storage/2RJA5W96/Eggenberger et al. - 2010 - Effects of rotation and magnetic fields on the lit.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {stars: abundances,stars: magnetic field,stars: oscillations,stars: rotation,stars: solar-type}
}

@article{eggenberger+2010a,
  title = {Effects of Rotational Mixing on the Asteroseismic Properties of Solar-Type Stars},
  author = {Eggenberger, P. and Meynet, G. and Maeder, A. and Miglio, A. and Montalban, J. and Carrier, F. and Mathis, S. and Charbonnel, C. and Talon, S.},
  year = {2010},
  month = sep,
  volume = {519},
  pages = {A116},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201014713},
  abstract = {Context. Observations of solar-like oscillations obtained either from
the ground or from space stimulated the study of the effects of various
physical processes on the modelling of solar-type stars. Aims:
The influence of rotational mixing on the evolution and asteroseismic
properties of solar-type stars is studied. Methods: Global and
asteroseismic properties of models of solar-type stars computed with and
without a comprehensive treatment of shellular rotation are compared.
The effects of internal magnetic fields are also discussed in the
framework of the Tayler-Spruit dynamo. Results: Rotational mixing
changes the global properties of a solar-type star with a significant
increase of the effective temperature resulting in a shift of the
evolutionary track to the blue part of the HR diagram. These differences
observed in the HR diagram are related to changes of the chemical
composition, because rotational mixing counteracts the effects of atomic
diffusion leading to larger helium surface abundances for rotating
models than for non-rotating ones. Higher values of the large frequency
separation are then found for rotating models than for non-rotating ones
at the same evolutionary stage, because the increase of the effective
temperature leads to a smaller radius and hence to an increase of the
stellar mean density. In addition to changing the global properties of
solar-type stars, rotational mixing also has a considerable impact on
the structure and chemical composition of the central stellar layers by
bringing fresh hydrogen fuel to the central stellar core, thereby
enhancing the main-sequence lifetime. The increase of the central
hydrogen abundance together with the change of the chemical profiles in
the central layers result in a significant increase of the values of the
small frequency separations and of the ratio of the small to large
separations for models including shellular rotation. This increase is
clearly seen for models with the same age sharing the same initial
parameters except for the inclusion of rotation as well as for models
with the same global stellar parameters and in particular the same
location in the HR diagram. By computing rotating models of solar-type
stars including the effects of a dynamo that possibly occurs in the
radiative zone, we find that the efficiency of rotational mixing is
strongly reduced when the effects of magnetic fields are taken into
account, in contrast to what happens in massive stars.},
  file = {/Users/Oliver/Zotero/storage/UIWKBMP7/Eggenberger et al. - 2010 - Effects of rotational mixing on the asteroseismic .pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {stars: interiors,stars: magnetic field,stars: oscillations,stars: rotation,stars: solar-type}
}

@article{eggenberger+2010b,
  title = {Effects of Rotation on the Evolution and Asteroseismic Properties of Red Giants},
  author = {Eggenberger, P. and Miglio, A. and Montalban, J. and Moreira, O. and Noels, A. and Meynet, G. and Maeder, A.},
  year = {2010},
  month = jan,
  volume = {509},
  pages = {A72},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/200912897},
  abstract = {Context. The recent observations of solar-like oscillations in many red giant stars with the CoRoT satellite stimulated the theoretical study of the effects of various physical processes on the modelling of these stars. Aims: The influence of rotation on the properties of red giants is studied in the context of the asteroseismic modelling of these stars. Methods: The effects of rotation on the global and asteroseismic properties of red giant stars with a mass larger than the mass limit for degenerate He burning are investigated by comparing rotating models computed with a comprehensive treatment of shellular rotation to non-rotating ones. Results: While red giants exhibit low surface rotational velocities, we find that the rotational history of the star has a large impact on its properties during the red giant phase. In particular, for stars massive enough to ignite He burning in non-degenerate conditions, rotational mixing induces a significant increase of the stellar luminosity and shifts the location of the core helium burning phase to a higher luminosity in the HR diagram. This of course results in a change of the seismic properties of red giants at the same evolutionary state. As a consequence the inclusion of rotation significantly changes the fundamental parameters of a red giant star as determined by performing an asteroseismic calibration. In particular rotation decreases the derived stellar mass and increases the age. Depending on the rotation law assumed in the convective envelope and on the initial velocity of the star, non-negligible values of rotational splitting can be reached, which may complicate the observation and identification of non-radial oscillation modes for red giants exhibiting moderate surface rotational velocities. By comparing the effects of rotation and overshooting, we find that the main-sequence widening and the increase of the H-burning lifetime induced by rotation
(Vini) = 150 km s-1) are well reproduced by non-rotating models with an overshooting parameter of 0.1, while the increase of luminosity during the post-main sequence evolution is better reproduced by non-rotating models with overshooting parameters twice as large. This illustrates the fact that rotation not only increases the size of the convective core but also changes the chemical composition of the radiative zone.},
  file = {/Users/Oliver/Zotero/storage/E4FXA7MS/Eggenberger et al. - 2010 - Effects of rotation on the evolution and asterosei.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {stars: fundamental parameters,stars: oscillations,stars: rotation}
}

@article{eggenberger+2013,
  title = {Effects of {{Rotation}} on {{Stellar Evolution}}},
  author = {Eggenberger, P. and Charbonnel, C. and Ekstr{\"o}m, S. and Georgy, C. and Haemmerl{\'e}, L. and Lagarde, N. and Maeder, A. and Meynet, G. and Miglio, A. and Montalban, J.},
  year = {2013},
  month = jul,
  pages = {7},
  abstract = {Not Available},
  file = {/Users/Oliver/Zotero/storage/UKP3QKJS/Eggenberger et al. - 2013 - Effects of Rotation on Stellar Evolution.pdf}
}

@article{eggenberger+2016,
  title = {Constraining the Efficiency of Angular Momentum Transport with Asteroseismology of Red Giants: The Effect of Stellar Mass},
  shorttitle = {Constraining the Efficiency of Angular Momentum Transport with Asteroseismology of Red Giants},
  author = {Eggenberger, P. and Lagarde, N. and Miglio, A. and Montalb{\'a}n, J. and Ekstr{\"o}m, S. and Georgy, C. and Meynet, G. and Salmon, S. and Ceillier, T. and Garc{\'i}a, R. A. and Mathis, S. and Deheuvels, S. and Maeder, A. and den Hartogh, J. W. and Hirschi, R.},
  year = {2016},
  month = dec,
  abstract = {Context: Constraints on the internal rotation of red giants are now available thanks to asteroseismic observations. Preliminary comparisons with rotating stellar models indicate that an undetermined additional process for the internal transport of angular momentum is required in addition to purely hydrodynamic processes. Aims: We investigate how asteroseismic measurements of red giants can help us characterize the additional transport mechanism. Methods: We first determine the efficiency of the missing transport mechanism for the low-mass red giant KIC 7341231 by computing rotating models that include an additional viscosity corresponding to this process. We then discuss the change in the efficiency of this transport of angular momentum with the mass, metallicity and evolutionary stage. Results: In the case of the low-mass red giant KIC 7341231, we find that the viscosity corresponding to the additional mechanism is constrained to the range 1 x 10\^3 - 1.3 x 10\^4 cm\^2/s. This constraint on the efficiency of the unknown additional transport mechanism during the post-main sequence is obtained independently of any specific assumption about the modelling of rotational effects during the pre-main sequence and the main sequence (in particular, the braking of the surface by magnetized winds and the efficiency of the internal transport of angular momentum before the post-main-sequence phase). When we assume that the additional transport mechanism is at work during the whole evolution of the star together with a solar-calibrated braking of the surface by magnetized winds, the range of nu\_add is reduced to 1 - 4 x 10\^3 cm\^2/s. In addition to being sensitive to the evolutionary stage of the star, we show that the efficiency of the unknown process for internal transport of angular momentum increases with the stellar mass.},
  archivePrefix = {arXiv},
  eprint = {1612.04258},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/BMX6AUZ9/Eggenberger et al. - 2016 - Constraining the efficiency of angular momentum tr.pdf;/Users/Oliver/Zotero/storage/QP9TGU9P/1612.html},
  journal = {arXiv:1612.04258 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{eisenstein+2011,
  title = {{{SDSS}}-{{III}}: {{Massive Spectroscopic Surveys}} of the {{Distant Universe}}, the {{Milky Way}}, and {{Extra}}-{{Solar Planetary Systems}}},
  shorttitle = {{{SDSS}}-{{III}}},
  author = {Eisenstein, Daniel J. and Weinberg, David H. and Agol, Eric and Aihara, Hiroaki and Allende Prieto, Carlos and Anderson, Scott F. and Arns, James A. and Aubourg, {\'E}ric and Bailey, Stephen and Balbinot, Eduardo and Barkhouser, Robert and Beers, Timothy C. and Berlind, Andreas A. and Bickerton, Steven J. and Bizyaev, Dmitry and Blanton, Michael R. and Bochanski, John J. and Bolton, Adam S. and Bosman, Casey T. and Bovy, Jo and Brandt, W. N. and Breslauer, Ben and Brewington, Howard J. and Brinkmann, J. and Brown, Peter J. and Brownstein, Joel R. and Burger, Dan and Busca, Nicolas G. and Campbell, Heather and Cargile, Phillip A. and Carithers, William C. and Carlberg, Joleen K. and Carr, Michael A. and Chang, Liang and Chen, Yanmei and Chiappini, Cristina and Comparat, Johan and Connolly, Natalia and Cortes, Marina and Croft, Rupert A. C. and Cunha, Katia and {da Costa}, Luiz N. and Davenport, James R. A. and Dawson, Kyle and De Lee, Nathan and {Porto de Mello}, Gustavo F. and {de Simoni}, Fernando and Dean, Janice and Dhital, Saurav and Ealet, Anne and Ebelke, Garrett L. and Edmondson, Edward M. and Eiting, Jacob M. and Escoffier, Stephanie and Esposito, Massimiliano and Evans, Michael L. and Fan, Xiaohui and Femen{\'i}a Castell{\'a}, Bruno and Dutra Ferreira, Leticia and Fitzgerald, Greg and Fleming, Scott W. and {Font-Ribera}, Andreu and Ford, Eric B. and Frinchaboy, Peter M. and Garc{\'i}a P{\'e}rez, Ana Elia and Gaudi, B. Scott and Ge, Jian and Ghezzi, Luan and Gillespie, Bruce A. and Gilmore, G. and Girardi, L{\'e}o and Gott, J. Richard and Gould, Andrew and Grebel, Eva K. and Gunn, James E. and Hamilton, Jean-Christophe and Harding, Paul and Harris, David W. and Hawley, Suzanne L. and Hearty, Frederick R. and Hennawi, Joseph F. and Gonz{\'a}lez Hern{\'a}ndez, Jonay I. and Ho, Shirley and Hogg, David W. and Holtzman, Jon A. and Honscheid, Klaus and Inada, Naohisa and Ivans, Inese I. and Jiang, Linhua and Jiang, Peng and Johnson, Jennifer A. and Jordan, Cathy and Jordan, Wendell P. and Kauffmann, Guinevere and Kazin, Eyal and Kirkby, David and Klaene, Mark A. and Knapp, G. R. and Kneib, Jean-Paul and Kochanek, C. S. and Koesterke, Lars and Kollmeier, Juna A. and Kron, Richard G. and Lampeitl, Hubert and Lang, Dustin and Lawler, James E. and Le Goff, Jean-Marc and Lee, Brian L. and Lee, Young Sun and Leisenring, Jarron M. and Lin, Yen-Ting and Liu, Jian and Long, Daniel C. and Loomis, Craig P. and Lucatello, Sara and Lundgren, Britt and Lupton, Robert H. and Ma, Bo and Ma, Zhibo and MacDonald, Nicholas and Mack, Claude and Mahadevan, Suvrath and Maia, Marcio A. G. and Majewski, Steven R. and Makler, Martin and Malanushenko, Elena and Malanushenko, Viktor and Mandelbaum, Rachel and Maraston, Claudia and Margala, Daniel and Maseman, Paul and Masters, Karen L. and McBride, Cameron K. and McDonald, Patrick and McGreer, Ian D. and McMahon, Richard G. and Mena Requejo, Olga and M{\'e}nard, Brice and {Miralda-Escud{\'e}}, Jordi and Morrison, Heather L. and Mullally, Fergal and Muna, Demitri and Murayama, Hitoshi and Myers, Adam D. and Naugle, Tracy and Neto, Angelo Fausti and Nguyen, Duy Cuong and Nichol, Robert C. and Nidever, David L. and O'Connell, Robert W. and Ogando, Ricardo L. C. and Olmstead, Matthew D. and Oravetz, Daniel J. and Padmanabhan, Nikhil and Paegert, Martin and {Palanque-Delabrouille}, Nathalie and Pan, Kaike and Pandey, Parul and Parejko, John K. and P{\^a}ris, Isabelle and Pellegrini, Paulo and Pepper, Joshua and Percival, Will J. and Petitjean, Patrick and Pfaffenberger, Robert and Pforr, Janine and Phleps, Stefanie and Pichon, Christophe and Pieri, Matthew M. and Prada, Francisco and {Price-Whelan}, Adrian M. and Raddick, M. Jordan and Ramos, Beatriz H. F. and Reid, I. Neill and Reyle, Celine and Rich, James and Richards, Gordon T. and Rieke, George H. and Rieke, Marcia J. and Rix, Hans-Walter and Robin, Annie C. and {Rocha-Pinto}, Helio J. and Rockosi, Constance M. and Roe, Natalie A. and Rollinde, Emmanuel and Ross, Ashley J. and Ross, Nicholas P. and Rossetto, Bruno and S{\'a}nchez, Ariel G. and Santiago, Basilio and Sayres, Conor and Schiavon, Ricardo and Schlegel, David J. and Schlesinger, Katharine J. and Schmidt, Sarah J. and Schneider, Donald P. and Sellgren, Kris and Shelden, Alaina and Sheldon, Erin and Shetrone, Matthew and Shu, Yiping and Silverman, John D. and Simmerer, Jennifer and Simmons, Audrey E. and Sivarani, Thirupathi and Skrutskie, M. F. and Slosar, An{\v z}e and Smee, Stephen and Smith, Verne V. and Snedden, Stephanie A. and Stassun, Keivan G. and Steele, Oliver and Steinmetz, Matthias and Stockett, Mark H. and Stollberg, Todd and Strauss, Michael A. and Szalay, Alexander S. and Tanaka, Masayuki and Thakar, Aniruddha R. and Thomas, Daniel and Tinker, Jeremy L. and Tofflemire, Benjamin M. and Tojeiro, Rita and Tremonti, Christy A. and Vargas Maga{\~n}a, Mariana and Verde, Licia and Vogt, Nicole P. and Wake, David A. and Wan, Xiaoke and Wang, Ji and Weaver, Benjamin A. and White, Martin and White, Simon D. M. and Wilson, John C. and Wisniewski, John P. and {Wood-Vasey}, W. Michael and Yanny, Brian and Yasuda, Naoki and Y{\`e}che, Christophe and York, Donald G. and Young, Erick and Zasowski, Gail and Zehavi, Idit and Zhao, Bo},
  year = {2011},
  month = sep,
  volume = {142},
  pages = {72},
  issn = {0004-6256},
  doi = {10.1088/0004-6256/142/3/72},
  abstract = {Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II),
SDSS-III is a program of four spectroscopic surveys on three scientific
themes: dark energy and cosmological parameters, the history and
structure of the Milky Way, and the population of giant planets around
other stars. In keeping with SDSS tradition, SDSS-III will provide
regular public releases of all its data, beginning with SDSS Data
Release 8 (DR8), which was made public in 2011 January and includes
SDSS-I and SDSS-II images and spectra reprocessed with the latest
pipelines and calibrations produced for the SDSS-III investigations.
This paper presents an overview of the four surveys that comprise
SDSS-III. The Baryon Oscillation Spectroscopic Survey will measure
redshifts of 1.5 million massive galaxies and Ly{$\alpha$} forest spectra
of 150,000 quasars, using the baryon acoustic oscillation feature of
large-scale structure to obtain percent-level determinations of the
distance scale and Hubble expansion rate at z {$<$} 0.7 and at z {$\approx$}
2.5. SEGUE-2, an already completed SDSS-III survey that is the
continuation of the SDSS-II Sloan Extension for Galactic Understanding
and Exploration (SEGUE), measured medium-resolution (R =
{$\lambda$}/{$\Delta\lambda$} {$\approx$} 1800) optical spectra of 118,000 stars in
a variety of target categories, probing chemical evolution, stellar
kinematics and substructure, and the mass profile of the dark matter
halo from the solar neighborhood to distances of 100 kpc. APOGEE, the
Apache Point Observatory Galactic Evolution Experiment, will obtain
high-resolution (R {$\approx$} 30,000), high signal-to-noise ratio (S/N {$>$}=
100 per resolution element), H-band (1.51 {$\mu$}m {$<$} {$\lambda$} {$<$} 1.70
{$\mu$}m) spectra of 105 evolved,

license: MIT

license_type: permissive

branch_name: refs/heads/master

extension: bib