A uniform asteroseismic analysis of 22 solar-type stars observed by Kepler
Savita Mathur,Travis S. Metcalfe,M. Woitaszek,Hans Bruntt,Graham A. Verner,Jørgen Christensen-Dalsgaard,Jørgen Christensen-Dalsgaard,O. L. Creevey,G. Doğan,G. Doğan,Sarbani Basu,Christoffer Karoff,Christoffer Karoff,Dennis Stello,T. Appourchaux,Tiago L. Campante,Tiago L. Campante,William J. Chaplin,Rafael A. García,Timothy R. Bedding,Othman Benomar,Alfio Bonanno,S. Deheuvels,Y. P. Elsworth,Patrick Gaulme,Joyce A. Guzik,Rasmus Handberg,Saskia Hekker,Saskia Hekker,W. Herzberg,Mário J. P. F. G. Monteiro,L. Piau,P.-O. Quirion,C. Régulo,C. Régulo,Markus Roth,David Salabert,Aldo Serenelli,Michael Thompson,Regner Trampedach,Timothy R. White,J. Ballot,I. M. Brandão,J. Molenda-Zakowicz,Hans Kjeldsen,Joseph D. Twicken,Kamal Uddin,Bill Wohler +47 more
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TLDR
In this paper, the authors performed a uniform analysis of 22 stars with the highest signal-to-noise ratio observed for 1 month each during the first year of the Kepler space telescope and quantified the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass and age that are possible using various methods.Abstract:
Asteroseismology with the Kepler space telescope is providing not only an improved characterization of exoplanets and their host stars, but also a new window on stellar structure and evolution for the large sample of solar-type stars in the field. We perform a uniform analysis of 22 of the brightest asteroseismic targets with the highest signal-to-noise ratio observed for 1 month each during the first year of the mission, and we quantify the precision and relative accuracy of asteroseismic determinations of the stellar radius, mass, and age that are possible using various methods. We present the properties of each star in the sample derived from an automated analysis of the individual oscillation frequencies and other observational constraints using the Asteroseismic Modeling Portal (AMP), and we compare them to the results of model-grid-based methods that fit the global oscillation properties. We find that fitting the individual frequencies typically yields asteroseismic radii and masses to ~1% precision, and ages to ~2.5% precision (respectively, 2, 5, and 8 times better than fitting the global oscillation properties). The absolute level of agreement between the results from different approaches is also encouraging, with model-grid-based methods yielding slightly smaller estimates of the radius and mass and slightly older values for the stellar age relative to AMP, which computes a large number of dedicated models for each star. The sample of targets for which this type of analysis is possible will grow as longer data sets are obtained during the remainder of the mission.read more
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Journal ArticleDOI
Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars
Bill Paxton,Matteo Cantiello,Phil Arras,Lars Bildsten,Edward F. Brown,Aaron Dotter,Christopher R. Mankovich,Michael H. Montgomery,Dennis Stello,Francis Timmes,Richard H. D. Townsend +10 more
TL;DR: Modules for Experiments in Stellar Astrophysics (MESA) as discussed by the authors is an open source software package for modeling the evolution of stellar structures and composition. But it is not suitable for large-scale systems such as supernovae.
Journal ArticleDOI
The PLATO 2.0 mission
Heike Rauer,Heike Rauer,C. Catala,Conny Aerts,Thierry Appourchaux,Willy Benz,Alexis Brandeker,Jørgen Christensen-Dalsgaard,Magali Deleuil,Laurent Gizon,Laurent Gizon,M. J. Goupil,Manuel Güdel,Eduardo Janot-Pacheco,M. Mas-Hesse,Isabella Pagano,Giampaolo Piotto,Don Pollacco,Ċ. Santos,Andrew Smith,Juan Carlos Suárez,Róbert Szabó,Stéphane Udry,V. Adibekyan,Yann Alibert,J. M. Almenara,Pau Amaro-Seoane,M. Ammler-von Eiff,Martin Asplund,E. Antonello,Sydney A. Barnes,Frédéric Baudin,K. Belkacem,Maria Bergemann,G. Bihain,Aaron C. Birch,Xavier Bonfils,Isabelle Boisse,Aldo S. Bonomo,Francesco Borsa,I. M. Brandão,Enzo Brocato,S. Brun,Matthew R. Burleigh,R. Burston,Juan Cabrera,Santi Cassisi,William J. Chaplin,Stéphane Charpinet,Cristina Chiappini,Ross P. Church,Sz. Csizmadia,Margarida S. Cunha,Mario Damasso,Mario Damasso,Melvyn B. Davies,Hans J. Deeg,Rodrigo F. Díaz,Stefan Dreizler,C. Dreyer,C. Dreyer,P. Eggenberger,David Ehrenreich,Philipp Eigmüller,Anders Erikson,Robert Farmer,Sofia Feltzing,F. De Oliveira Fialho,Pedro Figueira,T. Forveille,Malcolm Fridlund,Rafael A. García,Paolo Giommi,G. Giuffrida,G. Giuffrida,M. Godolt,J. Gomes da Silva,T. Granzer,John Lee Grenfell,A. Grotsch-Noels,E. Günther,Carole A. Haswell,A. P. Hatzes,Guillaume Hébrard,Saskia Hekker,Saskia Hekker,Ravit Helled,Kevin Heng,Jon M. Jenkins,Anders Johansen,Maxim L. Khodachenko,Kristina G. Kislyakova,Wilhelm Kley,Ulrich Kolb,Natalie A. Krivova,Friedrich Kupka,Helmut Lammer,Antonino F. Lanza,Yveline Lebreton,Demetrio Magrin,P. Marcos-Arenal,P. M. Marrese,P. M. Marrese,J. P. Marques,J. H. C. Martins,S. Mathis,Savita Mathur,S. Messina,Andrea Miglio,Josefina Montalbán,M. Montalto,Mário J. P. F. G. Monteiro,Hamed Moradi,Ehsan Moravveji,Christoph Mordasini,Thierry Morel,Annelies Mortier,Valerio Nascimbeni,Richard P. Nelson,Martin Bo Nielsen,Lena Noack,Andrew Norton,Aviv Ofir,Mahmoudreza Oshagh,R.-M. Ouazzani,Péter Pápics,V. C. Parro,Pascal Petit,Bertrand Plez,Ennio Poretti,Andreas Quirrenbach,Roberto Ragazzoni,Giuliano Raimondo,Monica Rainer,Daniel R. Reese,Ronald Redmer,Sabine Reffert,Bárbara Rojas-Ayala,Ian W. Roxburgh,Stéphanie Salmon,Alexandre Santerne,Jean Schneider,Jesper Schou,Sonja Schuh,Hannah Schunker,A. Silva-Valio,Roberto Silvotti,I. Skillen,Ignas Snellen,Frank Sohl,S. G. Sousa,Alessandro Sozzetti,Dennis Stello,Klaus G. Strassmeier,Michal Švanda,Gy. M. Szabó,Gy. M. Szabó,Andrew Tkachenko,Diana Valencia,Valérie Van Grootel,Sylvie Vauclair,Paolo Ventura,F. W. Wagner,N. A. Walton,Joerg Weingrill,Stephanie C. Werner,Peter J. Wheatley,Konstanze Zwintz +167 more
TL;DR: The PLATO 2.0 mission as discussed by the authors has been selected for ESA's M3 launch opportunity (2022/24) to provide accurate key planet parameters (radius, mass, density and age) in statistical numbers.
Journal Article
Low Temperature Rosseland Opacities.
TL;DR: In this paper, a new set of low-temperature opacity data has been assembled, and from this basic data set, Rosseland and Planck mean opacities have been computed for temperatures between 12,500 and 700 K. In addition to the usual continuous absorbers, atomic line absorption, molecular line absorption and grain absorption and scattering (by silicates, iron, carbon, and SiC) have been accounted for.
Journal ArticleDOI
Revised Stellar Properties of Kepler Targets for the Quarter 1-16 Transit Detection Run
Daniel Huber,Daniel Huber,Victor Silva Aguirre,Jaymie M. Matthews,Marc H. Pinsonneault,Eric Gaidos,Rafael A. García,Saskia Hekker,Saskia Hekker,Savita Mathur,Benoit Mosser,Guillermo Torres,Fabienne A. Bastien,Sarbani Basu,Timothy R. Bedding,Timothy R. Bedding,William J. Chaplin,William J. Chaplin,Brice-Olivier Demory,Scott W. Fleming,Zhao Guo,Andrew W. Mann,Jason F. Rowe,Jason F. Rowe,Aldo Serenelli,Myron A. Smith,Dennis Stello,Dennis Stello +27 more
TL;DR: In this paper, the authors presented revised properties for 196,468 stars observed by the NASA Kepler mission and used in the analysis of Quarter 1-16 (Q1-Q16) data to detect and characterize transiting planets.
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TL;DR: The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars, which is the region where planetary temperatures are suitable for water to exist on a planet's surface.
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