Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler Mission

Chaplin, W. J.; Kjeldsen, H.; Christensen‐Dalsgaard, J.; Basu, Sarbani; Miglio, A.; Appourchaux, T.; Bedding, Timothy R.; Elsworth, Y.; García, R. A.; Gilliland, Ronald L.; Girardi, L.; Houdek, G.; Karoff, C.; Kawaler, S. D.; Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Verner, G. A.; Ballot, J.; Bonanno, A.; Brandão, I. M.; Broomhall, Anne-Marie; Bruntt, H.; Campante, Tiago L.; Corsaro, E.; Creevey, O.; Doğan, G.; Esch, Lisa; Gai, Ning; Gaulme, P.; Hale, Steven J.; Handberg, R.; Hekker, S.; Huber, Daniel; Jiménez, A.; Mathur, S.; Mazumdar, A.; Mosser, B.; New, R.; Pinsonneault, Marc H.; Pricopi, D.; Quirion, Pierre-Olivier; Régulo, C.; Salabert, D.; Serenelli, Aldo; Aguirre, V. Silva; Sousa, S. G.; Stello, Dennis; Stevens, I. R.; Suran, M. D.; Uytterhoeven, K.; White, T. R.; Borucki, W. J.; Brown, Timothy M.; Jenkins, Jon M.; Kinemuchi, Karen; Cleve, J. Van; Klaus, Todd C.

doi:10.1126/science.1201827

Cited by 285 publications

(244 citation statements)

References 32 publications

Supporting

Mentioning

237

Contrasting

Unclassified

Order By: Relevance

“…The detection of extra-solar planets using the transit method boosted their numbers from dozens to nearly 5000 (Batalha et al 2013;Burke et al 2014;Rowe et al 2014), and the number is growing still as data are being mined. At the same time, asteroseismology witnessed an explosion in novel techniques and exciting new results (Chaplin et al 2011), ranging from main sequence B stars (Papics 2013) to solar-like oscillations in red giants (Gaulme et al 2013). The overlap between the fields is provided by using asteroseismic techniques that provide fundamental properties of planet candidate host stars, which in turn enables exoplanet researchers to obtain precise fundamental properties of planets (Huber et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Stellar statistics along the ecliptic and the impact on the K2 mission concept

Prša

Robin

Barclay

2014

International Journal of Astrobiology

View full text Add to dashboard Cite

K2 is the mission concept for a repurposed Kepler mission that uses two reaction wheels to maintain the satellite attitude and provide ∼85 days of coverage for ten 105-deg 2 fields along the ecliptic in the first 2.5 years of operation. We examine stellar populations based on the improved Besançon model of the Galaxy, comment on the general properties for the entire ecliptic plane, and provide stellar occurrence rates in the first 6 tentative K2 campaigns grouped by spectral type and luminosity class. For each campaign we distinguish between main sequence stars and giants and provide their density profile as a function of galactic latitude. We introduce the crowding metric that serves for optimized target selection across the campaigns. For all main sequence stars we compute the expected planetary occurrence rates for three planet sizes: 2-4 R ⊕ , 4-8 R ⊕ , and 8-32 R ⊕ with orbital periods up to 50 days. In conjunction with Gaia and the upcoming TESS and Plato missions, K2 will become a gold mine for stellar and planetary astrophysics.

show abstract

Section: Introductionmentioning

confidence: 99%

Stellar statistics along the ecliptic and the impact on the K2 mission concept

Prša

Robin

Barclay

2014

International Journal of Astrobiology

View full text Add to dashboard Cite

show abstract

“…More recently, high-precision time-resolved space photometry has been obtained by the ongoing missions CoRoT (Baglin et al 2006;Auvergne et al 2009) and Kepler (Burocki et al 2010;Gilliland et al 2010) providing significant progress in particular subfields of asteroseismology. Notable discoveries have been made of oscillation properties unknown prior to the era of space asteroseismology for solar-like oscillations, not only in both FGK-type main-sequence stars (e.g., Michel et al 2008;Chaplin et al 2011) and red giants (e.g., De Ridder et al 2009;Beck et al 2011;Bedding et al 2011), but also in a massive O-type star (Degroote et al 2010b).…”

Section: Introductionmentioning

confidence: 99%

Seismic modelling of theβ Cephei star HD 180642 (V1449 Aquilae)

Aerts

Briquet

Degroote

et al. 2011

A&A

View full text Add to dashboard Cite

Context. We present modelling of the β Cep star HD 180642 based on its observational properties deduced from CoRoT and groundbased photometry as well as from time-resolved spectroscopy. Aims. We investigate whether present-day state-of-the-art models are able to explain the full seismic behaviour of this star, which has extended observational constraints for this type of pulsator. Methods. We constructed a dedicated database of stellar models and their oscillation modes tuned to fit the dominant radial mode frequency of HD 180642, by means of varying the hydrogen content, metallicity, mass, age, and core overshooting parameter. We compared the seismic properties of these models with those observed. Results. We find models that are able to explain the numerous observed oscillation properties of the star, for a narrow range in mass of 11.4-11.8 M and no or very mild overshooting (with up to 0.05 local pressure scale heights), except for an excitation problem of the = 3, p 1 mode. We deduce a rotation period of about 13 d, which is fully compatible with recent magnetic field measurements. The seismic models do not support the earlier claim of solar-like oscillations in the star. We instead ascribe the power excess at high frequency to non-linear resonant mode coupling between the high-amplitude radial fundamental mode and several of the low-order pressure modes. We report a discrepancy between the seismic and spectroscopic gravity at the 2.5σ level.

show abstract

“…While dwarfs in Kepler fields seem to have their radii well reproduced by models, there is a discrepancy for masses, still to be clarified (Chaplin et al, 2011). Giants in Kepler represent the ideal sample for testing the variation of stellar properties with z, and hopefully will provide long-awaited constraints to disk-heating and accretion scenarios, and complement the kinematical information either already available (e.g.…”

Section: Discussionmentioning

confidence: 99%

The Expected Stellar Populations in the Kepler and CoRoT Fields

Girardi¹,

Barbieri²,

Miglio³

et al. 2014

Asteroseismology of Stellar Populations in the Milky Way

View full text Add to dashboard Cite

Using the stellar population synthesis tool TRILEGAL, we discuss the expected stellar populations in the Kepler and CoRoT fields. InroductionKepler and CoRoT asteroseismic observations are providing us with precious information about the properties and structure of stars displaced widely across the Galaxy. Observations of these fields will not be repeated any time soon with instrumentation of comparable precision and efficiency. Since both missions were primarily driven by the goal of "finding the most planets", they applied complex target selection criteria which are not ideal for the stellar populations and Galaxy archeology applications which were devised later. Therefore, what can be extracted from this data depends on a good understanding of the data selection, and of our ability to model the entire samples with population synthesis tools. This contribution will concentrate on the latter aspect.

show abstract

Ensemble Asteroseismology of Solar-Type Stars with the NASA Kepler Mission

Abstract: Measurements of 500 Sun-like stars show that their properties differ from those predicted by stellar population models.

Cited by 285 publications

References 32 publications

Stellar statistics along the ecliptic and the impact on the K2 mission concept

Stellar statistics along the ecliptic and the impact on the K2 mission concept

Seismic modelling of theβ Cephei star HD 180642 (V1449 Aquilae)

The Expected Stellar Populations in the Kepler and CoRoT Fields

Contact Info

Product

Resources

About