@article{5745bef167c84ab6901b3209340ef3c8,
title = "Oscillation mode linewidths of main-sequence and subgiant stars observed by Kepler",
abstract = "Context. Solar-like oscillations have been observed by Kepler and CoRoT in several solar-type stars. Aims. We study the variations in the stellar p-mode linewidth as a function of effective temperature. Methods. We study a time series of nine months of Kepler data. We analyse the power spectra of 42 cool main-sequence stars and subgiants using both maximum likelihood estimators and Bayesian estimators to recover individual mode characteristics such as frequencies, linewidths, and mode heights. Results. We report on the mode linewidth at both maximum power and maximum mode height for these 42 stars as a function of effective temperature. Conclusions. We show that the mode linewidth at either maximum mode height or maximum amplitude follows a scaling relation with effective temperature, which is a combination of a power law and a lower bound. The typical power-law index is about 13 for the linewidth derived from the maximum mode height, and about 16 for the linewidth derived from the maximum amplitude, while the lower bound is about 0.3 μHz and 0.7 μHz, respectively. We stress that this scaling relation is only valid for cool main-sequence stars and subgiants, and does not have any predictive power outside the temperature range of these stars.",
keywords = "asteroseismology, methods: data analysis, stars: solar-type",
author = "T. Appourchaux and O. Benomar and M. Gruberbauer and Chaplin, {W. J.} and Garc{\'i}a, {R. A.} and R. Handberg and Verner, {G. A.} and Antia, {H. M.} and Campante, {T. L.} and Davies, {G. R.} and S. Deheuvels and S. Hekker and R. Howe and D. Salabert and Bedding, {T. R.} and White, {T. R.} and G. Houdek and {Silva Aguirre}, V. and Elsworth, {Y. P.} and {Van Cleve}, J. and Clarke, {B. D.} and Hall, {J. R.} and H. Kjeldsen",
note = "Funding Information: The authors wish to thank the entire Kepler team, without whom these results would not be possible. Funding for this Discovery mission is provided by NASA{\textquoteright}s Science Mission Directorate. We also thank all funding councils and agencies that have supported the activities of KASC Working Group 1, as well as the International Space Science Institute (ISSI). This research was supported in part by the National Science Foundation under Grant No. NSF PHY05-51164. W.J.C., G.A.V., and Y.E. acknowledge financial support from the UK Science and Technology Facilities Council (STFC). R.A.G. and G.R.D. has received funding from the European Community{\textquoteright}s Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194. M.G. received financial support from an NSERC Vanier scholarship. This work employed computational facilities provided by ACEnet, the regional high performance computing consortium for universities in Atlantic Canada. SH acknowledges funding from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO). G.H. acknowledges support by the Austrian Science Fund (FWF) project P21205-N16. R.H. acknowledges computing support from the National Solar Observatory. D.S. acknowledges the financial support from the Centre National d{\textquoteright}Etudes Spatiales (CNES).",
year = "2012",
doi = "10.1051/0004-6361/201118496",
language = "English (US)",
volume = "537",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
}