T. S. Metcalfe, O. L. Creevey, G. Doǧan, S. Mathur, H. Xu, T. R. Bedding, W. J. Chaplin, J. Christensen-Dalsgaard, C. Karoff, R. Trampedach, O. Benomar, B. P. Brown, D. L. Buzasi, T. L. Campante, Z. «elik Orhan, M. S. Cunha, G. R. Davies, S. Deheuvels, A. Derekas, M. P. Di Mauro, R. A. GarcŪa, J. A. Guzik, R. Howe, K. B. MacGregor, A. Mazumdar, J. MontalbŠn, M. J. P. F. G. Monteiro, M. Gruberbauer, D. B. Guenther, Y. Lebreton, K. Molaverdikhani, D. Pricopi, R. Simoniello, T. R. White
Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been accompanied by a shift in analysis and modeling strategies to yield uniform sets of derived stellar properties more quickly and easily. We use previously published asteroseismic and spectroscopic data sets to provide a uniform analysis of 42 solar-type Kepler targets from the Asteroseismic Modeling Portal (AMP). We find that fitting the individual frequencies typically doubles the precision of the asteroseismic radius, mass and age compared to grid-based modeling of the global oscillation properties, and improves the precision of the radius and mass by about a factor of three over empirical scaling relations. We use the stellar radii and masses to test an empirical scaling relation for the frequency of maximum oscillation power, we derive new age-rotation-activity relations from the updated age estimates, we compare the bulk compositions to the expectations of Galactic chemical enrichment, and we find qualitative agreement between the derived mixing-length values and a recent calibration from threedimensional (3D) convection simulations.
methods: numerical—stars: evolution—stars: interiors—stars: oscillations
The Astrophysical Journal Supplement Series
Volume 214, Page 27_1