ASTEROSEISMIC DETERMINATION OF OBLIQUITIES OF THE EXOPLANET SYSTEMS KEPLER-50 AND KEPLER-65
Name
Winn_Asteroseismic.pdf
Size
2.87 MB
Format
Adobe PDF
Checksum (MD5)
29e91b333ad62a4af56cfc3c93d02bb2
Author(s)
Chaplin, William J.
Campante, T. L.
Handberg, R.
Stello, D.
Basu, S.
Christensen-Dalsgaard, J.
Davies, Guy R.
Metcalfe, T. S.
Buchhave, Lars A.
Fischer, Debra A.
Date Issued
March 2013
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Chaplin, W. J., R. Sanchis-Ojeda, T. L. Campante, R. Handberg, D. Stello, J. N. Winn, S. Basu, et al. “ASTEROSEISMIC DETERMINATION OF OBLIQUITIES OF THE EXOPLANET SYSTEMS KEPLER-50 AND KEPLER-65.” The Astrophysical Journal 766, no. 2 (March 14, 2013): 101.
Version
Author's final manuscript
Abstract
Results on the obliquity of exoplanet host stars—the angle between the stellar spin axis and the planetary orbital axis—provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1σ level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1088/0004-637x/766/2/101
