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Spin-Orbit Alignment for the Circumbinary Planet Host Kepler-16A | | Joshua N. Winn
; Simon Albrecht
; John Asher Johnson
; Guillermo Torres
; William D. Cochran
; Geoffrey W. Marcy
; Andrew Howard
; Howard Isaacson
; Debra Fischer
; Laurance Doyle
; William Welsh
; Joshua A. Carter
; Daniel C. Fabrycky
; Darin Ragozzine
; Samuel N. Quinn
; Avi Shporer
; Steve B. Howell
; David W. Latham
; Jerome Orosz
; Andrej Prsa
; Robert W. Slawson
; William J. Borucki
; David Koch
; Thomas Barclay
; Alan P. Boss
; Jorgen Christensen-Dalsgaard
; Forrest R. Girouard
; Jon Jenkins
; Todd C. Klaus
; Soren Meibom
; Robert L. Morris
; Dimitar Sasselov
; Martin Still
; Jeffrey Van Cleve
; | | Date: |
14 Sep 2011 | | Abstract: | Kepler-16 is an eccentric low-mass eclipsing binary with a circumbinary
transiting planet. Here we investigate the angular momentum of the primary
star, based on Kepler photometry and Keck spectroscopy. The primary star’s
rotation period is 35.1 +/- 1.0 days, and its projected obliquity with respect
to the stellar binary orbit is 1.6 +/- 2.4 degrees. Therefore the three largest
sources of angular momentum---the stellar orbit, the planetary orbit, and the
primary’s rotation---are all closely aligned. This finding supports a formation
scenario involving accretion from a single disk. Alternatively, tides may have
realigned the stars despite their relatively wide separation (0.2 AU), a
hypothesis that is supported by the agreement between the measured rotation
period and the "pseudosynchronous" period of tidal evolution theory. The
rotation period, chromospheric activity level, and fractional light variations
suggest a main-sequence age of 2-4 Gyr. Evolutionary models of low-mass stars
can reproduce the observed properties of the primary star except the model
radius is 2-3% too large, in contrast to the usual problem in which the models
underpredict the observed radius. | | Source: | arXiv, 1109.3198 | | Services: | Forum | Review | PDF | Favorites | |
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