Hot Stars With Hot Jupiters Have High Obliquities
Author(s)
Winn, Joshua Nathan
Fabrycky, Daniel C.
Albrecht, Simon H.
Johnson, John Asher
Date Issued
July 2010
Journal
Astrophysical Journal. Letters
Publisher
American Physical Society
Citation
Winn, Joshua N. et al. "Hot stars with hot Jupiters have high obliquities." Astrophysical Journal: Letters, 718.2, p.L145–L149, 2010 August 1
Version
Author's final manuscript
Abstract
We show that stars with transiting planets for which the stellar obliquity is large are preferentially hot (T [subscript eff] > 6250 K). This could explain why small obliquities were observed in the earliest measurements, which focused on relatively cool stars drawn from Doppler surveys, as opposed to hotter stars that emerged more recently from transit surveys. The observed trend could be due to differences in planet formation and migration around stars of varying mass. Alternatively, we speculate that hot-Jupiter systems begin with a wide range of obliquities, but the photospheres of cool stars realign with the orbits due to tidal dissipation in their convective zones, while hot stars cannot realign because of their thinner convective zones. This in turn would suggest that hot Jupiters originate from few-body gravitational dynamics and that disk migration plays at most a supporting role.
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 3.0
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1088/2041-8205/718/2/l145
