Skip to main content

A High Obliquity Orbit for the Hot-Jupiter HATS-14b Transiting a 5400K Star

Author(s): Zhou, G; Bayliss, D; Hartman, JD; Fulton, BJ; Bakos, Gaspar Aron; et al

Download
To refer to this page use: http://arks.princeton.edu/ark:/88435/pr1wt4f
Abstract: We report a spin–orbit misalignment for the hot-Jupiter HATS-14b, measuring a projected orbital obliquity of 76 . 5 4 ∣l∣ =  - + HATS-14b orbits a high metallicity, 5400 K G dwarf in a relatively short period orbit of 2.8 days. This obliquity was measured via the Rossiter–McLaughlin effect, obtained with observations from Keck-HIRES. The velocities were extracted using a novel technique, optimized for low signal-to-noise spectra, achieving a high precision of 4 m s-1 point-to-point scatter. However, we caution that our uncertainties may be underestimated. Due to the low rotational velocity of the star, the detection significance is dependent on the v i sin prior that is imposed in our modeling. Based on trends observed in the sample of hot Jupiters with obliquity measurements, it has been suggested that these planets modify the spin axes of their host stars, with an efficiency that depends on the stellar type and orbital period of the system. In this framework, short-period planets around stars with surface convective envelopes, like HATS-14b, are expected to have orbits that are aligned with the spin axes of their host stars. HATS-14b, however, is a significant outlier from this trend, challenging the effectiveness of the tidal realignment mechanism.
Publication Date: 20-Nov-2015
Electronic Publication Date: 19-Nov-2015
Citation: Zhou, G, Bayliss, D, Hartman, JD, Fulton, BJ, Bakos, GÁ, Howard, AW, Isaacson, H, Marcy, GW, Schmidt, BP, Brahm, R, Jordán, A. (2015). A High Obliquity Orbit for the Hot-Jupiter HATS-14b Transiting a 5400K Star. \apj, 814 (L16 - L16. doi:10.1088/2041-8205/814/1/L16
DOI: doi:10.1088/2041-8205/814/1/L16
Type of Material: Journal Article
Journal/Proceeding Title: Astrophysical Journal Letters
Version: Final published version. This is an open access article.



Items in OAR@Princeton are protected by copyright, with all rights reserved, unless otherwise indicated.