1. Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables
- Author
-
Andrew Bunting, Caroline Terquem, Department of Physics [Oxford], University of Oxford [Oxford], Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
010504 meteorology & atmospheric sciences ,detection ,[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,FOS: Physical sciences ,Perturbation (astronomy) ,01 natural sciences ,Asteroseismology ,Planet ,oscillations -asteroseismology -planets and satellites ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Astronomy and Astrophysics ,Observable ,Planetary system ,Orbital period ,Computational physics ,Radial velocity ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,planet-star interactions -stars ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We calculate the conversion from non-adiabatic, non-radial oscillations tidally induced by a hot Jupiter on a star to observable spectroscopic and photometric signals. Models with both frozen convection and an approximation for a perturbation to the convective flux are discussed. Observables are calculated for some real planetary systems to give specific predictions. Time-dependent line broadening and the radial velocity signal during transit are both investigated as methods to provide further insight into the nature of the stellar oscillations. The photometric signal is predicted to be proportional to the inverse square of the orbital period, $P^{-2}$, as in the equilibrium tide approximation. However, the radial velocity signal is predicted to be proportional to $ P^{-1}$, and is therefore much larger at long orbital periods than the signal corresponding to the equilibrium tide approximation, which is proportional to $P^{-3}$. The prospects for detecting these oscillations and the implications for the detection and characterisation of planets are discussed., Comment: 23 pages, 12 figures. Accepted for publication in MNRAS
- Published
- 2020
- Full Text
- View/download PDF