Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7

TY - JOUR

T1 - Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7

AU - Lund, Mikkel N.

AU - Lundkvist, Mia

AU - Silva Aguirre, Victor

AU - Houdek, Günter

AU - Casagrande, Luca

AU - Van Eylen, Vincent

AU - Campante, Tiago L.

AU - Karoff, Christoffer

AU - Kjeldsen, Hans

AU - Albrecht, Simon

AU - Chaplin, William J.

AU - Nielsen, Martin Bo

AU - Degroote, Pieter

AU - Davies, Guy R.

AU - Handberg, Rasmus

PY - 2014/10/1

Y1 - 2014/10/1

N2 - Context. The measurement of obliquities - the angle between the orbital and stellar rotation - in star-planet systems is of great importance for understanding planet system formation and evolution. The bright and well-studied HAT-P-7 (Kepler-2) system is intriguing because several Rossiter-McLaughlin (RM) measurements found a high projected obliquity in this system, but it was not possible so far to determine whether the orbit is polar and/or retrograde. Aims: The goal of this study is to measure the stellar inclination and hereby the full 3D obliquity of the HAT-P-7 system instead of only the 2D projection as measured by the RM effect. In addition, we provide an updated set of stellar parameters for the star. Methods: We used the full set of available observations from Kepler spanning Q0-Q17 to produce the power spectrum of HAT-P-7. We extracted oscillation-mode frequencies via an Markov chain Monte Carlo peak-bagging routine and used the results from this to estimate the stellar inclination angle. Combining this with the projected obliquity from RM and the inclination of the orbital plane allowed us to determine the stellar obliquity. Furthermore, we used asteroseismology to model the star from the extracted frequencies using two different approaches to the modelling, for which either the stellar evolution codes MESA or GARSTEC were adopted. Results: Our updated asteroseismic modelling shows, i.a., the following stellar parameters for HAT-P-7: M⋆ = 1.51+ 0.04-0.05 M⊙, R⋆ = 2.00+ 0.01-0.02 R⊙, and age = 2.07+ 0.28-0.23 Gyr. The modelling offers a high precision on the stellar parameters, the uncertainty on age, for instance, is of the order ˜ 11%. For the stellar inclination we estimate i⋆<36.5°, which translates into an obliquity of 83°

AB - Context. The measurement of obliquities - the angle between the orbital and stellar rotation - in star-planet systems is of great importance for understanding planet system formation and evolution. The bright and well-studied HAT-P-7 (Kepler-2) system is intriguing because several Rossiter-McLaughlin (RM) measurements found a high projected obliquity in this system, but it was not possible so far to determine whether the orbit is polar and/or retrograde. Aims: The goal of this study is to measure the stellar inclination and hereby the full 3D obliquity of the HAT-P-7 system instead of only the 2D projection as measured by the RM effect. In addition, we provide an updated set of stellar parameters for the star. Methods: We used the full set of available observations from Kepler spanning Q0-Q17 to produce the power spectrum of HAT-P-7. We extracted oscillation-mode frequencies via an Markov chain Monte Carlo peak-bagging routine and used the results from this to estimate the stellar inclination angle. Combining this with the projected obliquity from RM and the inclination of the orbital plane allowed us to determine the stellar obliquity. Furthermore, we used asteroseismology to model the star from the extracted frequencies using two different approaches to the modelling, for which either the stellar evolution codes MESA or GARSTEC were adopted. Results: Our updated asteroseismic modelling shows, i.a., the following stellar parameters for HAT-P-7: M⋆ = 1.51+ 0.04-0.05 M⊙, R⋆ = 2.00+ 0.01-0.02 R⊙, and age = 2.07+ 0.28-0.23 Gyr. The modelling offers a high precision on the stellar parameters, the uncertainty on age, for instance, is of the order ˜ 11%. For the stellar inclination we estimate i⋆<36.5°, which translates into an obliquity of 83°

KW - asteroseismology

KW - planetary systems

KW - stars: oscillations

KW - stars: individual: HAT-P-7

KW - methods: data analysis

KW - stars: rotation

U2 - 10.1051/0004-6361/201424326

DO - 10.1051/0004-6361/201424326

M3 - Journal article

SN - 0004-6361

VL - 570

JO - Astronomy & Astrophysics (A&A)

JF - Astronomy & Astrophysics (A&A)

ER -