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

Research output: Contribution to journalArticlepeer-review

Standard

Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7. / Lund, Mikkel N.; Lundkvist, Mia; Aguirre, Victor Silva; Houdek, Günter; Casagrande, Luca; Van Eylen, Vincent; Campante, Tiago L.; Karoff, Christoffer; Kjeldsen, Hans; Albrecht, Simon; Chaplin, William J.; Nielsen, Martin Bo; Degroote, Pieter; Davies, Guy R.; Handberg, Rasmus.

In: Astronomy and Astrophysics, Vol. 570, A54, 01.10.2014.

Research output: Contribution to journalArticlepeer-review

Harvard

Lund, MN, Lundkvist, M, Aguirre, VS, Houdek, G, Casagrande, L, Van Eylen, V, Campante, TL, Karoff, C, Kjeldsen, H, Albrecht, S, Chaplin, WJ, Nielsen, MB, Degroote, P, Davies, GR & Handberg, R 2014, 'Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7', Astronomy and Astrophysics, vol. 570, A54. https://doi.org/10.1051/0004-6361/201424326

APA

Lund, M. N., Lundkvist, M., Aguirre, V. S., Houdek, G., Casagrande, L., Van Eylen, V., Campante, T. L., Karoff, C., Kjeldsen, H., Albrecht, S., Chaplin, W. J., Nielsen, M. B., Degroote, P., Davies, G. R., & Handberg, R. (2014). Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7. Astronomy and Astrophysics, 570, [A54]. https://doi.org/10.1051/0004-6361/201424326

Vancouver

Author

Lund, Mikkel N. ; Lundkvist, Mia ; Aguirre, Victor Silva ; Houdek, Günter ; Casagrande, Luca ; Van Eylen, Vincent ; Campante, Tiago L. ; Karoff, Christoffer ; Kjeldsen, Hans ; Albrecht, Simon ; Chaplin, William J. ; Nielsen, Martin Bo ; Degroote, Pieter ; Davies, Guy R. ; Handberg, Rasmus. / Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7. In: Astronomy and Astrophysics. 2014 ; Vol. 570.

Bibtex

@article{3360fa099cc14632947bf2979054e108,
title = "Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7",
abstract = "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+ 0.04-0.05M, 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°11°. The planet HAT-P-7b is likely retrograde in its orbit, and the orbit is close to being polar. The new parameters for the star give an updated planetary density of ρp = 0.65 ± 0.03 g cm-3, which is lower than previous estimates.",
keywords = "Asteroseismology, Methods: data analysis, Planetary systems, Stars: individual: HAT-P-7, Stars: oscillations, Stars: rotation",
author = "Lund, {Mikkel N.} and Mia Lundkvist and Aguirre, {Victor Silva} and G{\"u}nter Houdek and Luca Casagrande and {Van Eylen}, Vincent and Campante, {Tiago L.} and Christoffer Karoff and Hans Kjeldsen and Simon Albrecht and Chaplin, {William J.} and Nielsen, {Martin Bo} and Pieter Degroote and Davies, {Guy R.} and Rasmus Handberg",
year = "2014",
month = oct,
day = "1",
doi = "10.1051/0004-6361/201424326",
language = "English",
volume = "570",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

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 - Aguirre, Victor Silva

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+ 0.04-0.05M, 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°11°. The planet HAT-P-7b is likely retrograde in its orbit, and the orbit is close to being polar. The new parameters for the star give an updated planetary density of ρp = 0.65 ± 0.03 g cm-3, which is lower than previous estimates.

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+ 0.04-0.05M, 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°11°. The planet HAT-P-7b is likely retrograde in its orbit, and the orbit is close to being polar. The new parameters for the star give an updated planetary density of ρp = 0.65 ± 0.03 g cm-3, which is lower than previous estimates.

KW - Asteroseismology

KW - Methods: data analysis

KW - Planetary systems

KW - Stars: individual: HAT-P-7

KW - Stars: oscillations

KW - Stars: rotation

UR - http://www.scopus.com/inward/record.url?scp=84907923044&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201424326

DO - 10.1051/0004-6361/201424326

M3 - Article

VL - 570

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A54

ER -