Kepler observations of the asteroseismic binary HD 176465
Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse...
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Journal article |
| Language: | English |
| Published: |
EDP Sciences
2017
|
| _version_ | 1797050715256913920 |
|---|---|
| author | White, T Benomar, O Silva Aguirre, V Ball, W Bedding, T Chaplin, W Christensen-Dalsgaard, J Garcia, R Gizon, L Stello, D Aigrain, S Antia, H Appourchaux, T Bazot, M Campante, T Creevey, O Davies, G Elsworth, Y Gaulme, P Handberg, R Hekker, S Houdek, G Howe, R Huber, D Karoff, C Marques, J Mathur, S McQuillan, A Metcalfe, T Mosser, B Nielsen, M Régulo, C Salabert, D Stahn, T |
| author_facet | White, T Benomar, O Silva Aguirre, V Ball, W Bedding, T Chaplin, W Christensen-Dalsgaard, J Garcia, R Gizon, L Stello, D Aigrain, S Antia, H Appourchaux, T Bazot, M Campante, T Creevey, O Davies, G Elsworth, Y Gaulme, P Handberg, R Hekker, S Houdek, G Howe, R Huber, D Karoff, C Marques, J Mathur, S McQuillan, A Metcalfe, T Mosser, B Nielsen, M Régulo, C Salabert, D Stahn, T |
| author_sort | White, T |
| collection | OXFORD |
| description | Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementaryparameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0 ± 0.5 Gyr old. The two components of HD 176465 are young physically-similar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology. |
| first_indexed | 2024-03-06T18:09:17Z |
| format | Journal article |
| id | oxford-uuid:02734206-c905-4440-af61-b0d1c63658fa |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:09:17Z |
| publishDate | 2017 |
| publisher | EDP Sciences |
| record_format | dspace |
| spelling | oxford-uuid:02734206-c905-4440-af61-b0d1c63658fa2022-03-26T08:40:55ZKepler observations of the asteroseismic binary HD 176465Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:02734206-c905-4440-af61-b0d1c63658faEnglishSymplectic Elements at OxfordEDP Sciences2017White, TBenomar, OSilva Aguirre, VBall, WBedding, TChaplin, WChristensen-Dalsgaard, JGarcia, RGizon, LStello, DAigrain, SAntia, HAppourchaux, TBazot, MCampante, TCreevey, ODavies, GElsworth, YGaulme, PHandberg, RHekker, SHoudek, GHowe, RHuber, DKaroff, CMarques, JMathur, SMcQuillan, AMetcalfe, TMosser, BNielsen, MRégulo, CSalabert, DStahn, TBinary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementaryparameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0 ± 0.5 Gyr old. The two components of HD 176465 are young physically-similar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology. |
| spellingShingle | White, T Benomar, O Silva Aguirre, V Ball, W Bedding, T Chaplin, W Christensen-Dalsgaard, J Garcia, R Gizon, L Stello, D Aigrain, S Antia, H Appourchaux, T Bazot, M Campante, T Creevey, O Davies, G Elsworth, Y Gaulme, P Handberg, R Hekker, S Houdek, G Howe, R Huber, D Karoff, C Marques, J Mathur, S McQuillan, A Metcalfe, T Mosser, B Nielsen, M Régulo, C Salabert, D Stahn, T Kepler observations of the asteroseismic binary HD 176465 |
| title | Kepler observations of the asteroseismic binary HD 176465 |
| title_full | Kepler observations of the asteroseismic binary HD 176465 |
| title_fullStr | Kepler observations of the asteroseismic binary HD 176465 |
| title_full_unstemmed | Kepler observations of the asteroseismic binary HD 176465 |
| title_short | Kepler observations of the asteroseismic binary HD 176465 |
| title_sort | kepler observations of the asteroseismic binary hd 176465 |
| work_keys_str_mv | AT whitet keplerobservationsoftheasteroseismicbinaryhd176465 AT benomaro keplerobservationsoftheasteroseismicbinaryhd176465 AT silvaaguirrev keplerobservationsoftheasteroseismicbinaryhd176465 AT ballw keplerobservationsoftheasteroseismicbinaryhd176465 AT beddingt keplerobservationsoftheasteroseismicbinaryhd176465 AT chaplinw keplerobservationsoftheasteroseismicbinaryhd176465 AT christensendalsgaardj keplerobservationsoftheasteroseismicbinaryhd176465 AT garciar keplerobservationsoftheasteroseismicbinaryhd176465 AT gizonl keplerobservationsoftheasteroseismicbinaryhd176465 AT stellod keplerobservationsoftheasteroseismicbinaryhd176465 AT aigrains keplerobservationsoftheasteroseismicbinaryhd176465 AT antiah keplerobservationsoftheasteroseismicbinaryhd176465 AT appourchauxt keplerobservationsoftheasteroseismicbinaryhd176465 AT bazotm keplerobservationsoftheasteroseismicbinaryhd176465 AT campantet keplerobservationsoftheasteroseismicbinaryhd176465 AT creeveyo keplerobservationsoftheasteroseismicbinaryhd176465 AT daviesg keplerobservationsoftheasteroseismicbinaryhd176465 AT elsworthy keplerobservationsoftheasteroseismicbinaryhd176465 AT gaulmep keplerobservationsoftheasteroseismicbinaryhd176465 AT handbergr keplerobservationsoftheasteroseismicbinaryhd176465 AT hekkers keplerobservationsoftheasteroseismicbinaryhd176465 AT houdekg keplerobservationsoftheasteroseismicbinaryhd176465 AT hower keplerobservationsoftheasteroseismicbinaryhd176465 AT huberd keplerobservationsoftheasteroseismicbinaryhd176465 AT karoffc keplerobservationsoftheasteroseismicbinaryhd176465 AT marquesj keplerobservationsoftheasteroseismicbinaryhd176465 AT mathurs keplerobservationsoftheasteroseismicbinaryhd176465 AT mcquillana keplerobservationsoftheasteroseismicbinaryhd176465 AT metcalfet keplerobservationsoftheasteroseismicbinaryhd176465 AT mosserb keplerobservationsoftheasteroseismicbinaryhd176465 AT nielsenm keplerobservationsoftheasteroseismicbinaryhd176465 AT reguloc keplerobservationsoftheasteroseismicbinaryhd176465 AT salabertd keplerobservationsoftheasteroseismicbinaryhd176465 AT stahnt keplerobservationsoftheasteroseismicbinaryhd176465 |