A seismic and gravitationally bound double star observed by Kepler: Implication for the presence of a convective core

T. Appourchaux, H. M. Antia, W. Ball, O. Creevey, Y. Lebreton, K. Verma, S. Vorontsov, T. L. Campante, G. R. Davies, P. Gaulme, C. Régulo, E. Horch, S. Howell, M. Everett, D. Ciardi, L. Fossati, A. Miglio, J. Montalbán, W. J. Chaplin, R. A. GarcíaLaurent Gizon

Research output: Contribution to journalArticle

Abstract

Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34-0.33+0.45 M. The total seismic mass using scaling relations is 2.47 ± 0.07 M. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as RA = 1.82-1.87R, MA = 1.25-1.39 M, AgeA = 2.6-3.5 Gyr; RB = 1.22-1.25 R, MB = 1.08-1.14 M, AgeB = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M and [1.34-1.39] M. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M.

Original languageEnglish (US)
Article numberA25
JournalAstronomy and Astrophysics
Volume582
DOIs
StatePublished - Oct 1 2015

Fingerprint

double stars
stars
orbits
oscillation
radii
speckle
interferometry
solar oscillations
asteroseismology
scaling
modeling
speckle interferometry
stellar models
probe
time series
metallicity
power spectra
envelopes
derivation
luminosity

Keywords

  • asteroseismology
  • astrometry
  • binaries: general
  • stars: evolution
  • stars: solar-type

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

A seismic and gravitationally bound double star observed by Kepler : Implication for the presence of a convective core. / Appourchaux, T.; Antia, H. M.; Ball, W.; Creevey, O.; Lebreton, Y.; Verma, K.; Vorontsov, S.; Campante, T. L.; Davies, G. R.; Gaulme, P.; Régulo, C.; Horch, E.; Howell, S.; Everett, M.; Ciardi, D.; Fossati, L.; Miglio, A.; Montalbán, J.; Chaplin, W. J.; García, R. A.; Gizon, Laurent.

In: Astronomy and Astrophysics, Vol. 582, A25, 01.10.2015.

Research output: Contribution to journalArticle

Appourchaux, T, Antia, HM, Ball, W, Creevey, O, Lebreton, Y, Verma, K, Vorontsov, S, Campante, TL, Davies, GR, Gaulme, P, Régulo, C, Horch, E, Howell, S, Everett, M, Ciardi, D, Fossati, L, Miglio, A, Montalbán, J, Chaplin, WJ, García, RA & Gizon, L 2015, 'A seismic and gravitationally bound double star observed by Kepler: Implication for the presence of a convective core', Astronomy and Astrophysics, vol. 582, A25. https://doi.org/10.1051/0004-6361/201526610
Appourchaux, T. ; Antia, H. M. ; Ball, W. ; Creevey, O. ; Lebreton, Y. ; Verma, K. ; Vorontsov, S. ; Campante, T. L. ; Davies, G. R. ; Gaulme, P. ; Régulo, C. ; Horch, E. ; Howell, S. ; Everett, M. ; Ciardi, D. ; Fossati, L. ; Miglio, A. ; Montalbán, J. ; Chaplin, W. J. ; García, R. A. ; Gizon, Laurent. / A seismic and gravitationally bound double star observed by Kepler : Implication for the presence of a convective core. In: Astronomy and Astrophysics. 2015 ; Vol. 582.
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abstract = "Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34-0.33+0.45 M⊙. The total seismic mass using scaling relations is 2.47 ± 0.07 M⊙. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M⊙ consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as RA = 1.82-1.87R⊙, MA = 1.25-1.39 M⊙, AgeA = 2.6-3.5 Gyr; RB = 1.22-1.25 R⊙, MB = 1.08-1.14 M⊙, AgeB = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M⊙ and [1.34-1.39] M⊙. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M⊙.",
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TY - JOUR

T1 - A seismic and gravitationally bound double star observed by Kepler

T2 - Implication for the presence of a convective core

AU - Appourchaux, T.

AU - Antia, H. M.

AU - Ball, W.

AU - Creevey, O.

AU - Lebreton, Y.

AU - Verma, K.

AU - Vorontsov, S.

AU - Campante, T. L.

AU - Davies, G. R.

AU - Gaulme, P.

AU - Régulo, C.

AU - Horch, E.

AU - Howell, S.

AU - Everett, M.

AU - Ciardi, D.

AU - Fossati, L.

AU - Miglio, A.

AU - Montalbán, J.

AU - Chaplin, W. J.

AU - García, R. A.

AU - Gizon, Laurent

PY - 2015/10/1

Y1 - 2015/10/1

N2 - Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34-0.33+0.45 M⊙. The total seismic mass using scaling relations is 2.47 ± 0.07 M⊙. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M⊙ consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as RA = 1.82-1.87R⊙, MA = 1.25-1.39 M⊙, AgeA = 2.6-3.5 Gyr; RB = 1.22-1.25 R⊙, MB = 1.08-1.14 M⊙, AgeB = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M⊙ and [1.34-1.39] M⊙. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M⊙.

AB - Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34-0.33+0.45 M⊙. The total seismic mass using scaling relations is 2.47 ± 0.07 M⊙. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M⊙ consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as RA = 1.82-1.87R⊙, MA = 1.25-1.39 M⊙, AgeA = 2.6-3.5 Gyr; RB = 1.22-1.25 R⊙, MB = 1.08-1.14 M⊙, AgeB = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M⊙ and [1.34-1.39] M⊙. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M⊙.

KW - asteroseismology

KW - astrometry

KW - binaries: general

KW - stars: evolution

KW - stars: solar-type

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