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. García & 1 others Laurent 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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    author = "T. Appourchaux and Antia, {H. M.} and W. Ball and O. Creevey and Y. Lebreton and K. Verma and S. Vorontsov and Campante, {T. L.} and Davies, {G. R.} and P. Gaulme and C. R{\'e}gulo and E. Horch and S. Howell and M. Everett and D. Ciardi and L. Fossati and A. Miglio and J. Montalb{\'a}n and Chaplin, {W. J.} and Garc{\'i}a, {R. A.} and Laurent Gizon",
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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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