The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

M. Bazot; M. J. Ireland; D. Huber; T. R. Bedding; A. M. Broomhall; T. L. Campante; H. Carfantan; W. J. Chaplin; Y. Elsworth; J. Meléndez; P. Petit; S. Théado; V. Van Grootel; T. Arentoft; M. Asplund; M. Castro; J. Christensen-Dalsgaard; J. D. Do Nascimento; B. Dintrans; X. Dumusque; H. Kjeldsen; H. A. McAlister; T. S. Metcalfe; M. J P F G Monteiro; N. C. Santos; S. Sousa; J. Sturmann; L. Sturmann; T. A. Ten Brummelaar; N. Turner; S. Vauclair

doi:10.1051/0004-6361/201015679

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

M. Bazot^*, M. J. Ireland, D. Huber, T. R. Bedding, A. M. Broomhall, T. L. Campante, H. Carfantan, W. J. Chaplin, Y. Elsworth, J. Meléndez, P. Petit, S. Théado, V. Van Grootel, T. Arentoft, M. Asplund, M. Castro, J. Christensen-Dalsgaard, J. D. Do Nascimento, B. Dintrans, X. DumusqueH. Kjeldsen, H. A. McAlister, T. S. Metcalfe, M. J P F G Monteiro, N. C. Santos, S. Sousa, J. Sturmann, L. Sturmann, T. A. Ten Brummelaar, N. Turner, S. Vauclair

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

27 Citations (Scopus)

17 Downloads (Pure)

Abstract

The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

Original language	English
Article number	L4
Pages (from-to)	1-4
Number of pages	4
Journal	Astronomy and Astrophysics
Volume	526
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361/201015679
Publication status	Published - 13 Dec 2010
Externally published	Yes

Bibliographical note

Access to Document

10.1051/0004-6361/201015679

Publisher version (open access).pdfFinal published version, 261 KB

Cite this

Bazot, M., Ireland, M. J., Huber, D., Bedding, T. R., Broomhall, A. M., Campante, T. L., Carfantan, H., Chaplin, W. J., Elsworth, Y., Meléndez, J., Petit, P., Théado, S., Van Grootel, V., Arentoft, T., Asplund, M., Castro, M., Christensen-Dalsgaard, J., Do Nascimento, J. D., Dintrans, B., ... Vauclair, S. (2010). The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry. Astronomy and Astrophysics, 526(1), 1-4. Article L4. https://doi.org/10.1051/0004-6361/201015679

@article{a1f618f01caa4431b55e74d8ca2dffed,

title = "The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry",

abstract = "The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.",

author = "M. Bazot and Ireland, \{M. J.\} and D. Huber and Bedding, \{T. R.\} and Broomhall, \{A. M.\} and Campante, \{T. L.\} and H. Carfantan and Chaplin, \{W. J.\} and Y. Elsworth and J. Mel{\'e}ndez and P. Petit and S. Th{\'e}ado and \{Van Grootel\}, V. and T. Arentoft and M. Asplund and M. Castro and J. Christensen-Dalsgaard and \{Do Nascimento\}, \{J. D.\} and B. Dintrans and X. Dumusque and H. Kjeldsen and McAlister, \{H. A.\} and Metcalfe, \{T. S.\} and Monteiro, \{M. J P F G\} and Santos, \{N. C.\} and S. Sousa and J. Sturmann and L. Sturmann and \{Ten Brummelaar\}, \{T. A.\} and N. Turner and S. Vauclair",

note = "Copyright 2010 ESO. First published in Astronomy and Astrophysics, Vol. 526, No. 1, published by EDP Sciences. The original publication is available at http://dx.doi.org/10.1051/0004-6361/201015679",

year = "2010",

month = dec,

day = "13",

doi = "10.1051/0004-6361/201015679",

language = "English",

volume = "526",

pages = "1--4",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "1",

}

Bazot, M, Ireland, MJ, Huber, D, Bedding, TR, Broomhall, AM, Campante, TL, Carfantan, H, Chaplin, WJ, Elsworth, Y, Meléndez, J, Petit, P, Théado, S, Van Grootel, V, Arentoft, T, Asplund, M, Castro, M, Christensen-Dalsgaard, J, Do Nascimento, JD, Dintrans, B, Dumusque, X, Kjeldsen, H, McAlister, HA, Metcalfe, TS, Monteiro, MJPFG, Santos, NC, Sousa, S, Sturmann, J, Sturmann, L, Ten Brummelaar, TA, Turner, N & Vauclair, S 2010, 'The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry', Astronomy and Astrophysics, vol. 526, no. 1, L4, pp. 1-4. https://doi.org/10.1051/0004-6361/201015679

TY - JOUR

T1 - The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

AU - Bazot, M.

AU - Ireland, M. J.

AU - Huber, D.

AU - Bedding, T. R.

AU - Broomhall, A. M.

AU - Campante, T. L.

AU - Carfantan, H.

AU - Chaplin, W. J.

AU - Elsworth, Y.

AU - Meléndez, J.

AU - Petit, P.

AU - Théado, S.

AU - Van Grootel, V.

AU - Arentoft, T.

AU - Asplund, M.

AU - Castro, M.

AU - Christensen-Dalsgaard, J.

AU - Do Nascimento, J. D.

AU - Dintrans, B.

AU - Dumusque, X.

AU - Kjeldsen, H.

AU - McAlister, H. A.

AU - Metcalfe, T. S.

AU - Monteiro, M. J P F G

AU - Santos, N. C.

AU - Sousa, S.

AU - Sturmann, J.

AU - Sturmann, L.

AU - Ten Brummelaar, T. A.

AU - Turner, N.

AU - Vauclair, S.

N1 - Copyright 2010 ESO. First published in Astronomy and Astrophysics, Vol. 526, No. 1, published by EDP Sciences. The original publication is available at http://dx.doi.org/10.1051/0004-6361/201015679

PY - 2010/12/13

Y1 - 2010/12/13

N2 - The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

AB - The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

UR - https://www.scopus.com/pages/publications/78650131000

U2 - 10.1051/0004-6361/201015679

DO - 10.1051/0004-6361/201015679

M3 - Article

AN - SCOPUS:78650131000

SN - 0004-6361

VL - 526

SP - 1

EP - 4

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

M1 - L4

ER -

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

Abstract

Bibliographical note

Access to Document

Other files and links

Fingerprint

Cite this