Testing stellar evolution models with the retired A star HD 185351

J. G. Hjørringgaard; V. Silva Aguirre; T. R. White; D. Huber; B. J. S. Pope; L. Casagrande; A. B. Justesen; J. Christensen-Dalsgaard

doi:10.1093/mnras/stw2559

Testing stellar evolution models with the retired A star HD 185351

J. G. Hjørringgaard, V. Silva Aguirre, T. R. White, D. Huber, B. J. S. Pope, L. Casagrande, A. B. Justesen, J. Christensen-Dalsgaard

Department of Physics and Astronomy - Stellar Astrophysics Centre

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Abstract

The physical parameters of the retired A star HD 185351 were analysed in great detail by Johnson et al. using interferometry, spectroscopy, and asteroseismology. Results from all independent methods are consistent with HD 185351 having a mass in excess of 1.5 M⊙. However, the study also showed that not all observational constraints could be reconciled in stellar evolutionary models, leading to mass estimates ranging from ˜1.6 to 1.9 M⊙ and casting doubts on the accuracy of stellar properties determined from asteroseismology. Here, we solve this discrepancy and construct a theoretical model in agreement with all observational constraints on the physical parameters of HD 185351. The effects of varying input physics are examined as well as the additional constraint of the observed g-mode period spacing is considered. This quantity is found to be sensitive to the inclusion of additional mixing from the convective core during the main sequence, and can be used to calibrate the overshooting efficiency using low-luminosity red giant stars. A theoretical model with metallicity [Fe/H] = 0.16 dex, mixing-length parameter αMLT = 2.00, and convective overshooting efficiency parameter f = 0.030 is found to be in complete agreement with all observational constraints for a stellar mass of M ≃ 1.60 M⊙.

Original language	English
Journal	Royal Astronomical Society. Monthly Notices
Volume	464
Issue	3
Pages (from-to)	3713-3719
Number of pages	7
ISSN	0035-8711
DOIs	https://doi.org/10.1093/mnras/stw2559
Publication status	Published - 1 Jan 2017

Keywords

asteroseismology
stars: individual: HD 185351
stars: interiors

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10.1093/mnras/stw2559

Testing stellar evolution models with the retired A star HD 185351Final published version, 2.39 MBLicence: Other

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title = "Testing stellar evolution models with the retired A star HD 185351",

abstract = "The physical parameters of the retired A star HD 185351 were analysed in great detail by Johnson et al. using interferometry, spectroscopy, and asteroseismology. Results from all independent methods are consistent with HD 185351 having a mass in excess of 1.5 M⊙. However, the study also showed that not all observational constraints could be reconciled in stellar evolutionary models, leading to mass estimates ranging from ˜1.6 to 1.9 M⊙ and casting doubts on the accuracy of stellar properties determined from asteroseismology. Here, we solve this discrepancy and construct a theoretical model in agreement with all observational constraints on the physical parameters of HD 185351. The effects of varying input physics are examined as well as the additional constraint of the observed g-mode period spacing is considered. This quantity is found to be sensitive to the inclusion of additional mixing from the convective core during the main sequence, and can be used to calibrate the overshooting efficiency using low-luminosity red giant stars. A theoretical model with metallicity [Fe/H] = 0.16 dex, mixing-length parameter αMLT = 2.00, and convective overshooting efficiency parameter f = 0.030 is found to be in complete agreement with all observational constraints for a stellar mass of M ≃ 1.60 M⊙.",

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author = "Hj{\o}rringgaard, {J. G.} and {Silva Aguirre}, V. and White, {T. R.} and D. Huber and Pope, {B. J. S.} and L. Casagrande and Justesen, {A. B.} and J. Christensen-Dalsgaard",

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Testing stellar evolution models with the retired A star HD 185351. / Hjørringgaard, J. G.; Silva Aguirre, V.; White, T. R. et al.
In: Royal Astronomical Society. Monthly Notices, Vol. 464, No. 3, 01.01.2017, p. 3713-3719.

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaper › Journal article › Research › peer-review

TY - JOUR

T1 - Testing stellar evolution models with the retired A star HD 185351

AU - Hjørringgaard, J. G.

AU - Silva Aguirre, V.

AU - White, T. R.

AU - Huber, D.

AU - Pope, B. J. S.

AU - Casagrande, L.

AU - Justesen, A. B.

AU - Christensen-Dalsgaard, J.

PY - 2017/1/1

Y1 - 2017/1/1

N2 - The physical parameters of the retired A star HD 185351 were analysed in great detail by Johnson et al. using interferometry, spectroscopy, and asteroseismology. Results from all independent methods are consistent with HD 185351 having a mass in excess of 1.5 M⊙. However, the study also showed that not all observational constraints could be reconciled in stellar evolutionary models, leading to mass estimates ranging from ˜1.6 to 1.9 M⊙ and casting doubts on the accuracy of stellar properties determined from asteroseismology. Here, we solve this discrepancy and construct a theoretical model in agreement with all observational constraints on the physical parameters of HD 185351. The effects of varying input physics are examined as well as the additional constraint of the observed g-mode period spacing is considered. This quantity is found to be sensitive to the inclusion of additional mixing from the convective core during the main sequence, and can be used to calibrate the overshooting efficiency using low-luminosity red giant stars. A theoretical model with metallicity [Fe/H] = 0.16 dex, mixing-length parameter αMLT = 2.00, and convective overshooting efficiency parameter f = 0.030 is found to be in complete agreement with all observational constraints for a stellar mass of M ≃ 1.60 M⊙.

AB - The physical parameters of the retired A star HD 185351 were analysed in great detail by Johnson et al. using interferometry, spectroscopy, and asteroseismology. Results from all independent methods are consistent with HD 185351 having a mass in excess of 1.5 M⊙. However, the study also showed that not all observational constraints could be reconciled in stellar evolutionary models, leading to mass estimates ranging from ˜1.6 to 1.9 M⊙ and casting doubts on the accuracy of stellar properties determined from asteroseismology. Here, we solve this discrepancy and construct a theoretical model in agreement with all observational constraints on the physical parameters of HD 185351. The effects of varying input physics are examined as well as the additional constraint of the observed g-mode period spacing is considered. This quantity is found to be sensitive to the inclusion of additional mixing from the convective core during the main sequence, and can be used to calibrate the overshooting efficiency using low-luminosity red giant stars. A theoretical model with metallicity [Fe/H] = 0.16 dex, mixing-length parameter αMLT = 2.00, and convective overshooting efficiency parameter f = 0.030 is found to be in complete agreement with all observational constraints for a stellar mass of M ≃ 1.60 M⊙.

KW - asteroseismology

KW - stars: individual: HD 185351

KW - stars: interiors

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JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

IS - 3

ER -

Testing stellar evolution models with the retired A star HD 185351

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