Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods

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Asteroseismic modelling of solar-type stars : internal systematics from input physics and surface correction methods. / Nsamba, B.; Campante, T. L.; Monteiro, M. J. P. F. G.; Cunha, M. S.; Rendle, B. M.; Reese, D. R.; Verma, K.

In: Monthly Notices of the Royal Astronomical Society, Vol. 477, No. 4, 07.2018, p. 5052-5063.

Research output: Contribution to journal/Conference contribution in journal/Contribution to newspaperJournal articleResearchpeer-review

Harvard

Nsamba, B, Campante, TL, Monteiro, MJPFG, Cunha, MS, Rendle, BM, Reese, DR & Verma, K 2018, 'Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods', Monthly Notices of the Royal Astronomical Society, vol. 477, no. 4, pp. 5052-5063. https://doi.org/10.1093/mnras/sty948

APA

Nsamba, B., Campante, T. L., Monteiro, M. J. P. F. G., Cunha, M. S., Rendle, B. M., Reese, D. R., & Verma, K. (2018). Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods. Monthly Notices of the Royal Astronomical Society, 477(4), 5052-5063. https://doi.org/10.1093/mnras/sty948

CBE

Nsamba B, Campante TL, Monteiro MJPFG, Cunha MS, Rendle BM, Reese DR, Verma K. 2018. Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods. Monthly Notices of the Royal Astronomical Society. 477(4):5052-5063. https://doi.org/10.1093/mnras/sty948

MLA

Vancouver

Nsamba B, Campante TL, Monteiro MJPFG, Cunha MS, Rendle BM, Reese DR et al. Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods. Monthly Notices of the Royal Astronomical Society. 2018 Jul;477(4):5052-5063. https://doi.org/10.1093/mnras/sty948

Author

Nsamba, B. ; Campante, T. L. ; Monteiro, M. J. P. F. G. ; Cunha, M. S. ; Rendle, B. M. ; Reese, D. R. ; Verma, K. / Asteroseismic modelling of solar-type stars : internal systematics from input physics and surface correction methods. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 477, No. 4. pp. 5052-5063.

Bibtex

@article{1b70c5f0df9340288ad0293487417001,
title = "Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods",
abstract = "Asteroseismic forward modelling techniques are being used to determine fundamental properties (e.g. mass, radius, and age) of solar-type stars. The need to take into account all possible sources of error is of paramount importance towards a robust determination of stellar properties. We present a study of 34 solar-type stars for which high signal-to-noise asteroseismic data are available from multiyear Kepler photometry. We explore the internal systematics on the stellar properties, that is associated with the uncertainty in the input physics used to construct the stellar models. In particular, we explore the systematics arising from (i) the inclusion of the diffusion of helium and heavy elements; (ii) the uncertainty in solar metallicity mixture; and (iii) different surface correction methods used in optimization/fitting procedures. The systematics arising from comparing results of models with and without diffusion are found to be 0.5 per cent, 0.8 per cent, 2.1 per cent, and 16 per cent in mean density, radius, mass, and age, respectively. The internal systematics in age are significantly larger than the statistical uncertainties. We find the internal systematics resulting from the uncertainty in solar metallicity mixture to be 0.7 per cent in mean density, 0.5 per cent in radius, 1.4 per cent in mass, and 6.7 per cent in age. The surface correction method by Sonoi et al. and Ball & Gizon's two-term correction produce the lowest internal systematics among the different correction methods, namely, similar to 1 per cent, similar to 1 per cent, similar to 2 per cent, and similar to 8 per cent in mean density, radius, mass, and age, respectively. Stellar masses obtained using the surface correction methods by Kjeldsen et al. and Ball & Gizon's one-term correction are systematically higher than those obtained using frequency ratios.",
keywords = "asteroseismology, stars: evolution, stars: fundamental parameters, stars: oscillations, METAL-POOR STARS, OSCILLATION FREQUENCIES, ELEMENT DIFFUSION, HELIUM ABUNDANCE, SUN, EVOLUTION, HELIOSEISMOLOGY, OPACITIES, INTERIOR, MISSION",
author = "B. Nsamba and Campante, {T. L.} and Monteiro, {M. J. P. F. G.} and Cunha, {M. S.} and Rendle, {B. M.} and Reese, {D. R.} and K. Verma",
year = "2018",
month = "7",
doi = "10.1093/mnras/sty948",
language = "English",
volume = "477",
pages = "5052--5063",
journal = "Royal Astronomical Society. Monthly Notices",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Asteroseismic modelling of solar-type stars

T2 - internal systematics from input physics and surface correction methods

AU - Nsamba, B.

AU - Campante, T. L.

AU - Monteiro, M. J. P. F. G.

AU - Cunha, M. S.

AU - Rendle, B. M.

AU - Reese, D. R.

AU - Verma, K.

PY - 2018/7

Y1 - 2018/7

N2 - Asteroseismic forward modelling techniques are being used to determine fundamental properties (e.g. mass, radius, and age) of solar-type stars. The need to take into account all possible sources of error is of paramount importance towards a robust determination of stellar properties. We present a study of 34 solar-type stars for which high signal-to-noise asteroseismic data are available from multiyear Kepler photometry. We explore the internal systematics on the stellar properties, that is associated with the uncertainty in the input physics used to construct the stellar models. In particular, we explore the systematics arising from (i) the inclusion of the diffusion of helium and heavy elements; (ii) the uncertainty in solar metallicity mixture; and (iii) different surface correction methods used in optimization/fitting procedures. The systematics arising from comparing results of models with and without diffusion are found to be 0.5 per cent, 0.8 per cent, 2.1 per cent, and 16 per cent in mean density, radius, mass, and age, respectively. The internal systematics in age are significantly larger than the statistical uncertainties. We find the internal systematics resulting from the uncertainty in solar metallicity mixture to be 0.7 per cent in mean density, 0.5 per cent in radius, 1.4 per cent in mass, and 6.7 per cent in age. The surface correction method by Sonoi et al. and Ball & Gizon's two-term correction produce the lowest internal systematics among the different correction methods, namely, similar to 1 per cent, similar to 1 per cent, similar to 2 per cent, and similar to 8 per cent in mean density, radius, mass, and age, respectively. Stellar masses obtained using the surface correction methods by Kjeldsen et al. and Ball & Gizon's one-term correction are systematically higher than those obtained using frequency ratios.

AB - Asteroseismic forward modelling techniques are being used to determine fundamental properties (e.g. mass, radius, and age) of solar-type stars. The need to take into account all possible sources of error is of paramount importance towards a robust determination of stellar properties. We present a study of 34 solar-type stars for which high signal-to-noise asteroseismic data are available from multiyear Kepler photometry. We explore the internal systematics on the stellar properties, that is associated with the uncertainty in the input physics used to construct the stellar models. In particular, we explore the systematics arising from (i) the inclusion of the diffusion of helium and heavy elements; (ii) the uncertainty in solar metallicity mixture; and (iii) different surface correction methods used in optimization/fitting procedures. The systematics arising from comparing results of models with and without diffusion are found to be 0.5 per cent, 0.8 per cent, 2.1 per cent, and 16 per cent in mean density, radius, mass, and age, respectively. The internal systematics in age are significantly larger than the statistical uncertainties. We find the internal systematics resulting from the uncertainty in solar metallicity mixture to be 0.7 per cent in mean density, 0.5 per cent in radius, 1.4 per cent in mass, and 6.7 per cent in age. The surface correction method by Sonoi et al. and Ball & Gizon's two-term correction produce the lowest internal systematics among the different correction methods, namely, similar to 1 per cent, similar to 1 per cent, similar to 2 per cent, and similar to 8 per cent in mean density, radius, mass, and age, respectively. Stellar masses obtained using the surface correction methods by Kjeldsen et al. and Ball & Gizon's one-term correction are systematically higher than those obtained using frequency ratios.

KW - asteroseismology

KW - stars: evolution

KW - stars: fundamental parameters

KW - stars: oscillations

KW - METAL-POOR STARS

KW - OSCILLATION FREQUENCIES

KW - ELEMENT DIFFUSION

KW - HELIUM ABUNDANCE

KW - SUN

KW - EVOLUTION

KW - HELIOSEISMOLOGY

KW - OPACITIES

KW - INTERIOR

KW - MISSION

U2 - 10.1093/mnras/sty948

DO - 10.1093/mnras/sty948

M3 - Journal article

VL - 477

SP - 5052

EP - 5063

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 4

ER -