The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase

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The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase. / Silva Aguirre, V.; Christensen-Dalsgaard, J.; Cassisi, S.; Miller Bertolami, M.; Serenelli, A.; Stello, D.; Weiss, A.; Angelou, G.; Jiang, C.; Lebreton, Y.; Spada, F.; Bellinger, E. P.; Deheuvels, S.; Ouazzani, R. M.; Pietrinferni, A.; Mosumgaard, J. R.; Townsend, R. H. D.; Battich, T.; Bossini, D.; Constantino, T.; Eggenberger, P.; Hekker, S.; Mazumdar, A.; Miglio, A.; Nielsen, K. B.; Salaris, M.

I: Astronomy & Astrophysics, Bind 635, A164, 03.2020.

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avisTidsskriftartikelForskningpeer review

Harvard

Silva Aguirre, V, Christensen-Dalsgaard, J, Cassisi, S, Miller Bertolami, M, Serenelli, A, Stello, D, Weiss, A, Angelou, G, Jiang, C, Lebreton, Y, Spada, F, Bellinger, EP, Deheuvels, S, Ouazzani, RM, Pietrinferni, A, Mosumgaard, JR, Townsend, RHD, Battich, T, Bossini, D, Constantino, T, Eggenberger, P, Hekker, S, Mazumdar, A, Miglio, A, Nielsen, KB & Salaris, M 2020, 'The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase', Astronomy & Astrophysics, bind 635, A164. https://doi.org/10.1051/0004-6361/201935843

APA

Silva Aguirre, V., Christensen-Dalsgaard, J., Cassisi, S., Miller Bertolami, M., Serenelli, A., Stello, D., Weiss, A., Angelou, G., Jiang, C., Lebreton, Y., Spada, F., Bellinger, E. P., Deheuvels, S., Ouazzani, R. M., Pietrinferni, A., Mosumgaard, J. R., Townsend, R. H. D., Battich, T., Bossini, D., ... Salaris, M. (2020). The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase. Astronomy & Astrophysics, 635, [A164]. https://doi.org/10.1051/0004-6361/201935843

CBE

Silva Aguirre V, Christensen-Dalsgaard J, Cassisi S, Miller Bertolami M, Serenelli A, Stello D, Weiss A, Angelou G, Jiang C, Lebreton Y, Spada F, Bellinger EP, Deheuvels S, Ouazzani RM, Pietrinferni A, Mosumgaard JR, Townsend RHD, Battich T, Bossini D, Constantino T, Eggenberger P, Hekker S, Mazumdar A, Miglio A, Nielsen KB, Salaris M. 2020. The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase. Astronomy & Astrophysics. 635:Article A164. https://doi.org/10.1051/0004-6361/201935843

MLA

Vancouver

Author

Silva Aguirre, V. ; Christensen-Dalsgaard, J. ; Cassisi, S. ; Miller Bertolami, M. ; Serenelli, A. ; Stello, D. ; Weiss, A. ; Angelou, G. ; Jiang, C. ; Lebreton, Y. ; Spada, F. ; Bellinger, E. P. ; Deheuvels, S. ; Ouazzani, R. M. ; Pietrinferni, A. ; Mosumgaard, J. R. ; Townsend, R. H. D. ; Battich, T. ; Bossini, D. ; Constantino, T. ; Eggenberger, P. ; Hekker, S. ; Mazumdar, A. ; Miglio, A. ; Nielsen, K. B. ; Salaris, M. / The Aarhus red giants challenge. I. Stellar structures in the red giant branch phase. I: Astronomy & Astrophysics. 2020 ; Bind 635.

Bibtex

@article{6de9319054274a74bb5512e35b58e2b9,
title = "The Aarhus red giants challenge.: I. Stellar structures in the red giant branch phase",
abstract = "Context. With the advent of space-based asteroseismology, determining accurate properties of red-giant stars using their observed oscillations has become the focus of many investigations due to their implications in a variety of fields in astrophysics. Stellar models are fundamental in predicting quantities such as stellar age, and their reliability critically depends on the numerical implementation of the physics at play in this evolutionary phase. Aims: We introduce the Aarhus red giants challenge, a series of detailed comparisons between widely used stellar evolution and oscillation codes that aim to establish the minimum level of uncertainties in properties of red giants arising solely from numerical implementations. We present the first set of results focusing on stellar evolution tracks and structures in the red-giant-branch (RGB) phase. Methods: Using nine state-of-the-art stellar evolution codes, we defined a set of input physics and physical constants for our calculations and calibrated the convective efficiency to a specific point on the main sequence. We produced evolutionary tracks and stellar structure models at a fixed radius along the red-giant branch for masses of 1.0 M⊙, 1.5 M⊙, 2.0 M⊙, and 2.5 M⊙, and compared the predicted stellar properties. Results: Once models have been calibrated on the main sequence, we find a residual spread in the predicted effective temperatures across all codes of ∼20 K at solar radius and ∼30-40 K in the RGB regardless of the considered stellar mass. The predicted ages show variations of 2-5% (increasing with stellar mass), which we attribute to differences in the numerical implementation of energy generation. The luminosity of the RGB-bump shows a spread of about 10% for the considered codes, which translates into magnitude differences of ∼0.1 mag in the optical V-band. We also compare the predicted [C/N] abundance ratio and find a spread of 0.1 dex or more for all considered masses. Conclusions: Our comparisons show that differences at the level of a few percent still remain in evolutionary calculations of red giants branch stars despite the use of the same input physics. These are mostly due to differences in the energy generation routines and interpolation across opacities, and they call for further investigation on these matters in the context of using properties of red giants as benchmarks for astrophysical studies. All our evolutionary calculations and models are available at http://https://github.com/vsilvagui/aarhus_RG_challenge",
keywords = "stars: evolution, stars: interiors, asteroseismology",
author = "{Silva Aguirre}, V. and J. Christensen-Dalsgaard and S. Cassisi and {Miller Bertolami}, M. and A. Serenelli and D. Stello and A. Weiss and G. Angelou and C. Jiang and Y. Lebreton and F. Spada and Bellinger, {E. P.} and S. Deheuvels and Ouazzani, {R. M.} and A. Pietrinferni and Mosumgaard, {J. R.} and Townsend, {R. H. D.} and T. Battich and D. Bossini and T. Constantino and P. Eggenberger and S. Hekker and A. Mazumdar and A. Miglio and Nielsen, {K. B.} and M. Salaris",
year = "2020",
month = mar,
doi = "10.1051/0004-6361/201935843",
language = "English",
volume = "635",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - The Aarhus red giants challenge.

T2 - I. Stellar structures in the red giant branch phase

AU - Silva Aguirre, V.

AU - Christensen-Dalsgaard, J.

AU - Cassisi, S.

AU - Miller Bertolami, M.

AU - Serenelli, A.

AU - Stello, D.

AU - Weiss, A.

AU - Angelou, G.

AU - Jiang, C.

AU - Lebreton, Y.

AU - Spada, F.

AU - Bellinger, E. P.

AU - Deheuvels, S.

AU - Ouazzani, R. M.

AU - Pietrinferni, A.

AU - Mosumgaard, J. R.

AU - Townsend, R. H. D.

AU - Battich, T.

AU - Bossini, D.

AU - Constantino, T.

AU - Eggenberger, P.

AU - Hekker, S.

AU - Mazumdar, A.

AU - Miglio, A.

AU - Nielsen, K. B.

AU - Salaris, M.

PY - 2020/3

Y1 - 2020/3

N2 - Context. With the advent of space-based asteroseismology, determining accurate properties of red-giant stars using their observed oscillations has become the focus of many investigations due to their implications in a variety of fields in astrophysics. Stellar models are fundamental in predicting quantities such as stellar age, and their reliability critically depends on the numerical implementation of the physics at play in this evolutionary phase. Aims: We introduce the Aarhus red giants challenge, a series of detailed comparisons between widely used stellar evolution and oscillation codes that aim to establish the minimum level of uncertainties in properties of red giants arising solely from numerical implementations. We present the first set of results focusing on stellar evolution tracks and structures in the red-giant-branch (RGB) phase. Methods: Using nine state-of-the-art stellar evolution codes, we defined a set of input physics and physical constants for our calculations and calibrated the convective efficiency to a specific point on the main sequence. We produced evolutionary tracks and stellar structure models at a fixed radius along the red-giant branch for masses of 1.0 M⊙, 1.5 M⊙, 2.0 M⊙, and 2.5 M⊙, and compared the predicted stellar properties. Results: Once models have been calibrated on the main sequence, we find a residual spread in the predicted effective temperatures across all codes of ∼20 K at solar radius and ∼30-40 K in the RGB regardless of the considered stellar mass. The predicted ages show variations of 2-5% (increasing with stellar mass), which we attribute to differences in the numerical implementation of energy generation. The luminosity of the RGB-bump shows a spread of about 10% for the considered codes, which translates into magnitude differences of ∼0.1 mag in the optical V-band. We also compare the predicted [C/N] abundance ratio and find a spread of 0.1 dex or more for all considered masses. Conclusions: Our comparisons show that differences at the level of a few percent still remain in evolutionary calculations of red giants branch stars despite the use of the same input physics. These are mostly due to differences in the energy generation routines and interpolation across opacities, and they call for further investigation on these matters in the context of using properties of red giants as benchmarks for astrophysical studies. All our evolutionary calculations and models are available at http://https://github.com/vsilvagui/aarhus_RG_challenge

AB - Context. With the advent of space-based asteroseismology, determining accurate properties of red-giant stars using their observed oscillations has become the focus of many investigations due to their implications in a variety of fields in astrophysics. Stellar models are fundamental in predicting quantities such as stellar age, and their reliability critically depends on the numerical implementation of the physics at play in this evolutionary phase. Aims: We introduce the Aarhus red giants challenge, a series of detailed comparisons between widely used stellar evolution and oscillation codes that aim to establish the minimum level of uncertainties in properties of red giants arising solely from numerical implementations. We present the first set of results focusing on stellar evolution tracks and structures in the red-giant-branch (RGB) phase. Methods: Using nine state-of-the-art stellar evolution codes, we defined a set of input physics and physical constants for our calculations and calibrated the convective efficiency to a specific point on the main sequence. We produced evolutionary tracks and stellar structure models at a fixed radius along the red-giant branch for masses of 1.0 M⊙, 1.5 M⊙, 2.0 M⊙, and 2.5 M⊙, and compared the predicted stellar properties. Results: Once models have been calibrated on the main sequence, we find a residual spread in the predicted effective temperatures across all codes of ∼20 K at solar radius and ∼30-40 K in the RGB regardless of the considered stellar mass. The predicted ages show variations of 2-5% (increasing with stellar mass), which we attribute to differences in the numerical implementation of energy generation. The luminosity of the RGB-bump shows a spread of about 10% for the considered codes, which translates into magnitude differences of ∼0.1 mag in the optical V-band. We also compare the predicted [C/N] abundance ratio and find a spread of 0.1 dex or more for all considered masses. Conclusions: Our comparisons show that differences at the level of a few percent still remain in evolutionary calculations of red giants branch stars despite the use of the same input physics. These are mostly due to differences in the energy generation routines and interpolation across opacities, and they call for further investigation on these matters in the context of using properties of red giants as benchmarks for astrophysical studies. All our evolutionary calculations and models are available at http://https://github.com/vsilvagui/aarhus_RG_challenge

KW - stars: evolution

KW - stars: interiors

KW - asteroseismology

U2 - 10.1051/0004-6361/201935843

DO - 10.1051/0004-6361/201935843

M3 - Journal article

VL - 635

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A164

ER -