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3D effects of rotation on spectroscopic observables

Published online by Cambridge University Press:  29 August 2024

Michael Abdul-Masih Open the ORCID record for Michael Abdul-Masih [Opens in a new window]
Michael Abdul-Masih*
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile
*
email: [email protected]
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Abstract

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When a star is rapidly rotating, it deviates from spherical symmetry causing non-uniform distributions of the surface gravity and temperature across the surface. These three-dimensional effects lead to an inclination dependence of many observable spectroscopic parameters, however this is often neglected when analyzing rapidly rotating systems. Using spamms, we generate synthetic spectra that account for the 3D geometry of the system and fit them with 1D models to investigate how much the 3D effects can change the derived stellar parameters. We show that these 3D effects can lead to observed temperature differences of thousands of kelvin for the same star viewed at different inclinations, and a systematic underestimation of the helium abundance.

Keywords

stars: rotationstars: fundamental parametersstars: abundancestechniques: spectroscopic
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 230 - 232
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Abdul-Masih, M., Sana, H., Conroy, K. E., Sundqvist, J., Prša, A., Kochoska, A., & Puls, J. 2020, A&A, 636, A59 10.1051/0004-6361/201937341CrossRefGoogle Scholar
Brott, I., et al. 2011, A&A, 530, A116 Google Scholar
Gräfener, G., Koesterke, L., & Hamann, W. R. 2002, A&A, 387, 244 10.1051/0004-6361:20020269CrossRefGoogle Scholar
Hillier, D. J., & Miller, D. L. 1998, ApJ, 496, 407 Google Scholar
Langer, N. 2012, ARA&A, 50, 107 10.1146/annurev-astro-081811-125534CrossRefGoogle Scholar
Maeder, A. 1987, A&A, 178, 159 Google Scholar
Prša, A., et al. 2016, ApJS, 227, 29 Google Scholar
Puls, J., Urbaneja, M. A., Venero, R., Repolust, T., Springmann, U., Jokuthy, A., & Mokiem, M. R. 2005, A&A, 435, 669 Google Scholar
von Zeipel, H. 1924, MNRAS, 84, 665 CrossRefGoogle Scholar
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