Universität zu Köln

Agrawal, Poojan ORCID: 0000-0002-1135-984X, Szecsi, Dorottya ORCID: 0000-0001-6473-7085, Stevenson, Simon ORCID: 0000-0002-6100-537X, Eldridge, Jan J. and Hurley, Jarrod (2022). Explaining the differences in massive star models from various simulations. Mon. Not. Roy. Astron. Soc., 512 (4). S. 5717 - 5726. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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Abstract

The evolution of massive stars is the basis of several astrophysical investigations, from predicting gravitational-wave event rates to studying star formation and stellar populations in clusters. However, uncertainties in massive star evolution present a significant challenge when accounting for these models' behaviour in stellar population studies. In this work, we present a comparison between five published sets of stellar models from the BPASS (Binary Population and Spectral Synthesis), BoOST (Bonn Optimized Stellar Tracks), Geneva, MIST (MESA Isochrones and Stellar Tracks), and PARSEC (PAdova and TRieste Stellar Evolution Code) simulations at near-solar metallicity. The different sets of stellar models have been computed using slightly different physical inputs in terms of mass-loss rates and internal mixing properties. Moreover, these models also employ various pragmatic methods to overcome the numerical difficulties that arise due to the presence of density inversions in the outer layers of stars more massive than 40 M-circle dot. These density inversions result from the combination of inefficient convection in the low-density envelopes of massive stars and the excess of radiative luminosity to the Eddington luminosity. We find that the ionizing radiation released by the stellar populations can change by up to 18 per cent, the maximum radial expansion of a star can differ between 100 and 1600 R-circle dot, and the mass of the stellar remnant can vary up to 20 M-circle dot between the five sets of simulations. We conclude that any attempts to explain observations that rely on the use of models of stars more massive than 40 M-circle dot should be made with caution.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Agrawal, Poojan UNSPECIFIED orcid.org/0000-0002-1135-984X UNSPECIFIED Szecsi, Dorottya UNSPECIFIED orcid.org/0000-0001-6473-7085 UNSPECIFIED Stevenson, Simon UNSPECIFIED orcid.org/0000-0002-6100-537X UNSPECIFIED Eldridge, Jan J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Hurley, Jarrod UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-684342
DOI:	10.1093/mnras/stac930
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	512
Number:	4
Page Range:	S. 5717 - 5726
Date:	2022
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language WOLF-RAYET STARS; M-CIRCLE-DOT; STELLAR EVOLUTION; LOSS RATES; PRESUPERNOVA EVOLUTION; EDDINGTON LIMIT; LUMINOUS STARS; B-STARS; O-STARS; METALLICITY Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/68434