2021
DOI: 10.1051/0004-6361/202140893
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General-relativistic instability in rapidly accreting supermassive stars: The impact of rotation

Abstract: Context. Supermassive stars (SMSs) collapsing via the general-relativistic (GR) instability are invoked as the possible progenitors of supermassive black holes. Their mass and angular momentum at the onset of the instability are key in many respects, in particular regarding the possibility for observational signatures of direct collapse. Accretion dominates the evolution of SMSs and, similar to rotation, it has been shown to impact their final properties significantly. However, the combined effect of accretion… Show more

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Cited by 20 publications
(9 citation statements)
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“…In this letter, we have assumed the evolutionary models are extremely slow rotators, but in reality, they probably evolve closer to the ΩΓ limit (Haemmerlé et al 2018). Although this would still mean they are slow rotators, even a modest rotation can affect the evolution, and more critically, the GR stability (Haemmerlé 2021b), though much is still unknown about the interplay of rotation and GR.…”
Section: Discussionmentioning
confidence: 98%
“…In this letter, we have assumed the evolutionary models are extremely slow rotators, but in reality, they probably evolve closer to the ΩΓ limit (Haemmerlé et al 2018). Although this would still mean they are slow rotators, even a modest rotation can affect the evolution, and more critically, the GR stability (Haemmerlé 2021b), though much is still unknown about the interplay of rotation and GR.…”
Section: Discussionmentioning
confidence: 98%
“…Hosokawa et al 2013; Schleicher Umeda et al 2016), these rates are too low to maintain a very extended envelope of the protostar, and it is more likely to contract on the Kelvin-Helmholtz timescale and form a supermassive star (see also Janka 2002; Begelman 2010). Such objects are expected to subsequently collapse due to the general relativistic instability, as described by Appenzeller & Fricke (1972a); Fuller et al (1986); Haemmerlé (2020Haemmerlé ( , 2021. A summary sketch of the overall scenario considered here is given in Fig.…”
Section: Formation and Evolution Of A Central Massive Objectmentioning
confidence: 94%
“…The formation of massive black holes could occur directly or through the formation of other types of progenitor objects, such as supermassive stars (e.g. Appenzeller & Fricke 1972a,b;Fuller et al 1986;Begelman 2010; Hosokawa ★ E-mail: dschleicher@astro-udec.cl Schleicher et al 2013b;Umeda et al 2016;Haemmerlé 2020Haemmerlé , 2021.…”
Section: Introductionmentioning
confidence: 99%
“…Up to this point, we have not considered the effect that an accretion envelope (Hosokawa et al 2013;Umeda et al 2016;Haemmerlé et al 2019) would have on the lightcurve. While the core of an accreting supermassive protostar has constant entropy, the envelope is thought to have entropy increasing as a power law Begelman (2010); Haemmerlé et al (2019); Haemmerlé (2020Haemmerlé ( , 2021b and this structure has been termed a hylotrope (Gk. hyle, 'matter' + tropos, 'turn') in Begelman (2010).…”
Section: With Hylotropic Envelopementioning
confidence: 99%