The evolution of runaway stellar collision products

By E. Glebbeek, E. Gaburov, Selma de Mink, O. Pols, S. P. Portegies Zwart. 2009

171 citations recorded by the source corpus.

In the cores of young dense star clusters, repeated stellar collisions involving the same object can occur. It has been suggested that this leads to the formation of an intermediate-mass black hole. To verify this scenario we compute the detailed evolution of the merger remnant of three sequences, then follow the evolution until the onset of carbon burning, and estimate the final remnant mass to determine the ultimate fate of a runaway merger sequence. We use a detailed stellar evolution code to follow the evolution of the collision product. At each collision we mix the two colliding stars, accounting for the mass loss during the collision. During the stellar evolution we apply mass-loss rates from the literature, as appropriate for the evolutionary stage of the merger remnant. We computed models for high (Z = 0.02) and low (Z = 0.001) metallicity to quantify metallicity effects. We find that the merger remnant becomes a Wolf-Rayet star before the end of core hydrogen burning. Mass loss from stellar winds dominates the mass increase due to repeated mergers for all three merger sequences that we consider. In none of our high-metallicity

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/05b777da41ebfbc58fdb81a9d245a9285b00296d

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Citations in the corpus

Formation of Supermassive Black Hole Seeds (2016, background): “…we discuss in the following sections, this mechanism strongly depends on the compactness and dynamical evolution of a stellar cluster and is particularly expected to occur in low metallicity clusters where mass loss from stellar winds is expected to be minimum (Hirschi 2007; Glebbeek et al. 2009).”
Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, methodology): “We include mass loss using the “Dutch” wind scheme with an efficiency value of 0.8 (Nieuwenhuijzen & de Jager 1990; Nugis & Lamers 2000; Vink et al. 2001; Glebbeek et al. 2009).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, methodology): “…(1975) for red giants, Bl ¨ ocker (1995) for AGB stars, de Jager et al. (1988) for a range of stars in the H-R diagram, mass loss for massive stars by Glebbeek et al. (2009), Vink et al. (2001), Nugis & Lamers (2000), and Nieuwenhuijzen & de Jager (1990), supersonic mass loss inspired by Prialnik…”
THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “We assume that a merger product efficiently loses the excess angular momentum, such that it rotates at near Keplerian rotation when it has settled to its thermal equilibrium structure (Sills et al. 2005; Glebbeek et al. 2009).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “In addition to the sub-dwarf O and B stars described above, the merged main-sequence stars exhibit properties quite unlike their single star counterparts (Glebbeek et al., 2009, 2013).”
Massive black hole binaries from runaway collisions: the impact of metallicity (2016, background): “However, only few studies consider metal-poor clusters (e.g. Glebbeek et al. 2009).”
Black-hole binaries, gravitational waves, and numerical relativity (2010, background): “IMBHs may form as the result of multiple mergers of smaller objects in the centers of dense stellar clusters in the present Universe (Miller and Colbert, 2004; Portegies Zwart and McMillan, 2002), assuming mass loss from stellar winds is not significant (Glebbeek et al., 2009).”
ON THE MAXIMUM MASS OF STELLAR BLACK HOLES (2009, background): “Stars more massive than 150M⊙ which are now being considered as possible progenitors of intermediate-mass BHs in dense star clusters are not considered (see Glebbeek et al. 2009 for an overview).”
Young Massive Star Clusters (2010, background): “…out in the recent literature, suggesting that the net growth rate, and hence the final mass of the resulting IMBH, may be much lower than suggested by purely dynamical simulations—perhaps as little as a few hundred solar masses (Yungelson et al. 2008, Glebbeek et al. 2009, Vanbeveren et al. 2009).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “For our models, mass loss for stars above 10 M uses a combination of radiative wind prescriptions, collectively called the Dutch mass loss scheme in MESA, inspired by Glebbeek et al. (2009).”
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS (2013, background): “The growth of the runaway merger product may be limited by strong stellar winds, removing the bulk of the mass and leaving a black hole of only∼ 10M⊙ for solar-metallicity stars (Glebbeek et al. 2009).”
ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “Stellar collisions in dense stellar environments (see Portegies Zwart et al. 1999) could potentially produce stars massive enough to form “heavy” BHs, but these objects are also subject to strong winds and intense mass loss unless they are stars of low metallicity (e.g., Glebbeek et al. 2009).”
THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, background): “…triggered by dynamical interactions between three bodies systems (e.g. Kozai 1962; Perets & Fabrycky 2009; Hamers et al. 2013) or as a result of (multiple) collisions in dense star clusters (Portegies Zwart et al. 2004; Glebbeek et al. 2009) or near the galactic center (Antonini et al. 2010, 2011).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, methodology): “Wind massloss is been implemented following the recipe of Glebbeek et al. (2009).”