THE EFFECT OF STARBURST METALLICITY ON BRIGHT X-RAY BINARY FORMATION PATHWAYS

By T. Linden, Vicky Kalogera, J. Sepinsky, A. Prestwich, A. Zezas, J. Gallagher III. 2010

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We investigate the characteristics of young (<20 Myr) and bright (LX > 1 × 1036 erg s−1) high-mass X-ray binaries (HMXBs) and find the population to be strongly metallicity dependent. We separate the model populations among two distinct formation pathways: (1) systems undergoing active Roche lobe overflow (RLO) and (2) wind accretion systems with donors in the (super)giant stage, which we find to dominate the HMXB population. We find metallicity to primarily affect the number of systems which move through each formation pathway, rather than the observable parameters of systems which move through each individual pathway. We discuss the most important model parameters affecting the HMXB population at both low and high metallicities. Using these results, we show that (1) the population of ultra-luminous X-ray sources can be consistently described by very bright HMXBs which undergo stable RLO with mild super-Eddington accretion and (2) the HMXB population of the bright starburst galaxy NGC 1569 is likely dominated by one extremely metal-poor starburst cluster.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1d6a2611874a212b18c2bae474573feaf9f97b3f

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Citations in the corpus

X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, methodology): “Several XRB PS studies that usedStarTrack (Belczynski et al. 2004; Belczynski & Taam 2004; Fragos et al. 2008, 2009, 2010; Linden et al. 2009, 2010) have been pivotal in interpreting observations of nearby galaxies and showed that despite the significant number of free parameters (∼ 10) and the…”
Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries (2016, background): “This results in a more massive and more numerous black hole population (Linden et al. 2010; Fragos et al. 2013a).”
Stellar black holes at the dawn of the universe (2011, background): “Observations now support the notion that massive stars with high metal content may end as neutron stars instead of black holes (Meynet & Maeder 2005; Georgy et al. 2009; Linden et al. 2010).”
Massive black hole binaries from runaway collisions: the impact of metallicity (2016, background): “However, it is difficult that an isolated binary system composed of two massive stars evolves into a BH-BH binary with such massive BHs (e.g. Linden et al. 2010), because mass transfer and common envelope often lead to the merger of the two stars or to the loss of most of the initial mass of the…”
THE ORIGIN AND OPTICAL DEPTH OF IONIZING RADIATION IN THE “GREEN PEA” GALAXIES (2013, methodology): “16 Jaskot & Oey Ionizing Radiation in the Green Peas 17 18 Jaskot & Oey Ionizing Radiation in the Green Peas 19 20 Jaskot & Oey At a burst age of 4-5 Myr and Z = 0.2Z⊙, Linden et al. (2010) predict the formation of 5 HMXBs with X-ray luminosities greater than 1036 ergs s−1 per 106M⊙ burst.”
The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “Moreover, closely orbiting binaries are more common at lower metallicities [475], where the progenitors of GRBs are normally found (though see [476]who showed that the close binary frequency of WRs is not metallicity dependent).”
The origin of spin in binary black holes (2019, background): “This is because a greater fraction of the total post-main-sequence expansion occurs during the HG for high-metallicity stars (Linden et al. 2010).”