Formation and evolution of compact binaries in globular clusters – II. Binaries with neutron stars

By Natalia Ivanova, C. Heinke, F. Rasio, Krzysztof Belczynski, John Fregeau. 2007

226 citations recorded by the source corpus.

In this paper, the second of a series, we study the stellar dynamical and evolutionary processes leading to the formation of compact binaries containing neutron stars (NSs) in dense globular clusters. For this study, 70 dense clusters were simulated independently, with a total stellar mass ∼2 × 10 7 M� , exceeding the total mass of all dense globular clusters in our Galaxy. We find that, in order to reproduce the empirically derived formation rate of low-mass X-ray binaries (LMXBs), we must assume that NSs can be formed via electron-capture supernovae with typical natal kicks smaller than in core-collapse supernovae. Our results explain the observed dependence of the number of LMXBs on ‘collision number’ as well as the large scatter observed between different globular clusters. We predict that the number of quiescent LMXBs in different clusters should not have a strong metallicity dependence. We compare the results obtained from our simulations with the observed population of millisecond pulsars (MSPs). We find that in our cluster model the following mass-gaining events create populations of MSPs that do not match the observations (either they are inconsistent with the observed LMXB production rates, or the inferred binary periods or companion masses are not observed among radio bMSPs): (i) accretion during a common-envelope event with a NS formed through electron-capture supernovae (ECSNe), and (ii) mass transfer (MT) from a white dwarf donor. Some processes lead only to a mild recycling ‐ physical collisions or MT in a post-accretion-induced collapse system. In addition, for MSPs, we distinguish low magnetic field (long-lived) and high magnetic field (short-lived) populations, where in the latter NSs are formed as a result of accretion-induced collapse or merger-induced collapse. With this distinction and by considering only those mass-gaining events that appear to lead to NS recycling, we obtain good agreement of our models with the numbers and characteristics of observed MSPs in 47 Tuc and Terzan 5, as well as with the cumulative statistics for MSPs detected in globular clusters of different dynamical properties. We find that significant production of merging double NSs potentially detectable as short γ -ray bursts occurs only in very dense, most likely core-collapsed clusters.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/92c2195384a868a5064d1ffbd9c7d1cbc5d3f1de

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In Astronomy and Astrophysics

1. Michela Mapelli
2. N. Giacobbo
3. Ilya Mandel
4. F. Rasio
5. D. Holz
6. F. Antonini
7. Mario Spera
8. Maya Fishbach

Citations in the corpus

• Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “…et al. 1984; Heinke et al. 2005; Ivanova 2013; Giesler et al. 2018; Kremer et al. 2018a), radio (e.g., Lyne et al. 1987; Sigurdsson & Phinney 1995; Ivanova et al. 2008; Ransom 2008; Fragione et al. 2018c; Ye et al. 2019), and gravitational wave (GW) sources (e.g., Moody & Sigurdsson 2009;…”
• BLACK HOLE MERGERS AND BLUE STRAGGLERS FROM HIERARCHICAL TRIPLES FORMED IN GLOBULAR CLUSTERS (2015, unknown): “…this we set the final integration time in our simulations equal to the encounter timescale for collisions with other stars (Binney & Tremaine 1987; Ivanova et al. 2008), Tenc≈ 8.5× 1012 yrP−4/32 M −2/3 tri σ −1 10 n −1 5 × [ 1 + 913 Mtri + 〈M〉 2P 2/3 2 M 1/3 tri σ 2 10 ]−1 (12) where σ10 is the…”
• Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors (2010, background): “Dynamical interactions in globular clusters are not expected to contribute significantly to the total rate of NS-NS coalescences [42, 43] and are not included in the results in this Section.”
• Compact binaries in star clusters – I. Black hole binaries inside globular clusters (2009, result): “By contrast Ivanova et al. (2008) and Sadowski et al. (2008) have conducted studies of the compact binary population in star clusters using stellar evolution prescriptions and simplified two-zone models of cluster dynamics.”
• Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (2014, methodology): “Theoretical simulation is the only method at present (Grindlay, Portegies Zwart & McMillan 2006; Ivanova et al. 2008).”
• ACCELERATING COMPACT OBJECT MERGERS IN TRIPLE SYSTEMS WITH THE KOZAI RESONANCE: A MECHANISM FOR “PROMPT” TYPE Ia SUPERNOVAE, GAMMA-RAY BURSTS, AND OTHER EXOTICA (2010, background): “A significant fraction of such interactions would be expected to produce a stable triple systm (see MH02; Wen 2003; Ivanova 2008; Ivanova et al. 2008, 2010).”
• THE FORMATION OF ECCENTRIC COMPACT BINARY INSPIRALS AND THE ROLE OF GRAVITATIONAL WAVE EMISSION IN BINARY–SINGLE STELLAR ENCOUNTERS (2013, background): “…as their stellar composition, eccentricity, and period distributions will be largely determined by past interactions with other stars (e.g. McMillan 1991; Hut et al. 1992; Ivanova et al. 2003; Ivanova et al. 2005b; Hopman et al. 2006; Ivanova et al. 2006; Fregeau 2008; Ivanova et al. 2008, 2010).”
• The dragon simulations: globular cluster evolution with a million stars (2016, background): “Podsiadlowski et al. (2004) suggest that electron capture supernovae (ECS) can result in reduced kicks of NSs. Ivanova et al. (2008); Ivanova (2014) study the binaries with ECS NSs in GCs and find that the ratio of core collapse supernova NSs to ECS NSs could be 30− 200 to 1 in a typical GC, as…”
• Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…in stellar clusters (Kulkarni et al. 1993; Sigurdsson & Hernquist 1993; Portegies Zwart & McMillan 2000; Grindlay et al. 2006; O’Leary et al. 2006; Ivanova et al. 2008; Sadowski et al. 2008; Downing et al. 2010, 2011; Clausen et al. 2013; Ziosi et al. 2014; Rodriguez et al. 2015, 2016a; Mapelli…”
• The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, background): “…& Phinney 1993; Sigurdsson & Hernquist 1993; Sigurdsson & Phinney 1995; Phinney 1996; Colpi et al. 2003; Mapelli et al. 2005; Grindlay et al. 2006; Ivanova et al. 2008; Clausen et al. 2013; Mapelli & Zampieri 2014; Ziosi et al. 2014; Rodriguez et al. 2015, 2016; Mapelli 2016; Askar et al. 2016;…”
• COSMIC Variance in Binary Population Synthesis (2019, background): “The collapse occurs when the mass of the stellar core is > 1.38 M (Miyaji et al. 1980; Nomoto 1984, 1987; Ivanova et al. 2008).”
• Multiple populations in globular clusters (2012, background): “…Heggie et al. 2006; Trenti et al. 2007; Hurley et al. 2007; see also Heggie & Hut 2003 for a review), and as potential seeds for the formation of a variety of exotic objects (e.g. LMXBs, CVs, blue stragglers etc.; see e.g. Ivanova et al. 2006, 2008; Ferraro & Lanzoni 2008 and references therein).”
• Double neutron stars: merger rates revisited (2017, background): “Another commonly quoted argument is the retention of NS in globular clusters (Pfahl et al. 2002a; Ivanova et al. 2008).”
• DOUBLE COMPACT OBJECTS. I. THE SIGNIFICANCE OF THE COMMON ENVELOPE ON MERGER RATES (2012, background): “…dense pop- ulations in which dynamical interactions between stars are important (i.e., globular clusters) have been presented elsewhere (Gültekin et al., 2004; O’Leary et al., 2006; Grindlay et al., 2006; Sadowski et al., 2008; Ivanova et al., 2008; Downing et al., 2010; Miller & Lauburg, 2009).”
• X-RAY BINARY EVOLUTION ACROSS COSMIC TIME (2012, background): “The only PS studies to date of dynamically formed LMXBs have been done for a few specific Galactic globular clusters and only in order to identify the various formation channels and their relative importance (Ivanova et al. 2006, 2008, 2010).”
• DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES (2015, unknown): “…in which dynamical interactions between stars are important (i.e., globular clusters and galactic nuclear clusters) have been presented elsewhere (Gültekin et al. 2004; Grindlay et al. 2006; O’Leary et al. 2006; Ivanova et al. 2008; Sadowski et al. 2008; Miller & Lauburg 2009; Downing et al. 2010).”
• Eight New Millisecond Pulsars in NGC 6440 and NGC 6441 (2007, background): “The ECS scenario is particularly appealing as this type of supernova also produces small kicks, which nicely solves the problem of neutron star retention in GCs (Ivanova et al. 2007).”