The Effects of Binary Evolution on the Dynamics of Core Collapse and Neutron Star Kicks

By P. Podsiadlowski, N. Langer, A. Poelarends, S. Rappaport, Alexander Heger, E. Pfahl. 2003

404 citations recorded by the source corpus.

We systematically examine how the presence in a binary affects the final core structure of a massive star and its consequences for the subsequent supernova explosion. Interactions with a companion star may change the final rate of rotation, the size of the helium core, the strength of carbon burning, and the final iron core mass. Stars with initial masses larger than ~11 M☉ that experience core collapse will generally have smaller iron cores at the point of explosion if they lost their envelopes through a binary interaction during or soon after core hydrogen burning. Stars below ~11 M☉, on the other hand, can end up with larger helium and metal cores if they have a close companion, since the second dredge-up phase that reduces the helium core mass dramatically in single stars does not occur once the hydrogen envelope is lost. We find that the initially more massive stars in binary systems with masses in the range 8-11 M☉ are likely to undergo an electron-capture supernova, while single stars in the same mass range would end as ONeMg white dwarfs. We suggest that the core collapse in an electron-capture supernova (and possibly in the case of relatively small iron cores) leads to a prompt or fast explosion rather than a very slow, delayed neutrino-driven explosion and that this naturally produces neutron stars with low-velocity kicks. This leads to a dichotomous distribution of neutron star kicks, as inferred previously, where neutron stars in relatively close binaries attain low kick velocities. We illustrate the consequences of such a dichotomous kick scenario using binary population synthesis simulations and discuss its implications. This scenario has also important consequences for the minimum initial mass of a massive star that becomes a neutron star. For single stars the critical mass may be as high as 10-12 M☉, while for close binaries it may be as low as 6-8 M☉. These critical masses depend on the treatment of convection, the amount of convective overshooting, and the metallicity of the star, and will generally be lower for larger amounts of convective overshooting and lower metallicity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/03ad32c0950b587c6d5518c4bdb43e9fb9b19aa6

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Citations in the corpus

Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, background): “…assuming that this period distribution applies for all massive binaries. d. Based on detailed evolutionary calculations of Nomoto (1984, 1987), Podsiadlowski et al. (2004) suggested that stars in binaries that develop a helium core (after case A/B Roche lobe overflow) with mass between 1.4 M…”
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…”
Evolution of massive AGB stars - II. model properties at non-solar metallicity and the fate of Super-AGB stars (2007, background): “The small mass range for which a star can evolve to EC-SN strengthens the argument developed by Podsiadlowski et al. (2004) that binarity might provide a better channel for this evolutionary path.”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, methodology): “We adopt a minimum metal core threshold of Mmin,metal = 1.37 M for a collapse (Nomoto 1984, 1987; Podsiadlowski et al. 2004; Takahashi et al. 2013).”
On the birthrates of Galactic neutron stars (2008, methodology): “…As a consistency check, we integrate the IMF to compute βCCSN = SFR〈m〉 fCCSN, (6) where 〈 m〉 is the mass expectation value and fCCSN is the fraction of stars which end their lives in a CCSN, i.e. those with initial masses in the range (11 ± 1) − 25 M (Heger et al. 2003; Podsiadlowski et al. 2004).”
Stellar-mass black holes in young massive and open stellar clusters and their role in gravitational-wave generation (2016, background): “NSs are also allowed to form via Electron Capture Supernovae (ECS; Podsiadlowski et al. 2004) as in Belczynski et al. (2008), which are of ≈ 1.26M and are as well assigned zero natal kick.”
Compact Object Modeling with the StarTrack Population Synthesis Code (2005, methodology): “We also allow for NS formation through ECS (e.g., Podsiadlowski et al. 2004).”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “Also recently detected hypervelocity stars might originate from disrupted binaries via asymmetric supernovae (SNe) with large NS kicks (Tauris 2015).”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…factor in the evolution of supernova progenitors, since it affects the distribution of key structural parameters like the helium core mass (e.g., Podsiadlowski et al. 2004) and – via the envelope structure – mixing processes during the later phases of the explosion and the observable transients.”
The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions (2012, background): “The textbook r-process source, core-collapse supernovae (SNe), have been found to be seriously challenged in providing the physical conditions (high entropy, low electron fraction together with rapid expansion) that are required to produce the heavy (A > 90) r-process elements (Fischer et al. 2010; ”
FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “The origin could either lie in strong winds of the very massive progenitor (& 30 M⊙; Chiosi & Maeder 1986; Woosley et al. 1993), sudden eruptions (Smith & Owocki 2006), interactions with a binary companion star (e.g., Nomoto et al. 1995; Podsiadlowski et al. 2004), or the interplay of all the above.”
Formation of Double Neutron Star Systems (2017, background): “Given the somewhat narrow mass window for producing EC SNe (Podsiadlowski et al. 2004), it is likely that Fe CCSNe dominate the formation rate of lowmass NSs. Detailed population synthesis studies are needed to answer this (Kruckow et al. 2017, in prep.).”
THE NEUTRON STAR MASS DISTRIBUTION (2010, background): “Therefore, while the bimodal feature found for the initial mass function (i.e. Mbirth) may be consistent with theoretical expectations for remnant masses produced by electron-capture versus Fe-core collapse SNe (Podsiadlowski et al. 2004), the evidence for a deviation of Mbirth from a unimodal distr”
Formation of millisecond pulsars with CO white dwarf companions – II. Accretion, spin-up, true ages and comparison to MSPs with He white dwarf companions (2012, background): “Stars exceeding the upper threshold mass for producing an ONeMg WD will leave behind a neutron star remnant via an electron capture supernova (Nomoto 1984; Podsiadlowski et al. 2004) or via a core-collapse supernova of type Ib/c for slightly more massive stars.”
Double neutron stars: merger rates revisited (2017, background): “All the ultra-stripped SN scenario, the double core scenario and electron-capture collapse mechanisms predict that low-kick neutron stars would form mainly (if not only) in binaries (Podsiadlowski et al. 2004; van den Heuvel 2007).”
Runaway stars as progenitors of supernovae and gamma-ray bursts (2011, background): “We note that here, we do not consider the possibility of a population of low-kick neutron stars emerging from electron-capture supernovae, as advocated by Podsiadlowski et al. (2004).”