Ultra-stripped supernovae: progenitors and fate

By T. Tauris, N. Langer, P. Podsiadlowski. 2015

309 citations recorded by the source corpus.

The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M_sun and may explain some of the recent discoveries of weak and fast optical transients. In Tauris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ~1.5 M_sun metal cores, barely above the Chandrasekhar mass limit. Here we present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M_He = 2.5 - 3.5 M_sun in tight binaries with orbital periods of P_orb = 0.06 - 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter - as well as single - helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe, and that the amount of helium ejected is correlated with P_orb - the tightest systems even having donors being stripped down to envelopes of less than 0.01 M_sun. We estimate the rise time of ultra-stripped SNe to be in the range 12 hr - 8 days, and light curve decay times between 1 and 50 days. Ultra-stripped SNe may produce NSs in the mass range 1.10 - 1.80 M_sun and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth. [Abridged]

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0f2b7ac33182baaa16e9efb9e582f46661653e4e

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Citations in the corpus

The Evolution of Massive Helium Stars, Including Mass Loss (2019, methodology): “For 8 now, we adopt an upper bound to the stars that make white dwarfs of 2.4 M (see also Tauris et al. 2015).”
COSMIC Variance in Binary Population Synthesis (2019, methodology): “For progenitors of DNSs, detailed modeling of this phase finds that mass transfer typically proceeds stably (Ivanova et al. 2003; Tauris et al. 2013, 2015) and does not lead to the onset of a CE.”
Double neutron stars: merger rates revisited (2017, background): “A number of authors suggested that there should be a connection between the magnitude of the kick and the mass of the ejected material, mass of the remnant NS and/or mass of the collapsing core (Jones et al. 2013; Tauris et al. 2015; Beniamini & Piran 2016; Bray & Eldridge 2016; Janka 2017).”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, methodology): “For helium stars with ZAMS masses up to 3.5 M and evolving to the stage of Case BB RLO with a compact object accretor (i.e. post-HMXB/CE evolution), ComBinE uses the recent results of (Tauris et al. 2015) to determine their evolution.”
The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, background): “50 km s−1, when the SN is ultra-stripped (Tauris et al. 2013, 2015; Bray & Eldridge 2016).”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, background): “We do not explicitly distinguish between electron capture and iron ccSN (e.g., Tauris et al. 2015).”
PULSAR J0453+1559: A DOUBLE NEUTRON STAR SYSTEM WITH A LARGE MASS ASYMMETRY (2015, background): “It is possible that the companion formed instead in an iron core collapse SN, where the core of the progenitor of the companion was stripped of its envelope (Tauris et al. 2015).”
Formation of Double Neutron Star Systems (2017, methodology): “Therefore, as discussed previously, the HMXBs are bound to become dynamically unstable upon efficient accretion (delayed-dynamical instability (DDI), Hjellming & Webbink 1987) — unless assuming some (most likely unrealistic) very large value of the wind-mass loss rate exceeding the rate at which mat”
Rates of compact object coalescences (2021, background): “…helium star progenitors of neutron stars may re-expand after the helium main sequence, engage in another mass transfer episode (case BB mass transfer) and ultimately explode in very weak ultra-stripped supernovae with greatly reduced kicks (Tauris et al., 2015, but see Mandel and Müller 2020).”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “5 (Tauris et al. 2015) are examples for ultra-stripped progenitors that can evolve from the companion star in high-mass X-ray binary (HMXB) systems which undergo common-envelope (CE) evolution followed by an additional (so-called Case BB) mass-transfer episode (Tauris et al. 2013, 2015, 2017).”
Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long-duration Gamma-Ray Bursts (2017, background): “…of FRB 121102 with a young pulsar embedded in the low mass ejecta of an “ultra-stripped” hydrogen-poor supernova (e.g. Kleiser & Kasen 2014; Tauris et al. 2015), a model that has been previously invoked to explain the observed population of fast-evolving Type Ic SNe (e.g. Drout et al.…”
The effect of the metallicity-specific star formation history on double compact object mergers (2019, background): “If the progenitor either experiences an electron capture supernova or is ultrastripped by an NS companion, we lower the 1D root mean square kick to 30 km s−1 (Pfahl et al. 2002; Podsiadlowski et al. 2004; Tauris et al. 2015, 2017; VignaGómez et al. 2018).”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “…several works (Scheck et al. 2006; Wongwathanarat et al. 2013; Suwa et al. 2015; Gessner 2014; Gessner & Janka 2017) and back up hypothetical low-kick scenarios discussed in the literature involving electron-capture and ultra-stripped SNe (Podsiadlowski et al. 2004; Tauris et al. 2013, 2015, 2016).”
Merging black holes in young star clusters (2019, background): “…al. 2007, 2008; Bogomazov et al. 2007; Moody & Sigurdsson 2009; Dominik et al. 2012, 2013, 2015; Mapelli et al. 2013; Mennekens & Vanbeveren 2014; Tauris et al. 2015, 2017; de Mink & Belczynski 2015; de Mink & Mandel 2016; Marchant et al. 2016; Belczynski et al. 2016a; Chruslinska et al. 2018;…”
An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients (2018, background): “…linked to electron-capture SNe (ecSNe; e.g., Miyaji et al. 1980; Nomoto et al. 1982), rather than an ultrastripped massive star explosion (e.g., Tauris et al. 2015). ecSNe are expected to originate from progenitors with mass ∼8–10M☉ and are predicted to have low explosion energy Ek∼10 50 erg,…”