Multidimensional Simulations of the Accretion-induced Collapse of White Dwarfs to Neutron Stars

By L. Dessart, Adam Burrows, Christian D. Ott, E. Livne, Sung-Chul Yoon, N. Langer. 2006

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We present 2.5-dimensional radiation-hydrodynamics simulations of the accretion-induced collapse (AIC) of white dwarfs, starting from two-dimensional rotational equilibrium configurations, thereby accounting consistently for the effects of rotation prior to and after core collapse. We focus our study on a 1.46 and a 1.92 M☉ a model. Electron capture leads to the collapse to nuclear densities of these cores a few tens of milliseconds after the start of the simulations. The shock generated at bounce moves slowly, but steadily, outward. Within 50-100 ms, the stalled shock breaks out of the white dwarf along the poles. The blast is followed by a neutrino-driven wind that develops within the white dwarf, in a cone of ~40° opening angle about the poles, with a mass loss rate of (5-8) × 10-3 M☉ s-1. The ejecta have an entropy on the order of (20-50)kB baryon-1 and an electron fraction that is bimodal. By the end of the simulations, at ≳600 ms after bounce, the explosion energy has reached (3-4) × 1049 ergs and the mass has reached a few times 10-3 M☉. We estimate the asymptotic explosion energies to be lower than 1050 ergs, significantly lower than those inferred for standard core collapse. The AIC of white dwarfs thus represents one instance where a neutrino mechanism leads undoubtedly to a successful, albeit weak, explosion. We document in detail the numerous effects of the fast rotation of the progenitors: the neutron stars are aspherical; the ``νμ'' and e neutrino luminosities are reduced compared to the νe neutrino luminosity; the deleptonized region has a butterfly shape; the neutrino flux and electron fraction depends strongly upon latitude (a la von Zeipel); and a quasi-Keplerian 0.1-0.5 M☉ accretion disk is formed.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/40bb851f469b14d850d22297e898e34977a320db

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Citations in the corpus

Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “Thus also stars below Mmas may explode as supernovae, but these events are at least a factor ten less energetic than SNe II (6 1050erg Dessart et al. 2006) and also a factor 10 smaller than SNe Ia.”
THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, background): “Rotation, Energetics and Light Curves Numerous studies (e.g., Woosley & Baron 1992; Fryer et al. 1999; Dessart et al. 2006, 2007) have shown that (at least) a low energy explosion, ∼ 1050 erg with ∼ 0.01M⊙ of 56Ni ejected, is an inevitable consequence of the accretion-induced collapse of a white…”
Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r‐process nuclei (2010, background): “…of optical absorption lines due to heavy neutron-rich elements (as in rprocess enriched halo stars; e.g. Sneden et al. 2003), which may not be present in white dwarf systems (although some rprocess nuclei may be produced in neutrino-heated winds in the case of AIC; e.g. Dessart et al. 2006).”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, methodology): “This choice of a small kick is motivated by arguments based on the pre-SN stellar structure as well as SN simulations showing that such SNe usually result in small kicks (Podsiadlowski et al. 2004; Kitaura et al. 2006; Dessart et al. 2006).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, methodology): “…mesh, our baseline calculations have typically employed 121-180 angular zones equally spaced over the entire 180◦ of the symmetry domain, and ∼160 radial shells logarithmically allocated between ∼20km (generally 10, 20, or 30 km) (Dessart et al. 2006b) and the outer radius at 6400−10000km.”
Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “As a result, the outer layers of the collapsing WD may form an accretion disk around the newly-formed NS (Dessart et al. 2006; Abdikamalov et al. 2010), the properties of which depend sensitively on the rotation rate (and the degree of differential rotation; Piro 2008) in the pre-collapse white…”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “In contrast, low-mass progenitors with ONeMg cores and iron cores are expected to explode with low energies of at most around 1050 erg (Kitaura et al. 2006; Dessart et al. 2006; Janka et al. 2012; Melson et al. 2015b).”
The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “If the collapsing white dwarf furthermore has sufficient angular momentum, an accretion disk forms around the neutron star (Michel 1987; Dessart et al. 2006).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “…spherical symmetry and a rotationally-deformed PNS emits, by von Zeipel’s law of gravity darkening, a greater neutrino flux along its rotational axis than through its equatorial regions (Janka & Moenchmeyer 1989a,b; Kotake et al. 2003; Walder et al. 2005; Buras et al. 2006a; Dessart et al. 2006b).”
Formation and evolution of compact binaries in globular clusters – II. Binaries with neutron stars (2007, background): “92 M⊙ if the ratio of the WD rotational energy to the gravitational binding energy is 0.0833 and the star is highly oblate (Dessart et al. 2006).”
ELECTRON-CAPTURE SUPERNOVAE AS THE ORIGIN OF ELEMENTS BEYOND IRON (2010, result): “This result was confirmed by Dessart et al. (2006) and excludes the prompt explosions of Hillebrandt et al. (1984).”
Short GRBs with Extended Emission from Magnetar Birth: Jet Formation and Collimation (2011, methodology): “It is thus possible that events could exist for which the extended emission is not observable because it is more collimated than the initial SGRB, in which case the event would be classified as a ‘normal’ short burst (see Barkov & 4 In such a ‘two jet’ scenario it is also unclear which jet to associ”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, methodology): “In this respect, our choice of models extends from the quasi-spherical s20.nr model, to the mildly oblate s20.π model, and finally to the strongly oblate (with a disk-like extension) AIC model.”