2019
DOI: 10.3847/1538-4357/ab3640
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Accretion-induced Collapse of Dark Matter Admixed White Dwarfs. II. Rotation and Gravitational-wave Signals

Abstract: We present axisymmetric hydrodynamical simulations of accretion-induced collapse (AIC) of dark matter (DM) admixed rotating white dwarfs (WD) and their burst gravitational-wave (GW) signals. For initial WD models with the same central baryon density, the admixed DM is found to delay the plunge and bounce phases of AIC, and decrease the central density and mass of the proto-neutron star (PNS) produced. The bounce time, central density and PNS mass generally depend on two parameters, the admixed DM mass M DM and… Show more

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Cited by 11 publications
(19 citation statements)
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References 78 publications
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“…Studies on the equilibrium structures of non-self-interacting DM-admixed neutron stars provided hints to search for DM from the neutron star diversities (Leung et al 2011;Ellis et al 2018). Ongoing studies have been focusing on different aspects of compact objects, including bosonic DM stars (Eby et al 2016;Lee et al 2021, in preparation), formation of neutron stars through the accretioninduced collapse of DM-admixed white dwarfs (WDs; Leung et al 2019;Zha et al 2019), tidal properties of DM-admixed neutron stars (Leung et al 2021, in preparation), thermalization of the WD core to produce a thermonuclear runaway (Bramante 2015;Acevedo & Bramante 2019;Janish et al 2019;Steigerwald et al 2019), and thermonuclear supernovae with point-mass DM cores (Leung et al 2015a). Other than compact objects, effects of DM admixture on stellar formation (Arun et al 2019) and evolution (Scott et al 2008;Freese et al 2016;Lopes & Lopes 2019) are actively investigated.…”
Section: Dm-admixed Stellar Objectsmentioning
confidence: 99%
“…Studies on the equilibrium structures of non-self-interacting DM-admixed neutron stars provided hints to search for DM from the neutron star diversities (Leung et al 2011;Ellis et al 2018). Ongoing studies have been focusing on different aspects of compact objects, including bosonic DM stars (Eby et al 2016;Lee et al 2021, in preparation), formation of neutron stars through the accretioninduced collapse of DM-admixed white dwarfs (WDs; Leung et al 2019;Zha et al 2019), tidal properties of DM-admixed neutron stars (Leung et al 2021, in preparation), thermalization of the WD core to produce a thermonuclear runaway (Bramante 2015;Acevedo & Bramante 2019;Janish et al 2019;Steigerwald et al 2019), and thermonuclear supernovae with point-mass DM cores (Leung et al 2015a). Other than compact objects, effects of DM admixture on stellar formation (Arun et al 2019) and evolution (Scott et al 2008;Freese et al 2016;Lopes & Lopes 2019) are actively investigated.…”
Section: Dm-admixed Stellar Objectsmentioning
confidence: 99%
“…We use a two-dimensional hydrodynamics code that we previously used extensively for SN simulations. The code is designed for multiple purposes and has been used in simulations of Type Ia SNe (Leung et al 2015;Leung & Nomoto 2018, electron capture SNe (Leung & Nomoto 2017Zha et al 2019b; and accretion-induced collapse (Leung et al 2019b;Zha et al 2019a). The code utilizes the fifth-order shock-capturing weighted essentially non-oscillatory (WENO) scheme (Barth & Deconinck 1999) and the five-step third-order non-strongstability-preserving Runge-Kutta scheme for time discretization (Wang & Spiteri 2007) of the Euler equations.…”
Section: Hydrodynamicsmentioning
confidence: 99%
“…Although its exact value is not clear [184], the typical runaway density should be ∼ 10 10 g cm −3 [185,186]. A critical density of a few times of 10 10 g cm −3 has also been adopted in multi-dimensional simulations of rotating collapse [124,125].…”
Section: Resultsmentioning
confidence: 99%
“…This gives rise to another possible explanation of the origin of the 2.6 M compact object. The AIC of a rapidly rotating WD [187,188] and a rotating WD admixed with a point DM [184,189] have been numerically investigated. It will be an interesting future research to analyze the possibilities of forming a 2.6 M DM-admixed rotating neutron star through multidimensional simulations.…”
Section: Resultsmentioning
confidence: 99%