Journal
ASTROPHYSICAL JOURNAL
Volume 884, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab3b5e
Keywords
dark matter; hydrodynamics; stars: neutron; white dwarfs
Categories
Funding
- World Premier International Research Center Initiative (WPI), MEXT, Japan
- JSPS KAKENHI [JP26400222, JP16H02168, JP17K05382]
- Research Grant Council of Hong Kong [14300317]
- Endowed Research Unit (Dark Side of the universe) by Hamamatsu Photonics K.K
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Recently observed pulsars with masses similar to 1.1 M-circle dot challenge the conventional neutron star (NS) formation path by core-collapse supernova (CCSN). Using spherically symmetric hydrodynamics simulations, we follow the collapse of a massive white dwarf (WD) core triggered by electron capture, until the formation of a proto-NS (PNS). For initial WD models with the same central density, we study the effects of a static, compact dark matter (DM) admixed core on the collapse and bounce dynamics and mass of the PNS, with DM mass similar to 0.01 M-circle dot. We show that increasing the admixed DM mass generally leads to a slower collapse and smaller PNS mass, down to about 1.0 M-circle dot. Our results suggest that the accretion-induced collapse of DM admixed WDs can produce low-mass NSs, such as the observed low-mass pulsar J0453+1559, which cannot be obtained by conventional NS formation path by CCSN.
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