4/5/2023 0 Comments Cassiopeia nebula![]() ![]() Optical spectra of filaments indicate a peak expansion velocity ≃1100 km s ⁻¹ with electron densities of ≤100–700 cm ⁻³ and a thick shell-like structure resembling its appearance in 22 μ m WISE images. Here we present deep optical λλ 6716,6731 images of Pa 30 that reveal an extraordinary and highly structured nebula 170″ in diameter with dozens of long (5″–20″), radially aligned filaments with a convergence point near the hot central star. Our study not only is the first-ever computation of GW from a collapsing DM object but also provides the key features to identify DM in AIC events through future GW detections.Ī newly recognized young Galactic supernova (SN) remnant, Pa 30 (G123.1+4.6), centered on a hot central star with a ∼16,000 km s ⁻¹ wind velocity, has recently been proposed to be the result of a double-degenerate merger leading to an SN Iax event associated with the guest star of 1181 CE. In the compact DM limit, the collapse dynamics of the DM in a Milky Way event generate GWs that are strong enough to be detectable by Advanced LIGO as continuous low-frequency (<1000 Hz) signals after the NM core bounce. In the diffusive DM limit, the DM admixture indirectly suppresses the post-bounce spectral peak of the NM GWs. ![]() The gravitational-wave (GW) signature from the DMAIC shows distinctive features. Thus, we demonstrate how a DM-admixed neutron star could form through DM-admixed AIC (DMAIC) for the first time, with the dynamics of DM taken into account. We find that the DM component follows the collapse of the normal matter (NM) component to become a bound DM core. We present two-dimensional hydrodynamic simulations of the accretion-induced collapse (AIC) of rotating white dwarfs admixed with an extended component of dark matter (DM) comprising sub-gigaelectronvolt degenerate fermionic DM particles. ![]()
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