no code implementations • 2 Mar 2021 • Shenghua Yu, Youjun Lu, C. Simon Jeffery
However, the majority of NS-WD binaries can avoid direct coalescence because mass transfer after contact can lead to a reversal of the orbital evolution.
High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
no code implementations • 7 Dec 2020 • Yunfeng Chen, Qingjuan Yu, Youjun Lu
The volumetric stellar tidal disruption rates are ~$3\times10^{-5}$/yr/Mpc$^3$ for MBHs in the mass range of $10^5$-$10^8$Msun at z=0; and the volumetric stellar consumption rates by MBHs with higher masses are ~$10^{-6}$/yr/Mpc$^3$, which can be the stellar tidal disruption rate if the high-mass BHs are extremely spinning Kerr BHs or the rate of being swallowed if those BHs are Schwarzschild ones.
High Energy Astrophysical Phenomena Astrophysics of Galaxies
