Motivated by recent discoveries of X-ray quasi-periodic eruptions, we revisit
the collision of a black hole and an accretion disk. Assuming that they are
orbiting a supermassive black hole in orthogonal orbits, we perform a general
relativistic simulation of the collision, varying the relative velocity $V_0$
from $0.032c$ to $0.2c$ (where $c$ is the speed of light) with a variety of
disk thickness and a realistic local density profile for the disk. Our findings
indicate that the mass of the outflow matter from the disk, $m_{\rm ej}$, is
slightly less than the expected value. Nel frattempo, the typical energy associated
with this outflow $E_{\rm ej}$ is $\sim m_{\rm ej}V_0^2$. Thus, the predicted
peak luminosity from disk flares is approximately equal to the Eddington
luminosity of the black hole, whereas the peak time and duration of the flares,
which are $\propto m_{\rm ej}^{1/2}$, are shorter than that previously
believed. We also demonstrate that the property of the outflow matter induced
by the incoming and outgoing stages of the black hole collision is appreciably
different. We find that a high mass accretion rate onto the black hole from the
disk persists for a timescale of $\sim 10^6$ Schwarzschild time of the black
hole after the collision for $V_0/c \lesssim 0.1$, making this long-term
accretion onto the black hole the dominant emission process for black hole-disk
collision events. Implications of these results are discussed.

Questo articolo esplora i giri e le loro implicazioni.

Scarica PDF: