Title:
Observable implications and dependence on stellar and 
black hole mass of tidal disruption events, based on 
fully general relativistic hydrodynamics simulations

Abstract:
A star is tidally disrupted by a supermassive black hole 
when their separation is shorter than the so-called “tidal radius”. 
Two important characteristic scales, the tidal radius and the energy of the stellar debris, 
are often estimated on an order-of-magnitude basis without taking into account 
the star’s internal structure and relativistic effects. Since tidal disruption events occur 
at shorter distances for higher black hole mass, fully general relativistic calculations of 
tidal forces are required to study the pericenter-dependence of 
tidal disruption properties for a wide range of black hole mass. 
Using fully general relativistic hydrodynamics simulations and 
MESA-model initial conditions, we determine the physical tidal radii yielding 
full disruptions and the characteristic energy widths of the stellar debris for 
eight stellar masses (0.15 <= M_{*}/M_sol <= 10) and six black hole masses 
(10^5 <=M_{BH}/M_\sol <= 5 \times 10^7). We also find a nearly-universal relation 
between the mass remaining and the angular momentum of the star's orbit for 
partial disruptions which take place outside the physical tidal radius. 
Finally, I will discuss their observational implications for the disruption cross section 
and the peak fallback rate and time.