Tidal radii of main sequence stars -- II. Simulation methodology and the
  character of full tidal disruptions
  This is the second in a series of papers presenting the results of fully
general relativistic simulations of stellar tidal disruptions in which the
stars' initial states are realistic main-sequence models. We consider eight
different stellar masses, from $0.15~{\rm M}_\odot$ to $10~{\rm M}_\odot$. In
the first paper (Ryu et al. 2019a), we gave an overview of this program and
discussed the principal observational implications of our work. Here we
describe our calculational method and provide details about the outcomes of
full disruptions. We find that, relative to the traditional order-of-magnitude
estimate $r_{\rm t}$, the physical tidal radius of low-mass stars is larger by
tens of percent, while for high-mass stars ($M_{\star} \gtrsim1~ {\rm
M}_\odot$) it is smaller by a factor $2-2.5$. The traditional estimate of the
range of energies found in the debris is approximately accurate for low-mass
stars, but is a factor $\sim 2$ too small for high-mass stars; in addition, the
energy distribution for high-mass stars has significant wings. For all stars
undergoing tidal encounters, we find that mass-loss continues for a long time
because the ${\it instantaneous}$ tidal radius, the distance out to which the
black hole's tidal gravity competes with the instantaneous stellar gravity at
the star's surface, stays comparable to the distance to the black hole until
the star has reached $O(10)~r_{\rm t}$. These findings indicate significant
failings in the popular "frozen-in" approximation.
