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 .
In the first paper ( 30 ) , 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 , focusing on the stellar mass dependence of the outcomes for a black hole of mass 10 ^ { 6 } M _ { \odot } .
We consider eight different stellar masses , from 0.15 ~ { } { M } _ { \odot } to 10 ~ { } { M } _ { \odot } .

We find that , relative to the traditional order-of-magnitude estimate r _ { t } , the physical tidal radius of low-mass stars ( M _ { \star } \lesssim 0.7 ~ { } { M } _ { \odot } ) is larger by tens of percent , while for high-mass stars ( M _ { \star } \gtrsim 1 ~ { } { M } _ { \odot } ) it is smaller by a factor 2–2.5 .
The traditional estimate of the range of energies found in the debris is \approx 1.4 \times too large 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 many stellar vibration times because the black hole ’ s tidal gravity competes with the instantaneous stellar gravity at the star ’ s surface until the star has reached a distance from the black hole \sim O ( 10 ) r _ { t } .