Using a suite of fully relativistic hydrodynamic simulations applied to main-sequence stars with realistic internal density profiles , we examine full and partial tidal disruptions across a wide range of black hole mass ( 10 ^ { 5 } \leq M _ { BH } / \mathrm { M } _ { \odot } \leq 5 \times 10 ^ { 7 } ) and stellar mass ( 0.3 \leq M _ { \star } / \mathrm { M } _ { \odot } \leq 3 ) as larger M _ { BH } leads to stronger relativistic effects .
For fixed M _ { \star } , as M _ { BH } increases , the ratio of the maximum pericenter distance yielding full disruptions ( \cal { R } _ { t } ) to its Newtonian prediction rises rapidly , becoming triple the Newtonian value for M _ { BH } = 5 \times 10 ^ { 7 } ~ { } { M } _ { \odot } , while the ratio of the energy width of the stellar debris for full disruptions to the Newtonian prediction decreases steeply , resulting in a factor of two correction at M _ { BH } = 5 \times 10 ^ { 7 } ~ { } { M } _ { \odot } .
We find that for partial disruptions , the fractional remnant mass for a given ratio of the pericenter to \cal { R } _ { t } is higher for larger M _ { BH } .

These results have several implications .
As M _ { BH } increases above \sim 10 ^ { 7 } ~ { } { M } _ { \odot } , the cross section for complete disruptions is suppressed by competition with direct capture .
However , the cross section ratio for partial to complete disruptions depends only weakly on M _ { BH } .
The relativistic correction to the debris energy width delays the time of peak mass-return rate and diminishes the magnitude of the peak return rate .
For M _ { BH } \gtrsim 10 ^ { 7 } ~ { } { M } _ { \odot } , the M _ { BH } -dependence of the full disruption cross section and the peak mass-return rate and time is influenced more by relativistic effects than by Newtonian dynamics .