Density slices of the TDE simulations of 1 M _⊙ stars at ≈15 t _dyn after the pericenter passage. The arrows indicate the direction to the SMBH. We rotate the slices of the debris configurations so that the directions toward the SMBH are aligned. Top: density slices of ZAMS stars after disruption by a nonrotating SMBH with a Newtonian (first row) and a GR (second row) description of gravity. Middle: density slices of TAMS stars after disruption by a nonrotating SMBH with a Newtonian (first row) and a GR (second row) description of gravity. Bottom: density slices of ZAMS (first row) and TAMS (second row) stars after disruption by a rotating SMBH for β = 3.