We present the first simulations of the tidal disruption of stars with realistic structures and compositions by massive black holes ( BHs ) .
We build stars in the stellar evolution code MESA and simulate their disruption in the 3D adaptive-mesh hydrodynamics code FLASH , using an extended Helmholtz equation of state and tracking 49 elements .
We study the disruption of a 1 M _ { \sun } star and 3 M _ { \sun } star at zero-age main sequence ( ZAMS ) , middle-age , and terminal-age main sequence ( TAMS ) .
The maximum BH mass for tidal disruption increases by a factor of \sim 2 from stellar radius changes due to MS evolution ; this is equivalent to varying BH spin from 0 to 0.75 .
The shape of the mass fallback rate curves is different from the results for polytropes of \citet 2013ApJ…767…25G .
The peak timescale t _ { peak } increases with stellar age , while the peak fallback rate \dot { M } _ { peak } decreases with age , and these effects diminish with increasing impact parameter \beta .
For a \beta = 1 disruption of a 1 M _ { \sun } star by a 10 ^ { 6 } ~ { } M _ { \sun } BH , from ZAMS to TAMS , t _ { peak } increases from 30 to 54 days , while \dot { M } _ { peak } decreases from 0.66 to 0.14 ~ { } M _ { \sun } /yr .
Compositional anomalies in nitrogen , helium , and carbon can occur before the peak timescale for disruptions of MS stars , which is in contrast to predictions from the “ frozen-in ” model .
More massive stars can show stronger anomalies at earlier times , meaning that compositional constraints can be key in determining the mass of the disrupted star .
The abundance anomalies predicted by these simulations provide a natural explanation for the spectral features and varying line strengths observed in tidal disruption events .