Tidal disruptions of main sequence stars -- III. Stellar mass dependence of the character of partial disruptions

Understand

In this paper, the third in this series, we continue our study of tidal disruption events of main-sequence stars by a non-spinning $10^{6}~\rm{M}_\odot$ supermassive black hole.

• Here we focus on the stellar mass dependence of the outcomes of partial disruptions.
• As the encounter becomes weaker, the debris mass is increasingly concentrated near the outer edges of the energy distribution.
• As a result, the mass fallback rate can deviate substantially from a $t^{-5/3}$ power-law, becoming more like a single peak with a tail declining as $t^{-p}$ with $p\simeq2-5$.