Kavli Affiliate: Rainer Spurzem
| First 5 Authors: Shiyan Zhong, Shuo Li, Peter Berczik, Rainer Spurzem,
| Summary:
Tidal disruption of stars in dense nuclear star clusters containing
supermassive central black holes (SMBH) is modeled by high-accuracy direct
N-body simulation. Stars getting too close to the SMBH are tidally disrupted
and a tidal disruption event (TDE) happens. TDEs probe properties of SMBH,
their accretion disks, and the surrounding nuclear stellar cluster. In this
paper we compare rates of full tidal disruption events (FTDE) with partial
tidal disruption events (PTDE). Since a PTDE does not destroy the star, a
leftover object emerges; we use the term ‘leftover star’ for it; two novel
effects occur in the simulation: (1) variation of the leftover star’s mass and
radius, (2) variation of the leftover star’s orbital energy. After switching on
these two effects in our simulation, the number of FTDEs is reduced by roughly
28%, and the reduction is mostly due to the ejection of the leftover stars from
PTDEs coming originally from relatively large distance. The number of PTDEs is
about 75% higher than the simple estimation given by Stone et al. (2020), and
the enhancement is mainly due to the multiple PTDEs produced by the leftover
stars residing in the diffusive regime. We compute the peak mass fallback rate
for the PTDEs and FTDEs recorded in the simulation, and find 58% of the PTDEs
have peak mass fallback rate exceeding the Eddington limit, and the number of
super-Eddington PTDEs is 2.3 times the number of super-Eddington FTDEs.
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