Classification of tidal disruption events by the stellar orbits
KH et al. 2017 (submitted to ApJ)
Kimi Hayasaki (CBNU) In collaboration with Shiyan Zhong1 , Shuo Li1 , Peter Berczik1, and Rainer Spurzem1,2,3 1National Astronomical Observatory China / Chinese Academy Science 2Kavli Institute for Astronomy and Astrophysics 3Astronomisches Rechen-Institut, Zentrum fu r ̈ Astronomie, University of Heidelberg, Germany Outline
1. Introduction # Tidal disruption events(TDEs)
2. Classification of TDEs by the stellar orbits # Our hypothesis # Testing it by N-body experiments 3. Summary and Discussion 1. Introduction Scientific motivation for studying TDEs
1. Probe of quiescent supermassive black holes (SMBHs) 2. Contribution to SMBH growth 3. Laboratory for super-Eddington accretion and outflow physics 4. Gravitational wave source candidates
Good phenomena for multi-messenger astronomy Tidal Disruption of a star by a SMBH
Standard Picture 1. Spread in debris energy by tidal force Rees (1988) GMbh r ⇤ ~1pc 5 ✏ = 4 rt rt 3 2. Debris specific energy 2 Stellar debris flies if ε>=0 1 away from the black hole
Parabolic orbit Stellar debris is bounded by if ε< 0 the black hole’s gravity and falls back to black hole
3. Fallback time of most tightly bound debris
2/3 1 1/2 r m Mbh t 0.1yr ⇤ ⇤ Tidal disruption radius fb ⇠ R M 106 M (Tidal force=self-gravity force): ✓ ◆ ✓ ◆ ✓ ◆ 1/3 Mbh rt = r What is the rate of mass fallback? m ⇤ ✓ ⇤ ◆ Tidal disruption radius
rS : Schwarzschild radius 2/3 M r =1.1 r bh t S 108 M ✓ ◆ 1. The condition that TDE occurs
8 rS