1. Multi-Messenger Astronomy of Tidal Stellar Pablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA Amaldi 11, Gwangju, Korea June 23, 2015

2. The Transient Sky van Velzen et al. 2011, ApJ, 741, 73 If TDEs, we will learn about Demographics of MBHs in quiescent galaxies Constraints on low mass galaxies hosting MBHs Growth of MBHS by accreting gas at super- Eddington rates Stellar dynamics in the neighborhood of MBH SN, GRBs, AGN or could they be TDEs? t -5/3

3. Tidal Forces and Radius Penetration Factor White Dwarf Main Sequence Black Hole Orbital Plane Star Tidal Radius

4. The Disruption of a Star: What to Look For Injection Disruption & Compression Fallback & Disk Formation Ejecta Near periapsis, the star disrupts and compresses with detonation, multiple bounces, and gravitational waves a possible outcome. Fallback material yields an accretion disk (soft x-rays), with super-Eddignton outflows (optical/UV) and relativistic jets (radio/x-rays) Unbound material could also yield emission lines if irradiated by the disk

5. Tidal Compression Carter & Luminet 1993 Haas, Shcherbakov, Bode, PL Black Hole Orbital Plane Star

6. Fallback & Disk Formation Rees 1988 Evans and Kochanek 89 Haas et al 2012Guillochon et al

7. TDEs with Prompt Accretion Evans, Laguna & Eracleous, ApJL 2015

8. Gravitational Waves from Star-BH System Kobayashi, Laguna, Meszaros & Phinney 2004

9. Gravitational Waves from Star Compression Black Hole Orbital Plane Star Guillichon et al 2008; Stone et al 2012

10. Summary  Early accretion, outflow and fallback rate will tell us about the BH’s spin  TDEs with prompt accretion will help identifying IMBH  Magnetic fields could provided models of jetted TDEs  TDEs of WD by IMBH are potentially good candidates for multi-messenger observations