1. Cosmological Heavy Ion Collisions: Colliding Neutron Stars Chang-Hwan Lee Hee-Suk Cho Young-Min Kim Hong-Jo Park ATHIC@Tsukuba Gravitational Waves & Gamma-Ray Bursts

2. Colliding Neutron Stars M = 1.5 solar mass R < 15km A = 10^57 composed of p, n, e, hyperons, quarks, … BH

3. Contents Introduction to Gravitational Wave Radiation & Gamma-Ray Bursts Colliding Neutron Star-Black Hole System Numerical Result

4. What is the GWR? Ripples in the Fabric of the Space-Time

5. Gravitational radiation Wave Equation Einstein Field Equation Linearized field equation

6. Gravitational radiation Polarization amplitude for compact binary system

7.  Gravitation Wave from Binary Neutron Star Effect of Gravitational Wave Radiation 1993 Nobel Prize Hulse & Taylor B1913+16 Hulse & Taylor (1975) Taylor & Weisberg

8. GW Sources - NS-BH, NS-NS, BH-BH mergers - Cosmological perturbations - Supernovae, … Grav. wave pattern: “ Urgent Demand For GW Detection !!”

9. Laser Interferometer Gravitational Wave Observatory LIGO I : in operation (since 2004) LIGO II: in progress (2014)

10. Science 308 (2005) 939

11. 11 Gamma-Ray Burst Duration: milli sec - min 1970s : Vela Satellite 1990s: CGRO, Beppo- SAX 2000s: HETE-II, Swift

12. 2016/2/15  12 Short-hard GRBs  hard  soft  short  long  1000 11  0.01 No optical counterpart Origin Neutron star merg er ? Magnetar flare? Supernova?  BATSE  Sample

13. NS (radio pulsar) which coalesce within Hubble time (in our galaxy, near earth) (1975) (1990) (2003) (2004) (2004) (1990) (2000) White Dwarf companion Possible Sources for GWR & s-GRB

14. All masses are < 1.5 M ⊙ side remark

15. Wanted  Can we get some (or any) information on NS EOS (Equation of States) from GW & GRB?  NS-NS binaries : seen several  NS-BH binaries : some clues  BH-BH binaries : expected in globular clusters where old-dead stars (NS, BH) are populated. Candidates for Cosmological Heavy-Ion Collisions

16. Neutron Star structure

17. Calculated By C.Y. Ryu @ Sungkyunkwan Univ. Mass-Radius relation of Neutron Star

18. Initial mass transfer rate 18 M BH =3M SUN

19. Mass transfer time scale 19 M BH =3M SUN

20. Mass transfer time scale 20 Proto-neutron Kaon Quark

21. BH spin up (key to GRBs) 21 M BH =3M SUN

22. 2008 Nuclear Physics School  Kaon model  NP model  Hyperon model  Quark model

23. ~ 2 times high Polarization amplitude(M ⊙ ) after mass transfer ~ 100 times short Kaon model Quark model

24. Frequency Quark Star Kaon-NS

25. Prospects Colliding Neutron Stars: - Possibility of probing NS EOS in GW & GRBs. - At least, may be able to exclude some EOS. Cosmological Heavy Ion Collisions Thank you !