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

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Presentation transcript:

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

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

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

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

Gravitational radiation Wave Equation Einstein Field Equation Linearized field equation

Gravitational radiation Polarization amplitude for compact binary system

 Gravitation Wave from Binary Neutron Star Effect of Gravitational Wave Radiation 1993 Nobel Prize Hulse & Taylor B Hulse & Taylor (1975) Taylor & Weisberg

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

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

Science 308 (2005) 939

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

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

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

All masses are < 1.5 M ⊙ side remark

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

Neutron Star structure

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

Initial mass transfer rate 18 M BH =3M SUN

Mass transfer time scale 19 M BH =3M SUN

Mass transfer time scale 20 Proto-neutron Kaon Quark

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

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

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

Frequency Quark Star Kaon-NS

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 !