Probing Neutron Star EOS in Gravitational Waves & Gamma-ray Bursts Kim Young-Min, Cho Hee-Suk Lee Chang.-Hwan, Park Hong-Jo (Pusan National University)

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Presentation transcript:

Probing Neutron Star EOS in Gravitational Waves & Gamma-ray Bursts Kim Young-Min, Cho Hee-Suk Lee Chang.-Hwan, Park Hong-Jo (Pusan National University) Dense Matter in Astrophysics

Contents Introduction to Gravitational Wave Radiation Neutron Star Binary System - (astrophysical part) In-Spiral & Mass Transfer(RLOF) - (dense matter part) Neutron Star Structures Numerical Result - Mass transfer time scales - Polarization amplitude of GWR in case by case - Comparison between normal NS and Quark star Conclusion & Outlook

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

Angle dependence Rotate axis

Gravitational wave from NS binary B Hulse & Taylor (1975)  1993 Nobel Prize Cumulative shift of periastron time decay due to the effect of Gravitational Wave Radiation

Sources of the GWR GRB~10 51 erg SN~10 40 erg Sun~10 33 erg H Bomb~10 20 erg Nuclear Power Plant~10 15 erg Light Bulb~10 8 erg Neutron Star-Neutron Star Neutron Star-Black Hole Black Hole-Black Hole Compact Star binary Source of GRB,too Callapsar: Woosley et al.

In-spiral ＆ Mass transfer Orbit shrinks due to the gravitational radiation Orbit increases due to the conservation of AM and mass transfer by Roche lobe over flow

Roche Lobe OverFlow Lagrange point Roche lobe Roche radius CM Orbit M m Roche radius =stellar radius Stable Mass transfer “ Roche lobe overflow ”

Neutron Star structure Calculated By C.Y. Sungkyunkwan Univ. TOV equation Nuclear matter 1) The properties of nuclear matter 2) N-N interaction 3) RMF models - Baryon octet - Kaon condensation Quark matter - MIT bag model

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

Initial mass transfer rate 14 M BH =3M SUN X-ray binary BH-WD

Mass transfer time scale 15 SHB duration ~2 s s Merging time ~2 M BH =3M SUN

Mass transfer time scale 16 Proto-neutron Kaon Quark

BH spin up 17 BH spin energy SHB energy ergs M BH =3M SUN

2008 Nuclear Physics School Kaon modelNP model Hyperon modelQuark model

Normal NS vs. Quark Star (kaon vs. quark) ~ 2 times higher Polarization amplitude(M ⊙ ) ~ 100 times quickly (After mass transfer occur) Kaon modelQuark model

Normal NS vs. Quark Star (kaon vs. quark) Frequency Quark Star Higher than Normal NS Nearly constant after mass transfer

Conclusions ＆ Outlook Possibility of probing NS EOS in GW & GRBs. (At least, may be able to exclude some EOS) Need to consider the spin & eccentricities of NS-BH binaries And something more??