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Probing Neutron Star EOS in Gravitational Waves & Gamma-ray Bursts

Explore the neutron star equations of state (EOS) using gravitational waves and gamma-ray bursts. Study neutron star binary systems and their structures, along with numerical results and comparisons between normal neutron stars and quark stars. Detect gravitational waves from various sources and examine the mass transfer process. Discuss the possibilities of probing the EOS and consider factors like spin and eccentricities of neutron star-black hole binaries.

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Probing Neutron Star EOS in Gravitational Waves & Gamma-ray Bursts

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

  2. 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

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

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

  5. Gravitational radiation Polarization amplitude for compact binary system

  6. Angle dependence Rotate axis

  7. Detection of GWR

  8. Gravitational wave from NS binary B1913+16 Hulse & Taylor (1975)  1993 Nobel Prize Cumulative shift of periastron time decay due to the effect of Gravitational Wave Radiation

  9. Sources of the GWR Compact Star binary Neutron Star-Neutron Star Neutron Star-Black Hole Black Hole-Black Hole Source of GRB ,too GRB~1051erg SN~1040erg Sun~1033erg H Bomb~1020erg Nuclear Power Plant~1015erg Light Bulb~108erg Callapsar: Woosley et al.

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

  11. Roche Lobe OverFlow Lagrangepoint M m CM Stable Mass transfer Rocheradius Roche radius =stellar radius Roche lobe “Roche lobe overflow” Orbit

  12. Neutron Star structure 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 Calculated By C.Y. Ryu @ Sungkyunkwan Univ.

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

  14. Initial mass transfer rate MBH=3MSUN X-ray binary BH-WD

  15. Mass transfer time scale MBH=3MSUN Merging time ~2 s SHB duration ~2 s

  16. Mass transfer time scale Proto-neutron Kaon Quark

  17. BH spin up BH spin energy MBH=3MSUN ergs SHB energy ergs

  18. Polarization amplitude of GW Kaon model NP model Hyperon model Quark model 2008 Nuclear Physics School

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

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

  21. 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??

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