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K-GRB2@hanyang

K-GRB2@hanyang. Introduction to GRB: Classifications and Progenitors. Chang-Hwan Lee @. GRB. Introduction to GRB. Short Hard GRB. NS-NS, NS-BH Mergers. Hee-Suk Cho & Soomin Jeong’s Talk. Long Soft GRB. Supernova Association. Another class ?. Some Recent Issues. GRB. Gamma-ray Bursts.

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K-GRB2@hanyang

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  1. K-GRB2@hanyang Introduction to GRB: Classifications and Progenitors Chang-Hwan Lee @

  2. GRB Introduction to GRB Short Hard GRB NS-NS, NS-BH Mergers Hee-Suk Cho & Soomin Jeong’s Talk. Long Soft GRB Supernova Association Another class ? Some Recent Issues

  3. GRB Gamma-ray Bursts

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

  5. GRB

  6. GRB Galactic ?

  7. GRB

  8. GRB Two groups of GRBs • Short Hard Gamma-ray Bursts:Duration time < 2 secNS-NS, NS-LMBH mergers • Long-duration Gamma-ray Bursts:from spinning HMBH HMBH (High-mass black hole) 5-10 solar mass

  9. SHB Short-Hard Gamma-ray Bursts Talks by Hee-Suk Cho Soomin Jeong

  10. Short-hard GRBs SHB hard BATSE Sample • No optical counterpart (?) • Origin • Neutron star merger? • Magnetar flare? • Supernova? short long soft 0.01 1000 1

  11. SHB NS (radio pulsar) which coalesce within Hubble time (2003)(2004) (1990) (2004) (1975) (1990)(2000) Not important Globular Cluster : no binary evolution White Dwarf companion

  12. Introduction • All masses are < 1.5 M⊙ • 1534, 2127: masses are within 1% • J0737, J1756: DM = 0.1 - 0.2 M⊙

  13. SHB Short-Hard Gamma-ray Burst : Colliding NS binaries Very Important for Gravitational Waves, too Science 308 (2005) 939

  14. SHB Laser Interferometer Gravitational Wave Observatory LIGO I : in operation (since 2004) LIGO II: in progress (2010 ?)

  15. Introduction Network of Interferometers LIGO Virgo GEO TAMA LIGO Louisiana 4km AIGO

  16. L-GRB Long-duration Gamma-ray Bursts

  17. L-GRB Long-duration GRBs: Afterglow Host Galaxy Association = Distance Estimation

  18. L-GRB GRB/Supernova Association Afterglow GRB980425 SN1998bw

  19. L-GRB • Gamma-Ray Bursts are the brightest events in the Universe. • During their peak, they emit more energy than all the stars and galaxies in the Universe combined !

  20. L-GRB What caused GRB/Supernova ? Most-likely Black Holes Callapsar: Asymmetric Explosion of a Massive Star Most-likely Rapid-Rotation

  21. L-GRB How to form rapidly spinning black holes? Most likely in BH binaries (Soft X-ray Transients) Companion star can keep BH progenitor rotating Formation of rapidly rotating stellar mass BHs

  22. at birth Tidal interaction Fe rapidlyspinning BH

  23. L-GRB Q) How to generate chaotic(?) light curves ?Q) Is there a model that explains all the light curves ?

  24. L-GRB A Generic GRB Fireball UV/opt/IR/radio gamma-ray X-ray UV/optical IR mm radio gamma-ray central photosphere internal external shocks engine shocks (reverse & forward)

  25. Recent Issues

  26. Fraction of fainter or equal pixels SN GRBs are concentrated in the more bright regions of galaxy GRBs GRBs from low metallicity galaxies

  27. GRB hosts (blue color) are fainter & smaller

  28. Fruchter et al. • L-GRBs are far more conentrated in the very brightest regions of their host galaxies than core-collapse SN • Host galaxies of L-GRBs are significantly fainter and more irregular than the hosts of core-collapse SN. • L-GRB are associated with the most extremely massive stars and may be restricted to galaxies of limited chemical evolution (lower metallicity).

  29. GRB 060614 • Duration : 102 sec (Long-GRB ?) • Long-lag : Short-GRB ?(usually, short-lag : Long-GRBs) • Some pulses of GRB 060614 show no lag : consistent with Long-GRBs The existence of new class:still open questions

  30. Key Issues Classifications:Is there third or sub-classes ? Progenitors:S-GRB: NS-NS, NS-BH, …L-GRB: with SN, w/o SN, …. Properties of host galaxies & afterglow!

  31. Korean GRB Theory: -- Progenitors -- Central Engine -- Statistical Approaches Observations & Experiment -- afterglow observations (SHBs & L-GRBs) -- gamma-ray & X-ray telescope

  32. Thank you

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