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KGRB@ewha

KGRB@ewha. Introduction to GRB and Motivation of KGRB. Chang-Hwan Lee @. GRB. GRB. Introductio to GRB. Short Hard GRB. Gravitational Wave Detection. NS-NS, NS-BH Mergers. Long Soft GRB. Collapsar / Hypernova. Spin of Stellar Mass Black Holes. Another class ?. Soomin Jeong’s talk.

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KGRB@ewha

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  1. KGRB@ewha Introduction to GRB and Motivation of KGRB Chang-Hwan Lee @

  2. GRB

  3. GRB Introductio to GRB Short Hard GRB Gravitational Wave Detection NS-NS, NS-BH Mergers Long Soft GRB Collapsar / Hypernova Spin of Stellar Mass Black Holes Another class ? Soomin Jeong’s talk

  4. GRB Gamma-ray Bursts

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

  6. GRB

  7. GRB Galactic ?

  8. GRB

  9. 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

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

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

  12. L-GRB GRB/Supernova Association GRB030329/Supernova Association (z=0.2: closest GRB/Afterglow) Top 10 Scientific Achievement in 2003 [New York Times] Nature 423 (2003), 843, 844, 847 Afterglow GRB980425 SN1998bw

  13. 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 !

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

  15. 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

  16. L-GRB Discovery of X-ray BH Binaries X-rays Mass accretion from a companion star to a compact object

  17. L-GRB X-ray & Optical Telescopes Oscillating Brightness (GRO J1655-40)

  18. L-GRB Number of X-ray Sources (enough to explain GRBs) 1970s 1990s  1,000  50,000

  19. L-GRB Hypernovae in BH binaries (soft X-ray Transients)

  20. L-GRB m=2Msun ; MBH=6Msun Nova Sco 94 [Xi/H]: logarithmic abundances relative to solar Israelial et al. 1999, Nature It’s impossible for normal stars! Where did they come from?

  21. L-GRB Abundances in the secondary of Nova Sco They had to come from black hole progenitor when it exploded. Hypernova to explain the observations.

  22. L-GRB Another evidence ? C.M. System velocity (-106 km/s) : Abrupt Mass Loss by Explosion Mg,Si,S,…

  23. L-GRB Hypernova Explosions from Rotating BH Spinning BH (QPOs) High Black Hole Mass ( > 5 Msun) --- Maximum Neutron Star Mass < 2 Msun

  24. L-GRB Reconstructed BH Binaries at Birth HN/GRB BH Spin – 10000/sec

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

  26. 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) Talk by Prof. Hyun Kyu Lee

  27. SHB Short-Hard Gamma-ray Bursts

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

  29. 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

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

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

  32. SHB Short-Hard Gamma-ray Bursts (SHBs) • Observed NS-NS binaries are inconsistent with SHBs • Invisible old ( > 6 Gyr) NS binaries are responsible for short-hard gamma-ray bursts (SHBs) Nakar et al. What are the invisible old NS binaries ? Soomin Jeong’s Talk

  33. SHB Invisible NS/BH binaries by Bethe/Brown/Lee • NS/LMBH is 5 times more dominant than NS/NS due to hypercritical acctetion. • NS/LMBH will increase LIGO detection rate by factor of 10.

  34. SHB Binary Neutron Stars : Observation vs Prediction Black Holes ? Lee et al., ApJ, accepted (2007)

  35. SHB NS-WD binaries

  36. SHB Pulsar J0751+1807 2.1 ± 0.2 solar mass Nice et al., ApJ 634 (2005) 1242. Nice, talk@40 Years of Pulsar, McGill, Aug 12-17, 2007 1.26 +0.14 -0.12 solar mass Loop-hole in Bayesian analysis for WD mass

  37. SHB R0=17 Mpc (initial LIGO), 280 Mpc (advanced LIGO)

  38. SHB

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

  40. Thank you

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