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07.02.27@apctp

07.02.27@apctp. Spin of Stellar Mass Black Holes: Hypernova and BH Spin Correlation in Soft X-ray BH Binaries. Chang-Hwan Lee @. Compact Stars. White Dwarf [M < 1.4 Msun; R=1000 km] Neutron Star [M < 3 Msun; R < 15 km] Black Holes. Density of Neutron Star. 1 cm 3.

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07.02.27@apctp

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  1. 07.02.27@apctp Spin of Stellar Mass Black Holes: Hypernova and BH Spin Correlation in Soft X-ray BH Binaries Chang-Hwan Lee @

  2. Compact Stars • White Dwarf [M < 1.4 Msun; R=1000 km] • Neutron Star [M < 3 Msun; R < 15 km] • Black Holes Density of Neutron Star 1 cm3 All buildings in Busan

  3. Theoretical Black Holes ? Einstein’s General Relativity Sun : r = 3 km Earch : r = 9 mm Light cannot escape ! Total Nonsense !?

  4. Observed (visible) Black Holes • Center of galaxies [106-109 Msun] • Black Hole Binaries (Soft X-ray Transients )

  5. Discovery of blackhole binaries Discovery of X-ray Binaries X-rays Mass accretion from a companion star to a compact object

  6. Sources of Strong X-ray in the Universe X-ray emission by accretion • Neutron Stars [M < 3 MSun; R <15 km] • Black Holes • … …

  7. Now we believe that black holes exist ! X-ray Observations (2002 Nobel Prize) • First Observation 1962 • First X-ray SatelliteUhuru (Dec. 1970) • .. • Current MissionsChandra (NASA) XMM-Newton (Europe) • Future Xeus (ESA), …… Chandra (NASA)

  8. BH at the Center of a galaxy (M87) Jet=100000 light year

  9. Number of X-ray Sources 1970s 1990s  1,000  50,000

  10. What is a black hole in real observation ? • Souce of strong X-ray emission • X-ray emission region is very small • No stable star exists with given mass & size 5-10 Msun Beyond Neutron Star We call it a Black Hole !

  11. Soft X-ray Transients Black Hole Binaries in our Galaxy Galactic Disk XTE J1118+480

  12. X-ray & Optical Telescopes Oscillating Brightness (GRO J1655-40)

  13. 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?

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

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

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

  17. Related Issues to be clarified • Neutrinos from hypernova • Nucleosynthesis from hypernova • Evidences of asymmetric explosions • Connection to GRBs • … …

  18. Hypernovae in BH X-ray Binaries We have seen it twice. So, does it happen everywhere? Nova Sco, V4641 Sgr

  19. Q) How can we understand the population of SXTs ? MS companion 15 10 MBH (Msun) Evolved companion 5 1 10 Orbital period (days)

  20. Evolution of BH Progenitor Progenitors • before BH Goal : At the time BH Formation • after BH • Evolution of Donor Star Current Observation

  21. before BH High Mass Black Hole progenitor (20-40 Msolar) • Bigger star evolves fast ! • High Mass Black Hole is formed when the separation is large (Case C; meet at supergiant stage) • NS/LMBH is formed when the separation is relatively small (Case A, B; meet at/before red giant stage)

  22. before BH Fe core mass Neutron Star In Close Binaries

  23. before BH Case C HMBH Case B NS/LMBH A

  24. before BH NS LMBH HMBH Formation in Case C HMBH Phase II Current 1915+105(108 Rsun)

  25. before BH Formation of Stellar Mass Black Holes Assumption • Case C Mass Transfer (in supergiant stage of BH progenitor) • If BH formation through Case B (in giant stage) is possible, contrary to the observation, we should see about 10 times more BHs in our Galaxy.

  26. At the time of BH Formation Rapidly Rotating Black Holes • Assumption: Synchronization of BH-Progenitor Spin & Binary Orbital Period • Rapidly rotating BH with large Kerr parameter (even close to 1) • SXTs with short orbital periods Possible sources of Hypernovae/GRB

  27. Marginally bound orbit Kerr Black Holes Inner disk can extend to RSch for a=1 Marginally stable orbit

  28. At the time of BH Formation • Kerr parameter (Lee et al. 2002) Preexplosion orbital period (days)

  29. BH Spin Observation Line Profile Doppler effect + Gravitational Redshifts Indication of BH spin

  30. At the time of BH Formation • Kerr parameter 4U 1543-47GRO J1655-40 Shafee et al. (2006) Preexplosion orbital period (days)

  31. At the time BH Formation Reconstructed BH Binaries at Birth BH Spin – 10000/sec HN/GRB

  32. At the time BH Formation Gamma Ray Bursts from Black Hole Systems • Energy > 1051 ergs • Rinit = O(100 km) • M < 30 Msun • dT = ms – min • …… Most likely BHs ! BH Binary is natural source of rapidly rotating black hole Energy in Hypernovae = Energy in GRBs BH Binaries -> Long-duration GRBs (> 2 sec)

  33. after BH Shrink Evolved Companion Expand MS companion I: Hubble TimeII: Main SequenceIII: Oveflow at t=0 AML: Angular Mom Loss Nu: Nuclear Burning

  34. after BH Current Observation

  35. after BH OK 15 Msun ? 10 Msun Q) How to Evolve ?

  36. after BH • Kerr parameter McClintock et al. (2006) GRS 1915+105P=33 daysa* > 0.98 4U 1543-47GRO J1655-40 Preexplosion orbital period (days)

  37. after BH Q) How to form BHs in 10-15 Msun ? • problem 1:It’s hard to form BH with masses > 10 Msun from stellar evolution. • problem 2:The current separation is too large. • Problem 3:Observed Kerr parameter is too big. • easiest solution: Accrete extra mass after BH formation

  38. after BH ?

  39. after BH Conservative Mass Transfer V4641 Sgr Data: 33.5 days 2.817 days GRS 1915+105 Consistent within error range

  40. after BH 1915+105 V4641 Sgr 15 Msun 9.5 Msun + 6.5 Msun P=3 day 10 Msun 14 Msun + 2 Msun P=33 days Beauty of Simple Physical Laws !

  41. after BH Spin-up due to accretion GRS 1915+105a* > 0.98 McClintock et al. (2006)

  42. after BH • Kerr parameter GRS 1915+105P=33 daysa* > 0.98 4U 1543-47GRO J1655-40 Preexplosion orbital period (days)

  43. At the time BH Formation Pre-Explosion Properties V4641 & 1915

  44. At the time BH Formation Reconstructed BH Binaries at Birth BH Spin – 10000/sec HN/GRB

  45. Conclusions • Soft X-ray BH binaries • Formation and evolution : - only “Case C mass transfer” can explain HMBH in binaries. • Spin of stellar-mass BHs :- tidal (BH progenitor spin-orbit) interaction is consistent with the current BH spin observation • Long-time scale GRBs and Hypernovae :- Short orbital period ( P<0.5 day) HMBH binaries are the sources of long-duration GRBs and Hypernovae

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

  47. Motivations

  48. Motivations Galactic ?

  49. Motivations

  50. Motivations • 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 !

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