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Mass Transfer Processes in the Evolution of Black Hole Binaries

2003.4.12. Chang-Hwan Lee. Mass Transfer Processes in the Evolution of Black Hole Binaries. Black Holes : Ultimate fate of dense matter. Neutron Stars ( < 2 solar mass). Q) How they are formed ?. Stellar Mass Black Holes (5-10 solar mass). Q) Are there intermediate mass BHs ?.

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Mass Transfer Processes in the Evolution of Black Hole Binaries

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  1. 2003.4.12 Chang-Hwan Lee Mass Transfer Processes in the Evolution of Black Hole Binaries

  2. Black Holes : Ultimate fate of dense matter Neutron Stars ( < 2 solar mass) Q) How they are formed ? Stellar Mass Black Holes (5-10 solar mass) Q) Are there intermediate mass BHs ? Galactic Center (106-109 solar mass)

  3. Why do we consider accretion in NS/BH ? • Accretion by Fallback after SN Explosion • SN 1987A : NS/BH was covered by material for a few years • Numerical Calculation [a few solar mass can accrete] • Accretion by Companion Star • Missing Ingredient in SN explosion • Rotation • Binary provide natural rotation by tidal interaction • NS/BH accrete matter from companion

  4. Contents • Black Holes in Soft X-ray Transients • Case C Mass Transfer • Ultraluminous X-ray Sources (ULXs) • ULXs from Soft X-ray Transients • Conclusion

  5. Soft X-ray Transients (BH+ small mass donor star) 15 Msun 10 Msun Q) How to evolve ?

  6. Ultra Luminous X-Ray Sources LEdd = 1.3 x 1038 (M/Msun) ergs/s

  7. Eddington Luminosity & Mass Accretion Rate LEdd = 1.3 x 1038 (M/Msun) erg/s Spherical Accretion L = f GMdM/R If f=1 & L=LEdd dM = dMEdd

  8. Ultraluminous X-ray Sources • Original Claim • Discovery of Intermediate Mass BH ( > 100 Msun ) • cf) dominant BH : stellar => 10 Msun • galactic => 106-109 Msun • Problem • Too Many of them • Hard to evolve them • Question: Then, what are they ?

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

  10. C HMBH NS/LMBH B A

  11. Mass gap between observed NS & BH HMBH (5-10 Msun) NS/LMBH (< 2 Msun)

  12. HMBH Formation in Case C NS LMBH HMBH Current 1915+105(108 Rsun)

  13. Soft X-ray Transients (BH+ small mass donor star) 15 Msun OK 10 Msun Q) How to evolve ?

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

  15. Soft X-ray Transients 33day 14 Msun + 2 Msun 3day 15 Msun 9.5 Msun + 6.5 Msun 10 Msun 1915+105 V4641 Sgr Beauty of Simple Physical Laws !

  16. Pre-Explosion Properties V4641 & 1915

  17. Q) How mass is transferred from Donor to Black Hole?

  18. Evolution of Donor

  19. Evolution of Donor

  20. Mass Transfer Rate from Donor to Black Hole

  21. SXTs (10 Msun BH) with evolved companions => 100 Eddington Mass Accretion Rate LLimit = N LEdd N = O(10) : Porous Disk [white dwarf] => 10 Msun BH can explain the ULXs ! LLimit = f GMdM/R f = O(0.1) : Photon Trapping dM =100dMEdd 10 Msun BH can have 10 LEdd & 100 dMEdd

  22. Ultra Luminous X-Ray Sources LLimit = 10 LEdd= 13 x 1038 (M/Msun) ergs/s

  23. SXTs with initial heavy companion ULXs (0 degree) L > 10 LEdd GRS 1915+105 (70 degree) L = LEdd 10 Msun BH + 6 Msun Companion

  24. Conclusion • HMBH formation in Case C mass transfer • ULXs may be BH binaries similar to SXTs in our Galaxy. • LLimit = 10 LEdd • We predict efficiency f=O(0.1) with photon trapping based on the evolution from V4641 Sgr to 1915+105. • dM = 100 dMEdd

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