1 / 23

Connections between NLSy 1s and Stellar BHCs

Connections between NLSy 1s and Stellar BHCs. Hitoshi Negoro Nihon University. S. Miyamoto, S. Kitamoto (BHCs) W. Brinkmann, I. Papadakis, M. Glizzio, M. Matsuoka (NLSy1s) S. Mineshige (Accretion Disk Model). BHCs v.s. NLSy1s. STATE. Properties. Very High (Slim) High/Soft

theo
Télécharger la présentation

Connections between NLSy 1s and Stellar BHCs

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Connections between NLSy 1s and Stellar BHCs Hitoshi Negoro Nihon University S. Miyamoto, S. Kitamoto (BHCs) W. Brinkmann, I. Papadakis, M. Glizzio, M. Matsuoka (NLSy1s) S. Mineshige (Accretion Disk Model)

  2. BHCs v.s. NLSy1s STATE Properties Very High (Slim) High/Soft (Intermediate) Low/Hard (Off) Very Bright Soft Excess Comptonization Rapid Time Var. Break Freq. in PSD

  3. Ancient History of Timing Studies of BHCs Nolan et al. 1981

  4. Fractal or Shots ? Cyg X-1 in the hard state (Ginga 1990)

  5. Dramatic Spectral Hardening in BHCs in the Hard State Negoro, Miyamoto & KItamoto 1994 0.2 sec

  6. Comparison with Fourier Analayses Negoro et al. 2001

  7. Current Status of Timing Studies of AGNs Ton S180 Ark 564 ASCA Edelson et al. 2002 Papadakis et al. 2002

  8. Ark 564 ASCA longest-look observation Edelson et al. 2002

  9. Ark 564 Negoro, Brinkmann, Papadakis, Gliozzi, & Matsuoka (in prep) Cross Correlation Function (CCF) of Intensity and Hardness Ratio Evidence for the BH Mass-Scaling Law ≤ 1,000 sec ~ tdyn at 3rs for 106 M Ark 564

  10. Total G ~ 2.8-3.0 Rise Phase (- average) Decay Phase (-average) G ~ 2. Two Spectral Components & Rise and Decay Phase Energy Spectra

  11. Very High State (QPO) GS1124-68 Negoro 1997 BHC in Other States Soft State Li et al. 2002

  12. Other NSLy1s ? MCG -6-30-15 Negoro et al. 1999 also Tons S180, NGC 7314

  13. Origin of the flares/Shots • flare/shot time scales (~ 105/2-5 s) >> dynamical time scales in the inner region of an Accretion Disk (< 103/1 ms) • profile independent of the peak intensity • rapid spectral hardening Local Events Local Instability Magnetic Reconnections Beaming Effect (Rotating Hot Spots)

  14. 6 r/rg Aperiodic Mass Accretion Negoro 1995 Clumping matter falling onto a BH Radial Velocity radial velocity dr/dt = - C r -1/2 released energy L = GMm/2r2 (-dr/dt) expected time variation L(t) = C’/(t - t)a Gravitational Potential

  15. Machidaet al. 2001 Fractal Function Fits L(t) = C’/(t - t)a asimple= 5/3 a ~ 1

  16. Related Theoretical Works S t Magnetic Reconnection r Manmoto et al. 1996 Machida & Matsumoto 2003

  17. Summary • Rapid Specral Hardening common to BHCs in the hard state also likely to common to NLSy1 (and Sy1 ?) direct evidence for the BH accretion disk • Origin of the Flares/Shots Advection dominated, aperiodic mass accretion onto a BH (but probably in optically thick and thin accretion disks) Magnetic reconnection occurs near the innermost radius, resulting in the rapid spectral hardening.

  18. The End

  19. Other BHCs Negoro 1998

  20. Energy Spectrum of the Shots Power Law G ~ 1.45 Comptonized BB TBB ~ 0.2 keV, Te ~ 45 keV

  21. Extended Works - QPO in the very high state • GS 1124-684

  22. Dynamic Accretion Flow Diagnostic of Accretion Disk Convection, MHD, Mass ejection… Local Fluctuations Magnetic Reconnection Plasma Instability, (Self-Organized Criticality) Summary (BHCs in the hard state)

More Related