SIS-BH workshop in Kyoto 2003

Connections between NLSy 1s and Stellar BHCs

Hitoshi NegoroNihon University

S. Miyamoto, S. Kitamoto (BHCs)W. Brinkmann, I. Papadakis, M. Glizzio, M. Matsuoka (NLSy1s)S. Mineshige (Accretion Disk Model)

SIS-BH workshop in Kyoto 2003

BHCs v.s. NLSy1s

Very High(Slim)

High/Soft(Intermediat

e)Low/Hard

(Off)

Soft Excess

Rapid Time Var.

Break Freq. in PSD

Comptonization

Very Bright

STATE Properties

SIS-BH workshop in Kyoto 2003

Ancient History of Timing Studies of BHCs

Nolan et al. 1981

SIS-BH workshop in Kyoto 2003

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

SIS-BH workshop in Kyoto 2003

Dramatic Spectral Hardening in BHCs in the Hard State

0.2 sec

Negoro, Miyamoto & KItamoto 1994

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Comparison with Fourier Analayses

Negoro et al. 2001

SIS-BH workshop in Kyoto 2003

Current Status of Timing Studies of AGNs

Edelson et al. 2002Papadakis et al. 2002

Ark 564

ASCA

Ton S180

SIS-BH workshop in Kyoto 2003

Ark 564 ASCA longest-look

observation Edelson et al. 2002

SIS-BH workshop in Kyoto 2003

Ark 564

Cross Correlation Function (CCF) of

Intensity and Hardness Ratio

Cross Correlation Function (CCF) of

Intensity and Hardness RatioEvidence for the BH Evidence for the BH

Mass-Scaling LawMass-Scaling Law

Ark 564

Negoro, Brinkmann, Papadakis, Gliozzi, & Matsuoka (in prep)

≤ 1,000 sec~ dyn at 3rs for 106 M

SIS-BH workshop in Kyoto 2003Two Spectral Components & Rise and Decay Phase Energy

Spectra

Total Rise Phase (- average)

Decay Phase (-average)

SIS-BH workshop in Kyoto 2003

BHC in Other States

Li et al. 2002

Soft State

Negoro 1997

Very High State (QPO)GS1124-68

SIS-BH workshop in Kyoto 2003

Other NSLy1s ?Negoro et al. 1999MCG -6-30-15

also Tons S180, NGC 7314

SIS-BH workshop in Kyoto 2003

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 hardeningLocal Events

Local InstabilityMagnetic ReconnectionsBeaming Effect (Rotating Hot Spots)

SIS-BH workshop in Kyoto 2003

Aperiodic Mass AccretionNegoro 1995

dr/dt = - C r -1/2

radial velocity

Clumping matter falling onto a BH

released energyL = GMm/2r2 (-dr/dt)

expected time variationL(t) = C’/( - t)

€

vr ∝ vKep ∝1 r

€

E p = −GM ˙ m

r∝−

1

r

r/rg6

Radial Velocity

Gravitational Potential

SIS-BH workshop in Kyoto 2003

Fractal Function Fits

simple = 5/3L(t) = C’/( - t)

~ 1

MachidaMachida et al. 2001et al. 2001

SIS-BH workshop in Kyoto 2003

Related Theoretical Works

Machida & Matsumoto 2003

Magnetic Reconnection

r

t

Manmoto et al. 1996

SIS-BH workshop in Kyoto 2003

Summary

• Rapid Specral Hardeningcommon to BHCs in the hard statealso likely to common to NLSy1 (and Sy1 ?)direct evidence for the BH accretion disk

• Origin of the Flares/ShotsAdvection 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.

SIS-BH workshop in Kyoto 2003

The End

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Other BHCs

Negoro 1998

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Energy Spectrum of the Shots

Comptonized BBTBB ~ 0.2 keV,Te ~ 45 keV

Power Law ~ 1.45

SIS-BH workshop in Kyoto 2003

Extended Works - QPO in the very high state

• GS 1124-684

SIS-BH workshop in Kyoto 2003

Summary (BHCs in the hard state)Dynamic Accretion FlowDiagnostic of Accretion Disk

Convection, MHD,Mass ejection…

Local FluctuationsMagnetic ReconnectionPlasma Instability,(Self-Organized Criticality)

SIS-BH workshop in Kyoto 2003