Stellar-Mass, Intermediate-M Stellar-Mass, Intermediate-M ass, ass, and Supermassive Black Holes and Supermassive Black Holes ー ー Overview Overview ー ー Shin Mineshige (Yukawa Institute, Kyoto) • Comparative study of astrophysical BHs • Beyond the standard disk model • BH formation & evolution
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Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes ー Overview ー
Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes ー Overview ー. Shin Mineshige ( Yukawa Institute, Kyoto ). Comparative study of astrophysical BHs Beyond the standard disk model BH formation & evolution. 10 8. 10 6. 10 4. 10 2. 10 0. Black Hole Candidates. - PowerPoint PPT Presentation
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and Supermassive Black Holesand Supermassive Black Holes
ー ー Overview Overview ーー Shin Mineshige (Yukawa Institute, Kyoto)
• Comparative study of astrophysical BHs • Beyond the standard disk model• BH formation & evolution
Black Hole Candidates
BHs can be found in many places and seem to have had great influence on the evolution of the universe.
mass (solar m
ass)
Our Galaxy nearby galaxies distant galaxies early universe100
102
104
106
108
stellar-mass BHs
intermediate-mass BHs (ULXs)
galactic nuclei
gamma-ray bursts (?)
before 〜 1995 after〜 1995
(NLS1s)
(unknown populations??)
(c) K. Makishima
(quasars)
Sgr A*
Comparative study of Comparative study of astrophysical black holesastrophysical black holes
If physics is common, then we expect
Soft (blackbody) comp. ⇒ Teff ∝ MBH-1/4
Hard (power-law) comp. ⇒ T ∝ MBH0
Accretion-rate dependent evolution also in ULXs & AGNs
Soft-state AGNs?
Variability timescale ∝ MBH
X-ray nova (XN)-type eruptions in AGN?
Common physics? Fundamental differences?
Accretion rate-dependent Accretion rate-dependent evolution in X-ray binariesevolution in X-ray binaries
Similar transition in other BH objects?
Very high state
High/soft state
Intermediate state
Low/hard state
Quiescence
Esin et al. (1997)
Slim disk (+corona)
Standard disk+corona
Standard disk
ADAF/CDAF/MHD Flow
?m .
Session 1 (10/28 morning)
Soft-state AGN?Soft-state AGN?
We expect the presence of soft-state AGNs!!
(1) Standard disk solution exists for AGN parameters.
(2) Disk-corona model also predicts soft-state AGN.
Liu et al. (ApJ 572, L173, 2002; ApJ 587, 571, 2003)
Simple disk-corona model based on the analogy with solar corona Reconnection heating = Compton cooling in corona Conduction heating = evaporation cooling in chromosphere
(3) (Some of) narrow-line Sy 1s show soft-state spectra.
Session 7 (10/31 morning)
Variability timescaleVariability timescale ∝∝ MMBHBH ?? Hayashida et al. (1998)
×104
×106
Compare Fourier frequency at a fixed normalized PSD.
Variability t.s. ∝(r3/GMBH)1/2 ∝MB
H (r/rs)3/2
Such a scaling law is expected, if physics underlying variability is the same.
Session 5 (10/30, morning)
X-ray nova type eruptions in X-ray nova type eruptions in AGN?AGN? Mineshige & Shields (ApJ 1990)
Limit-cycle instability
Cool disks (below 104 K) are unstable, giving rise to quasi-periodic outbursts.
⇒ Dwarf-nova & X-ray nova eruptions
AGN disks are also unstable at ~ 0.1 pc.
⇒ Possible AGN eruptions, but no such report so far. Just missing? Or instability is somehow suppressed?