stellar-mass, intermediate-mass, and supermassive black holes ー overview ー

　　 Stellar-Mass, Intermediate-Mass,Stellar-Mass, Intermediate-Mass,

　　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?

Σ

M・

4/34/1

2Edd

2/1

sun8

BHeff pc 1.0 /1010

(K) 2500~

r

cL

M

M

MT

Osaki (74), Hoshi (79), Meyer & Meyer-Hofmeister (81)

Beyond the standard modelBeyond the standard model

The standard disk model is very successful buThe standard disk model is very successful bu

t is not an only solution.t is not an only solution.

What differs in other disk models?What differs in other disk models?

Slim disk (near-critical accretion flow)Slim disk (near-critical accretion flow) Radiatively inefficient flow Radiatively inefficient flow 　　　　　　　　　　　　　　　　　　　　　　　　 (ADAF/CDAF/MHD flow (ADAF/CDAF/MHD flow …)…) Neutrino-cooled accretion flowNeutrino-cooled accretion flow

Various disk modelsVarious disk models

Kato, Fukue & Mineshige (1998), Narayan, Piran & Kumar

(2001)

standard disk : Qvis = Qrad ≫ Qadv , Qν 　　　　　　　　

ADAF (CDAF): Qvis = Qadv(sgas) ≫ Q rad , Qν 　

slim disk : Qvis = Qadv(srad) ≫Q rad , Qν 　　　　 　　　　 　　　　　　　

NDAF : Qvis = Qν ≫ Qadv , 　 Q rad 　

Radiation

Fluid

Trapped photons

Grav. energy

→

→

→

Neutrinos

→

Qadv ～ ΣTvr (ds/dr ) = advection term

Qvis = viscous heating

Qrad ( Qν ) = radiative (neutrino) cooling

How can we distinguish standard and How can we distinguish standard and slim disks?slim disks? Manmoto & Mineshige (in prep.)

Temp. profiles

Teff ∝ r -3/4 (low M)

Teff ∝ r -1/2 (high M)

Disk inner edge

rin ～ 3rS (low M)

rin ～ rS (high M)

3 rS

. M/(LE/c2)=1,10,102,103 　

　　　　　 MBH=105Msun

.

.

.

.

Disk inner edge shifts from 3rS to ～ rS as L increases.

BHCs inBHCs in TTinin- - LL diagram diagram (Watarai, Mizuno, Mineshige, ApJ 549, L77, 200

1)

r in=co

nst

rin decreases

as L increases

Sessions 1 & 2 (10/28)

Spectral states at Spectral states at LL ～～ LLEddEdd

Slim-disk state Blackbody-like spectra Small variability

Very high state Three spectral components:

BB + power-law + Compton. BB Large variability

High/soft state

Low/hard state

….

Apparently looks like the low-hard state.

Apparently looks like the high-soft state.

Kubota et al. (2002)

M .

Sessions 1 & 2 (10/28)

Radiatively inefficient flow Radiatively inefficient flow (ADAF, CDA(ADAF, CDAF, …)F, …)

Advection-Dominated Accretion Flow (ADAF) Low emissivity high temp. geometrically thick flow

Convection (CDAF) 　　　　

Outflow (ADIOS)

Magnetized (MHD) flow Low emissivity large pgas large pmag enhanced mag. activity

Ichimaru (1977); Abramowicz et al.

(1995); Narayan & Yi (1994, 1995)

1D (radial) model

3D simulation

Sessions 4 (10/29)

Simulation movie: magnetic-tower

jetKato, Mineshige & Shibata (2003)

Sessions 3 & 4 (10/29)

Formation/evolution of BHsFormation/evolution of BHs

Formation

SN explosion can generate a stellar-mass BH.

More massive BHs can be created either by a collapse

　 of supermassive star or merger of lower-mass object

s.

Evolution Cosmological growth of BHs and AGN phenominon. Co-evolution of galaxies and BHs.

Were supermassive BHs generated from IMBHs?

Merger scenarios for forming SuperMerger scenarios for forming Supermassive BHsmassive BHs (cf. Ebisuzaki et al. 2000)

Status at the End of Starburst Star Clusters with IMBH Sink of Star Clusters with IMBHs

into Galaxy CenterMerge of Star Clusters and

Sink of IMBHs into Galaxy Center

Merge of IMBHs into a Super Massive BH by Radiation of Gravitational Wave

67

8

9

GlobularCluster

BulgeSuper MassiveBlack Hole

Jet, Radiation

Formation of Bulge, Globular Clusters and AGN

10 QSO in Early Universe

coutersy of T. Tsuru

Sessions 6 (10/30, afternoon)

Cosmological evolution of Cosmological evolution of AGN spatial densityAGN spatial density

Number density of higher luminosity AGNs peaked at higher redshifts.

Ueda et al. (2003)

Similar evolutions are found for star-formation rates.

Sessions 6 (10/30, afternoon)

Summary:Summary: Outstanding Outstanding issuesissues

Discoveries of intermediate-mass black hole candidates prompt thorough

comparative study of different BHs.

Interesting subclass: narrow-line Seyfert 1s (NLS1s).

Recent BH observations draw even larger attention to the study of BH f

ormation and evolution processes.

Unified picture of BH accretion flows and jets is still under construction.

Multi-wavelength variability properties and theory.

Observability of general relativistic effects.

New eyes to observe astrophysical black holes.

(Session 7)

(Sessions 5 & 8)

(Session 6)

(Sessions 5 & 8)

(Sessions 3 & 4) (All sessions)

(All sessions)

Organization and SupportOrganization and Support

Organized by • Kyoto University (Dept. of Physics, Yukawa Institute)• University of Tokyo (Dept. of Physics)• ISAS

Supported by • Grant-in-aid of Monbu-Kagakushou (MEXT) in Japan: 　“ Ne

w Development in Black Hole Astronomy” (K. Makishima)

• 21 Century COE Grant of Monbu-Kagakushou (MEXT): 　 “ Center for Universality and Diversity of Physics” (K. Koyama)

• Yukawa Institute for Theoretical Physics

From the LOC…From the LOC…

Poster sessions • Poster rooms (Room 1/2) will be available from ～ 12:00am, t

oday until ～ 12:00am on the last day.• Coffee/tea service (in the afternoon break) in the poster room.

Support desk • Support desk is open until tomorrow, 5:00pm.

Other remarks • Please do not carry drinks to this event hall.• If you don’t mind, we wish to collect your presentation file after

your talk. It will be posted in the conference web-site.