1. Stellar-Mass, Intermediate-Mass, Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes ー Overview ー ー Overview ー Shin Mineshige (Yukawa Institute, Kyoto) Comparative study of astrophysical BHs Beyond the standard disk model BH formation & evolution

2. 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 mass) Our Galaxynearby galaxies distant galaxies early universe 10 0 10 2 10 4 10 6 10 8 stellar-mass BHs intermediate-mass BHs (ULXs) galactic nuclei gamma-ray bursts (?) before 〜 1995after 〜 1995 (NLS1s) (unknown populations??) (c) K. Makishima (quasars) Sgr A*

3. Comparative study of astrophysical black holes If physics is common, then we expect Soft (blackbody) comp. ⇒ T eff ∝ M BH - 1/4 Hard (power-law) comp. ⇒ T ∝ M BH 0 Accretion-rate dependent evolution also in ULXs & AGNs Soft-state AGNs? Variability timescale ∝ M BH X-ray nova (XN)-type eruptions in AGN? Common physics? Fundamental differences?

4. Accretion rate-dependent evolution 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)

5. 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)

6. Variability timescale ∝ M BH ? Hayashida et al. (1998) ×10 4 ×10 6 Compare Fourier frequency at a fixed normalized PSD. Variability t.s. ∝ (r 3 /GM BH ) 1/2 ∝ M BH (r/r s ) 3/2 Such a scaling law is expected, if physics underlying variability is the same. Session 5 (10/30, morning)

7. X-ray nova type eruptions in AGN? X-ray nova type eruptions in AGN? Mineshige & Shields (ApJ 1990) Limit-cycle instability Cool disks (below 10 4 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 ・ Osaki (74), Hoshi (79), Meyer & Meyer-Hofmeister (81)

8. Beyond the standard model The standard disk model is very successful but is not an only solution. What differs in other disk models? Slim disk (near-critical accretion flow) Slim disk (near-critical accretion flow) Radiatively inefficient flow (ADAF/CDAF/MHD flow …) Radiatively inefficient flow (ADAF/CDAF/MHD flow …) Neutrino-cooled accretion flow Neutrino-cooled accretion flow

9. Various disk models Various disk models Kato, Fukue & Mineshige (1998), Narayan, Piran & Kumar (2001) standard disk : Q vis = Q rad ≫ Q adv, Q ν ADAF (CDAF): Q vis = Q adv (s gas ) ≫ Q rad, Q ν slim disk : Q vis = Q adv (s rad ) ≫ Q rad, Q ν NDAF : Q vis = Q ν ≫ Q adv, Q rad Radiation Fluid Trapped photons Grav. energy → → → Neutrinos → Q adv ～ ΣTv r (ds/dr ) = advection term Q vis = viscous heating Q rad ( Q ν ) = radiative (neutrino) cooling

10. How can we distinguish standard and slim disks? How can we distinguish standard and slim disks? Manmoto & Mineshige (in prep.) Temp. profiles T eff ∝ r -3/4 (low M) T eff ∝ r -1/2 (high M) Disk inner edge r in ～ 3r S (low M) r in ～ r S (high M) 3 rS3 rS. M/(L E /c 2 )=1,10,10 2,10 3 M BH =10 5 M sun..... Disk inner edge shifts from 3r S to ～ r S as L increases.

11. BHCs in T in - L diagram BHCs in T in - L diagram (Watarai, Mizuno, Mineshige, ApJ 549, L77, 2001) r in =const r in decreases as L increases Sessions 1 & 2 (10/28)

12. Spectral states at L ～ L Edd 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)

13. Radiatively inefficient flow (ADAF, CDAF, … ) Advection-Dominated Accretion Flow (ADAF) Low emissivity  high temp.  geometrically thick flow Convection (CDAF) Outflow (ADIOS) Magnetized (MHD) flow Low emissivity  large p gas  large p mag  enhanced mag. activity Ichimaru (1977); Abramowicz et al. (1995); Narayan & Yi (1994, 1995) 1D (radial) model 3D simulation Sessions 4 (10/29)

14. Simulation movie: magnetic-tower jet Kato, Mineshige & Shibata (2003) Sessions 3 & 4 (10/29)

15. Formation/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 objects. Evolution Cosmological growth of BHs and AGN phenominon. Co-evolution of galaxies and BHs. Were supermassive BHs generated from IMBHs?

16. Merger scenarios for forming Supermassive BHs Merger scenarios for forming Supermassive BHs (cf. Ebisuzaki et al. 2000) coutersy of T. Tsuru Sessions 6 (10/30, afternoon)

17. Cosmological evolution of AGN 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)

18. Summary: Outstanding issues 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 formation 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)

19. Organization 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: “New 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

20. From the LOC … Poster sessions Poster rooms (Room 1/2) will be available from ～ 12:00am, today 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.