Conference Summary

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Conference Summary
Sorry, covering oral talks only

• SOC
• Andrzej Zdziarski, Yasuo Tanaka,
• Ramesh Narayan, Richard Mushotzky,
• Felix Mirable, Jeff McClintock,
• Karen Leighly, Katsuji Koyama,
• Rob Fender, Chris Done,
• Thomas Boller, Roger Blandford,
• Kazuo Makishima

These members have agreed to serve as the
international advisory committee for the
Grand-in-Aid for a Priority Research Area New
Development in BH Astronomy
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1 Galactic BHB ULX/IMBH

• Q1A Three basic issues of the WS S.Mineshige
• Comparative study of various BHs BHB-ULX-AGN
• Beyond the standard accretion disk.
• Formation and evolution of BHs.
• Q1B Have we understood BHB state
  classifications?
• Spectra and variability --gt mostly OK
  R.Remillard, C.Done, A.Kubota low/hard state,
  high/soft/standard state, and..
• Compton dominated (very high, or anomalous) state
• Slim disk may apply to some BHB in the outbutst
  peaks A.Kubota, ULXs A.Kubota, K.Ebisawa, and
  NLSy1 T.Kawaguchi.
• Q1C Do we see phenomena on dynamical t.s.?
• Yes, at last msec flares from Cyg X-1
  M.Gierlinski spectral changes across shots
  in Cyg X-1 and NLS1s H.Negoro
• The 102-3 sec X-ray, K-band A.Eckart, and
  radio M.Miyoshi flare from Sgr A may be, too.

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• Q1D Are ULXs and the M82 X-1 IMBHs?
• Yes, they are From luminosity A.Kubota,
  R.Mushotzky, T.Tsuru, QPO frequency
  R.Moshotzky, close similarity to Galactic
  microQSOs that are not beamed toward us
  A.Kubota, and lack of evidence for strong
  beaming Mushotzky.
• IMBHs may form in dense stellar clusters
  J.Makino, and/or as endpoints of pop-III stars
  Y.Taniguchi
• At least some ULXs, with a very cool disk
  component, are likely to be so J.Miller, A.Kong,
  R. Di Stefano.
• However
• Unlikely From evolutionary viewpoint, binary
  formation, fueling etc the Cartwheel galaxy --gt
  cannot invoke metal-poor 1st generation star A.
  King.
• ULXs may instead be mildly beamed and mildly
  super-Eddington A. King.
• Super-Eddington luminosity may be possible
  F.Meyer.
• They may represent the highest-M and highest
  M-dot end of HMXBs M.Gilfanov, K.Ebisawa.

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• Q1D continued. --- Future work TBD
• 1. Examine the degree of X-ray beaming in XRBs.
  SS433 --gt is there any evidence for radiation
  anisotropy besides relativistic Doppler with
  0.26c? microQSOs is there any evidence of
  X-ray bemaing?
• 2. Study the evolution of the most massive stars.
• 3. Search for transitions between Compton and
  standard-disk states.
• Q1F Is the too hot disk due to Kerr disk or
  slim disk?
• Slim disk preferred K.Ebisawa.
• GRO1655-40 and LMC X-3 they have very similar
  parmeters, but their disk temperatures are much
  different -- a hidden variable?

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2 Jets Theoretical/Numerical

• Q2A Is the hard X-ray emission from BHB
  significantly contributed by jets?
• Yes because jets can do everything a corona can
  H.Falcke.
• A good analogy between microQSOs and AGNs
  F.Mirabel.
• Jets are ubiquitous, particularly at low mdot A.
  Celotti.
• Low-mdot AGNs tight Lr-Lx correlation H.Falcke,
  E.Gallo.
• However
• Hard X-rays in low-state BHBs must be
  disk-dominated, because the high-energy cutoff is
  too abrupt for a synchrotron break A.Zdziarski.
• Disk-dominated AGN (Syferts, radio-quiet QSOs)
  and jet-dominated ones (radio-loud QSOs and
  Blazars) show distinct multi-band SEDs.
• A definite answer --gt X-ray polarimetry T.
  Takahashi, T.Tanimori

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• Q2B Do we have a good understanding of
  stellar-mass BH formation? --gt Probably No.
• BH formation in the dark F.Mirabel.
• Q2C Which radiatively inefficient flow do we
  expect?
• ADAF, ADIOS, CDAF, ETC, some realized in
  simulation I.Igmenshuchev JDAF H.Falcke. But
  no distinction yet.
• Q2D Is the BH spin related with jet activity?
• AGN fundamental plane Lr, Lx, mass E.Gallo
  apparently rules out the freedom for a 3rd
  parameter, but the scatter around the plane may
  be due to the BH spin.
• Disks around Kerr BHs are more strongly
  mangetized J.Krolik.
• Jets emanating from ergo sphere around a Kerr BH
  S.Koide.
• General consensus (Prograde) BH spin enhances
  jets.
• But To what extent the jet activity depends on
  the BH spin?
• Then How to observationally prove the jest vs.
  BH spin correlation?

7

• Q2F Are magnetic fields essential in accretion?
  
• Yes to specify viscosity in non ad-hoc way
  Good-bye to Alpha I.Igumenshchev, J.Hawley,
  R.Matsumoto, J. Krolik, S.Koide.
• Betagt1 in disk and betalt1 in corona J.Hawley,
  or the other way around when considering cooling
  R.Matsumoto.
• Consensus Simple hydro calculation is
  inadequate.
• But How to quantify the MHD simulation results?
  Comparing Mdot R.Matsumoto, J.Krolik --gt
  calculate emissivity.
• Q2E Are jets leptonic or hadronic?
• Still an open question A.Celloti.
• Hadronic flow may be needed to transport energy
  T. Takahashi.
• Q2G Are jets magnetically-driven of pressure
  driven?
• Jets are pressure driven (along the minimum-B
  region) but magnetically collimated J.Hawley,
  answering to Q from S.Koide.

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3 SMBHs BH formation/evolution

• 3A Various efforts of probing SMBHs

Direct imaging H.Hirabayashi, M.Miyoshi
Dynamical A.Eckert Sgr A M3.6e6 Msun
Spectroscopic M.Kishimoto
SMBH Evidence, Mass, Mdot, Spin Environment,Fuelin
g mechnanism, Outflow, etc
Historical echo K.Koyama
Time variation P.Uttley, A.Eckart
New technology is important
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3B Formation mechanism of SMBHs

• The long-lasting issue since the Reess work
• J.Makino Runaway stellar mergers --gt IMBHs --gt
  Growth due to accretion --gt Mergers in the GC
  region --gt SMBHs
• Y.Taniguchi Pop III star (z25) --gt IMBH (100
  Msun) --gt Growth of SMBH (z8) --gt Magorrian
  phase
• W.Duschl Galaxy-galaxy merger --gt SMBHs and
  fueling
• M.Umemura ULIRG -gt photon drag --gt fueling and
  growth of SMBH-- gt QSO --gt BH-mass vs. bulge
  correlation

numerical
observational
theoretical
theornum
? What provides seed BHs? Pop III or runaway
stellar mergers? ? Does the seed BH grow via
accretion? If so, how to fuel it, and how the
object appear observationally? ? Does the seed BH
grow via mergers? If so, any evidence? How to
extract angular momentum-- via GW, or by
launching helical Alfven waves?
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3C Solution to the CXB puzzle Y.Ueda

• ASCA deep survay opt.ID Chandra..
• Major contributor to CXB Lx1043.8, z0.6
• Then
• Are the results consistent with general scenario
  of AGN formation and evolution?
• Future hard X-ray deep survey, with ASTRO-E2 HXD
  to be launched in Jan/Feb. 2005

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4NLS1s Key Evidence GRB
Consensus low-M and high-mdot AGNs, but
mysterious Th.Boller, K.Leighly, Y.Tanaka,
H.Negoro, M.Guzainazzi
Q4A What produces the soft excess?

• A standard disk model can reproduce spectral
  shape, but too hot, and the apparent disk radius
  changes with kT kept constant.
• Compton e.g.,Vaughan et al, or slimm disk
  e.g.Mineshige?
• PLexponential -- Comptonized (VH) state
  M.Murashima?

Q4B The nature of G?2.5 PL with a sharp Fe-K
edge?

• The PL slope close to those seen in H or VH state
  of BHB.
• The edge feature unlikely to be reflection (no
  Fe-K emission line) due to partial covering with
  Fe-rich matter Tanaka?

• Complex spectral changes M.Guzainazzi
• Spectral changes across the shot -- similar to
  Cyg X-1 H.Negoro
• QPO-like behavior of periods 104-5 sec

Q4D How about optical properties? K.Leighly
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Q4E What is the current status of the Fe-K
lines?

• The broad Fe-K line, discovered with ASCA,
  appears to be robust, but is less variable than
  the continuum K.Iwasawa.
• The lime profile may be explained as
  relativistic broadening in accretion disks, but
  models are important K. Beckwith.
• The lack of line variability may be explained by
  a Kerr disk a ring-shaped source above it with
  varying heitht G.Miniutti.
• But what is the reality of the illuminating
  ring ?

Q4F Other key physical evidence for BHs

• Are BHCs really BHs? --gt Yes! Based on Type I
  butsts, quiescence luminosity, spectral color,
  etc. R.Narayan.
• Search for MeV thermal signals vua pion
  production T.Tanimori

GRB
N,Kawai, A.Beloborov, K.Nommoto

• Wonderful coordination among HETE-2, robotic
  telescopes, and theories.

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Thank all the conference participants, including
the invited speakers in particular. Our knowledge
horizon has expanded and swallowed all of us!
Thank LOC

• S. Mineshige, T. Tanimori, T. Tsuru,
• H. Matsumoto, H. Kubo, K. Miuchi,
• Secretaries and Graduate Students at
• Yukawa Institute and Cosmic-Ray Laboratory of
  Kyoto University