Accretion Disks in AGNs
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Accretion Disks in AGNs. Omer Blaes University of California, Santa Barbara. Collaborators. Spectral Models: Shane Davis, Ivan Hubeny Numerical Simulations: Shigenobu Hirose, Neal Turner Simulation Analysis and Theory: Julian Krolik. AGNSPEC.

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Accretion Disks in AGNs

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Accretion disks in agns

Accretion Disks in AGNs

Omer Blaes

University of California, Santa Barbara


Accretion disks in agns

Collaborators

  • Spectral Models: Shane Davis, Ivan Hubeny

  • Numerical Simulations: Shigenobu Hirose, Neal Turner

  • Simulation Analysis and Theory: Julian Krolik


Accretion disks in agns

AGNSPEC

-Hubeny & Hubeny 1997, 1998; Hubeny et al. (2000, 2001)


Accretion disks in agns

  • The Good:

  • Models account for relativistic disk structure and relativistic

  • Doppler shifts, gravitational redshifts, and light bending in

  • a Kerr spacetime.

  • Models include a detailed non-LTE treatment of abundant

  • elements.

  • Models include continuum opacities due to bound-free and

  • free-free transitions, as well as Comptonization. (No lines

  • at this stage, though.)


Accretion disks in agns

  • The Bad --- Ad Hoc Assumptions:

  • Stationary, with no torque inner boundary condition.

  • RPtot with  constant with radius - determines surface

  • density.

  • Vertical structure at each radius depends only on height

  • and is symmetric about midplane.

  • Vertical distribution of dissipation per unit mass assumed

  • constant.

  • Heat is transported radiatively (and not, say, by bulk

  • motions, e.g. convection).

  • Disk is supported vertically against tidal field of black

  • hole by gas and radiation pressure only.


Accretion disks in agns

LMC X-3 in the thermal dominant state

BeppoSAX

RXTE

-Davis, Done, & Blaes (2005)

The same sort of accretion disk modeling that has been

attempted for AGN works pretty well for black hole X-ray binaries

(BHSPEC, Davis et al. 2005, Davis & Hubeny 2006).


Accretion disks in agns

Some Recent Observational Developments

That Have Direct Bearing on Our Understanding

Of Accretion Disks in AGN

Spectropolarimetry has succeeded in removing BLR, NLR,

and dust emission in the optical and infrared, revealing the

underlying broadband continuum shape for the first time

(Kishimoto’s talk later in this session).

Ton 202

-Kishimoto et al. (2004)


Accretion disks in agns

(2) Microlensing observations have now placed constraints

on the physical size of the optical continuum emitting

region in many QSO’s.

0.33

0.1

-Pooley et al. (2006)


Accretion disks in agns

-Dai et al. (2006)


Accretion disks in agns

(3) Reverberation mapping leveraged by

BLR radius/continuum luminosity correlations has given

a method of getting approximate black hole masses for

the huge number of SDSS quasars.

5100/4000

4000/2200

2200/1350

-Bonning et al. (2006)


Accretion disks in agns

5100/1350

-Bonning et al. (2006)


Accretion disks in agns

AGNSPEC

Blackbodies

-Davis et al. (2006)


Accretion disks in agns

SDSS data

(4000-2200)

(2200-1450)

AGNSPEC

AGNSPEC

With

E(B-V)=0.04

-Davis et al. (2006)


Accretion disks in agns

begone!!!

Thermodynamically consistent, radiation MHD simulations of

MRI turbulence in vertically stratified shearing boxes are telling

us a lot about the likely vertical structure of accretion disks.

Turner (2004): prad>>pgas

Hirose et al. (2006): prad<<pgas

Krolik et al. (2006): prad~pgas


Accretion disks in agns

Radiation

Magnetic

times 10

Gas


Accretion disks in agns

Expect strong (but marginally stable) thermal fluctuations at

low energy and stable (damped) fluctuations at high energy.


Accretion disks in agns

Gravity

Total

Magnetic

Radiation

Gas


Accretion disks in agns

CVI K-edge

With magnetic

fields

No magnetic

fields

-Blaes et al. (2006)


Accretion disks in agns

Photosphere

Photon Bubble

Shock Train???

Parker

Complex Structure of Surface Layers


Accretion disks in agns

Spectral Consequences

  • Magnetically supported upper layers decrease density at

  • effective photosphere, resulting in increased ionization and

  • a hardening of the spectrum.

  • Strong (up to factor 100) irregular density inhomogeneities

  • exist well beneath photosphere of horizontally averaged

  • structure. They will soften the spectrum.

  • Actual photosphere is therefore complex and irregular,

  • which will reduce intrinsic polarization of emerging photons

  • (Coleman & Shields 1990). Magnetic fields may also

  • Faraday depolarize the photons (Gnedin & Silant’ev 1978):


Accretion disks in agns

Photosphere

Parker Unstable

Regions

MRI - the source of

accretion power

Parker Unstable

Regions

Photosphere

Overall Vertical Structure of Disk with Prad~Pgas

Pmag>Prad~Pgas

Prad~Pgas>Pmag

Pmag>Prad~Pgas


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