Collaborating with

A. Pierens, J.M. Hure (Meudon Observatory)

C. Matsumoto, K.M. Leighly (Univ. of Oklahoma, USA)

Radiation Spectra from Super-Eddington Active Galctic Nuclei

Toshihiro KAWAGUCHI (Meudon Observatory, France)

1. Introduction to Super Eddington accretion:

2. Latest disc model 1: Vicinity of Black Hole (< 100 RSch)

3. Latest disc model 2: Outer region (~ 104 RSch)

4. Spectral fit to Narrow Line Seyfert 1 galaxies

5. Summary

Optically Thick, Advection Dominated Flow with M >> LEdd/c2

•Begelman & Meier (1982)– t(accretion) >> t(diffusion)

(M < LEdd/c2)

– t(accretion) << t(diffusion)

“Photon Trapping”

(M >> LEdd/c

2)

•Abramowicz et al. (1988)

– L < several x LEdd

– Flow shines

even inside 3 x RSch

～

～

Radius (RSCH)

1-3. Models of super-Eddington accretion:

(Kawaguchi 2003)

~

2-1. Effects of Comptonization: y*

⇒ Comptonization in slim d

isks [Mdot/(LEdd/c2) >> 1] is muc

h more important than that

in standard disks

[Mdot/(LEdd/c2) < 10].~

Spectral distortion due to electron scattering

M / (LEdd/c2)

y* = 1

M_BH=32Msun

M_BH = 10^6.5 M_sun, = 0.1

2-1. Comptonization; why do we get so large y*?

_es’ ~ 10

y* = (4kT/mec2)

(_es’)2

Scattering +

absorption

z

Sub-Eddington (M=LEdd/c2) SuperEdd(M=1000LEdd/c2)

Larger density, lower Tem. Lower density, higher Tem.

es/abs ~ 100 es/abs ~ 10^5

_es’ ~ 300

2-3. Spectra with several effects

M_BH = 10^6.5 M_sun, Mdot/(LEdd/c2) = 1000, = 0.1

No Advection: [heating = rad. Cooling]

R_in = 3 R_Sch, L = 63LEdd

Soft X-ray

With Advection [still

In = Bn(Teff);

Mineshige et al. 2000]

L ~ 5.1 LEdd

+ Gravitational Redshift

+ Transverse Doppler S

hift (Innermost region b

ecomes faint):

L ~ 2.6 LEdd

2-3. Spectra with several effectsＭ /(LEdd/c2) =

1000With Advection

+ Relativistic CorrectionNo Advection

+ Opacity of Electron Scatteri

ng

(ie, Modified blackbody)

+ Comptonization

Soft X-ray

Gradual Slopes in

Soft X-ray

Comparison with observations

T_color / T_eff ~ 3.4

(Kawaguchi 2003)

=

If > (sg) → Self-gravity onsets

Kawaguchi (2003)

Mdot = 1000 LEdd/c2

3-1. Latest disc model - 2 : Outer region-- A problem in the current disc model --

Den

sity

Radius

104 RSch

Computations invalid

3-3. Outer edge of non self-gravitating disk

Mdot

RSG

Sub-EddingtonSupper-Eddingto

n

= (sg) [ = Ω2 / (4 G) ] at RSG

(Kawaguchi, Pierens, Hure 2003)

SG

SG: corresponding to

emission from RSG

1-2 m

Torus

Non self-gravitating disc

“Spectral Window to Observe Self-Gravity”

4-1. Spectral fit to Ton S 180 & PG1448:

- Nearby Narrow-Line Seyfert 1 galaxies at z~0.065

- highest-(Mdot/MdotEdd) objects (Mdot > 500LEdd/c2)

L

(B

-ban

d)

MBH Kawaguchi (2003)Low-MBH

High-M/MEdd

4-2. Ton S 180: SED

- Data from Turner ++ 02 (Vaughan ++02), and IRAS

L

4-4. Ton S 180: Inner Slim Disk

- (MBH, Mdot, ) are determined by the least square fit

→ 106.8 MSun, 1000 LEdd/c2, 0.002

→ RSG = 3000 RSch

R<RSG

4-5. Ton S 180: Dusty Torus

- Power-Law with a cut-off (Tmax = 1500 K, here)

- Inner most radius is about 3 x 105 RSch (= 100 RSG)

R>100RSG

R<RSG

~

4-8. Ton S 180: Self-Gravitating Disk-1

- Assumptions; R, R ( 1)

- Inner boundary conditions; (RSG) and H(RSG)

- Outer most radius is chosen to be 10 RSG

R>100RSG

R<RSG

(Kawaguchi, Pierens, Hure 2003)

~ RSG-10RSG

4-9. Ton S 180: Self-Gravitating Disk-2 in self-gravitating disks

SPH simulation by Lodato & Rice (2003)

(grav. Instabilites) > (viscous), if disc mass is large.

Radius Radius Radius

Mdisc=0.05MBH 0.1MBH 0.25MBH

4-10. Ton S 180: Self-Gravitating Disk-3

Three solutions below fit the observed spectrum equally.

out ( ~ r^) Mdisc

0.002 0.3 0.4MBH

(i.e. constant )

0.02 -0.6 1.4MBH

0.1 -1.5 7MBH

radiusRsg

out

Further understanding of grav is necessary

4-18. Broad-band fit to PG1448 (preliminary)

(Kawaguchi, et al. in prep.)

TonS180

4-18. Broad-band fit to PG1448 (preliminary)

(Kawaguchi, et al. in prep.)

TonS180PG1448, NH(Gal)

corrected

Soft X-ray gradually deviate from hard X-ray power-law component.

4-18. Broad-band fit to PG1448 (preliminary)

(Kawaguchi, et al. in prep.)

-TonS180-PG1448, NH(Gal)

corrected-NH(Gal +

intrinsicmax)

corrected

no strong OI edge (~0.5keV)

4-18. Broad-band fit to PG1448 (preliminary)

(Kawaguchi, et al. in prep.)

-TonS180-PG1448, NH(Gal)

corrected-NH(Gal +

intrinsicmax)

corrected

-MBH ~

10^6.2 Msun,

Mdot ~ 1400 LEdd/c

2

~ 0.002

6. Summary-1/2

•Disk model for super-Eddington accretion disk is improved:

- Vicinity of black hole

* Relativistic correction & Electron Scattering

- Outer, self-gravitating part

* Non self-gravitating disc (~0.001 pc) radiates UV-X-ray

* SG part (~0.01 pc) emits optical

(SG has been studied by maser spots at pc-scale.)

* Disc mass is comparable to/larger than BH mass.

6. Summary-2/2

Mid-IR to X-ray SED of the highest-(Mdot/MdotEdd) objects:

- fitted well by inner non SG disk + outer SG disk + torus

Issues to be solved theoretically;

* Small (~ 0.001) is inferred in the inner,

advection dominated (i.e. photon trapped) part.

=> Radiative MHD simulations will answer.

* Efficient transfer/heating by gravitational instabilities

at outer SG part?