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

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Radiation Spectra from Super-Eddington Active Galctic Nuclei. Toshihiro KAWAGUCHI (Meudon Observatory, France). Collaborating with A. Pierens, J.M. Hure (Meudon Observatory) C. Matsumoto, K.M. Leighly (Univ. of Oklahoma, USA). 1. Introduction to Super Eddington accretion: - PowerPoint PPT Presentation
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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 Nucle i Toshihiro KAWAGUCHI (Meudon Observatory, Franc e) 1. Introduction to Super Eddington accretion: 2. Latest disc model 1: Vicinity of Black Hole (< 100 R Sch ) 3. Latest disc model 2: Outer region (~ 1 0 4 R Sch )
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Page 1: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 2: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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)

~

Page 3: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 4: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 5: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 6: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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)

Page 7: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

=

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

Page 8: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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”

Page 9: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 10: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

4-2. Ton S 180: SED

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

L

Page 11: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 12: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

~

Page 13: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 14: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 15: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 16: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

(Kawaguchi, et al. in prep.)

TonS180

Page 17: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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.

Page 18: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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)

Page 19: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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

Page 20: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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.

Page 21: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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?

Page 22: Collaborating with A. Pierens, J.M. Hure (Meudon Observatory)

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