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

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:

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

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  1. Radiation Spectra from Super-Eddington Active Galctic Nuclei ToshihiroKAWAGUCHI (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: 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

  2. 1-3. Models of super-Eddington accretion: 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/c2) • Abramowicz et al. (1988) • L < several x LEdd • Flow shines even inside 3 x RSch ～ ~ ～ Radius (RSCH) (Kawaguchi 2003)

  3. 2-1. Effects of Comptonization: y* M_BH=32Msun M/ (LEdd/c2) M_BH = 10^6.5 M_sun, a = 0.1 y* = 1 ⇒ Comptonizationinslim disks [Mdot/(LEdd/c2) >> 1]is much more important than that in standard disks [Mdot/(LEdd/c2) < 10]. ~ Spectral distortion due to electron scattering

  4. 2-1. Comptonization; why do we get so large y*? Sub-Eddington (M=LEdd/c2) SuperEdd(M=1000LEdd/c2) Larger density, lower Tem. Lower density, higher Tem. tes/tabs ~ 100 tes/tabs ~ 10^5 y* = (4kT/mec2) (t_es’)2 z t_es’ ~ 10 t_es’ ~ 300 Scattering + absorption

  5. 2-3. Spectra with several effects M_BH = 10^6.5 M_sun, Mdot/(LEdd/c2) = 1000, a = 0.1 With Advection [still In = Bn(Teff); Mineshige et al. 2000] L ~ 5.1 LEdd No Advection: [heating = rad. Cooling] R_in = 3 R_Sch, L = 63LEdd + Gravitational Redshift + Transverse Doppler Shift (Innermost region becomes faint): L ~ 2.6 LEdd Soft X-ray

  6. 2-3. Spectra with several effects T_color / T_eff ~ 3.4 Ｍ/(LEdd/c2) = 1000 With Advection No Advection + Relativistic Correction + Opacity of Electron Scattering (ie, Modified blackbody) + Comptonization Gradual Slopes in Soft X-ray Soft X-ray Comparison with observations (Kawaguchi 2003)

  7. 3-1. Latest disc model - 2 : Outer region-- A problem in the current disc model -- Mdot = 1000 LEdd/c2 Computations invalid Density a = 104 RSch Radius Kawaguchi (2003) If r > r(sg) → Self-gravity onsets

  8. 3-3. Outer edge of non self-gravitating disk RSG • = r (sg) [ = Ω2 / (4 p G) ] at RSG lSG: l corresponding to emission from RSG lSG Torus 1-2 mm “Spectral Window to Observe Self-Gravity” Non self-gravitating disc Mdot (Kawaguchi, Pierens, Hure 2003) Sub-Eddington Supper-Eddington

  9. 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) High-M/MEdd n Ln (B-band) Low-MBH MBH Kawaguchi (2003)

  10. 4-2. Ton S 180: SED n Ln n • Data from Turner ++ 02 (Vaughan ++02), and IRAS

  11. 4-4. Ton S 180: Inner Slim Disk R<RSG • (MBH, Mdot, a) are determined by the least square fit → 106.8 MSun, 1000 LEdd/c2, 0.002 → RSG = 3000 RSch

  12. 4-5. Ton S 180: Dusty Torus R<RSG R>100RSG ~ • Power-Law with a cut-off (Tmax = 1500 K, here)- Inner most radius is about 3 x 105 RSch (= 100 RSG)

  13. 4-8. Ton S 180: Self-Gravitating Disk-1 (Kawaguchi, Pierens, Hure 2003) R<RSG R>100RSG ~ RSG-10RSG - Assumptions; S ~ Rg, H ~ Rb (b ~ 1)- Inner boundary conditions; S(RSG) and H(RSG) - Outer most radius is chosen to be 10 RSG

  14. 4-9. Ton S 180: Self-Gravitating Disk-2a in self-gravitating disks Mdisc=0.05MBH 0.1MBH 0.25MBH a Radius Radius Radius SPH simulation by Lodato & Rice (2003) a(grav. Instabilites) > a(viscous), if disc mass is large.

  15. 4-10. Ton S 180: Self-Gravitating Disk-3 a aout Three solutions below fit the observed spectrum equally.aoutg (S ~ r^g) Mdisc0.002 0.3 0.4MBH (i.e. constant a)0.02 -0.6 1.4MBH0.1 -1.5 7MBH Rsg radius Further understanding of agrav is necessary

  16. 4-18. Broad-band fit to PG1448 (preliminary) TonS180 (Kawaguchi, et al. in prep.)

  17. 4-18. Broad-band fit to PG1448 (preliminary) TonS180 PG1448, NH(Gal) corrected Soft X-ray gradually deviate from hard X-ray power-law component. (Kawaguchi, et al. in prep.)

  18. 4-18. Broad-band fit to PG1448 (preliminary) -TonS180 -PG1448, NH(Gal) corrected -NH(Gal + intrinsicmax) corrected no strong OI edge (~0.5keV) (Kawaguchi, et al. in prep.)

  19. 4-18. Broad-band fit to PG1448 (preliminary) • -TonS180 • -PG1448, • NH(Gal) • corrected • -NH(Gal + • intrinsicmax) • corrected • MBH ~ • 10^6.2 Msun, • Mdot ~ 1400 • LEdd/c2 • a ~ 0.002 (Kawaguchi, et al. in prep.)

  20. 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.

  21. 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 a (~ 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?

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