)%&!# ($#&(!$#$#($''( "(!#(&',*Daisuke Toyouchi,Kyoto univ. in collaboration withKazuyuki Sugimura (Maryland univ.), Riouhei Nakatani (RIKEN),
Takashi Hosokawa (Kyoto univ.), Rolf Kuiper (Tubingen Univ.)
+  @  2019/11/13

-       
109 MsunMarziani et al. (2012)Black hole mass

Massive seed black hole ?

104 Msunsuper-Edd. growth ?

100 Msun
Eddington mass growth limitz ~ 20-30

z~7Redshift      

MBH = 108 Msun

Circum-nuclear disk (CND)

Schwarzschild scale~ 1 AU

Bondi scale
1-102 pc Galactic scale
1-100 kpc

Ohsuga+2005

super-Edd. accretion!

à 3D-RHD sim.

galaxy merger à dM/dt ~ 101-2 Msun/yr(c.f., Hopkins+2010)    
Wada et al. (2016, 2018)
ü High spatial resolution 2563 grids, Δx ~ 104 AU
ü Various chemical species : H, H2, H+, H-, e-, O, O2, O+, H2O, C, C+, CO, He, He+, HCO+ etc.

 
Wada et al.
• Local AGNsThis work
• IMBHs growing in the early universeü Mbh > 106 Msun (MCND/Mbh < 1)

ü Mbh = 104 Msun (MCND/Mbh > 1)

ü Solar-abundanceü Z < 0.1 Zsun

ü Assuming sub-Edd. LAGNü Exploring condition for super-Edd.

• Detailed simulations only for a fewcases
ü 2563 uniform grids
ü various chemical species• Examining various situations
ü (Nr, Nθ, Nφ) = (128, 36, 72) (Finergrids near the equatorial plane)ü only essential chemical species
ü dependence on gas density andmetallicity      l HD simulation (public code “PLUTO”)
ül 

Self-gravity of gas

Hydrodynamics

Chemistry

Radiative transferüphotoionization (EUV)ü

dust attenuation (FUV, EUV)

üdust thermal emission (IR; FLD approximation)üradiation pressure (Thomson scattering,

Radiative transfer

photoionization, dust UV & IR radiative force)lNon-equilibrium Chemistryü

six species: HI, HII, HeI, HeII, HeIII, e-, (some heavy elements, molecules)üphotoionization, recombination, collisional excitation & ionization, freefree emission, metal line cooling, dust-gas collisional cooling etc.

l HD simulation (public code “PLUTO”)
ül 

self-gravity of gas

Radiative transferüphotoionization (EUV)üdust attenuation (FUV, EUV)

üdust thermal emission (IR; FLD approximation)üradiation pressure (Thomson scattering,photoionization, dust UV & IR radiative force)lChemistry

Hydrodynamics

Radiative transfer

Key effects!!

Non-equilibrium Chemistryü

six species: HI, HII, HeI, HeII, HeIII, e-, (some heavy elements, molecules)üphotoionization, recombination, collisional excitation & ionization, freefree emission, metal line cooling, dust-gas collisional cooling etc.

   
3D-spherical coordinate5e3 AU < r < 5e5 AU, 0 < θ < π/2, 0 < φ < 2π
Mass flux at inner boundary à BH luminosity(Watarai+2000)

Anisotropic radiation

F (✓) / cos2 ✓(Ohsuga+2005)<latexit sha1_base64="yLjYj2OAPEhcaP7hhrXa88HAJEM=">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</latexit>

dMin/dt = Fin x (Edd. rate)Vin,φ = 0.5 x (Kepler velocity)
Gas inflow along
the equatorial plane

MBH = 104 Msun
Fragmentation of the ring due to the self-gravity

Fin102
(dMin/dt = Fin x Edd. rate)

Z3F2

Z2F2

Z1F2

Z2F1

101
10-3

10-2

Z/Zsun10-1   

Face-onnH    
Edge-onnHTgas   

 

Super-Edd. accretion!

     

Finsuper-Edd.!!

Z2F240 (40 %)102
110Z1F250 (50 %)Z/Zsun10-3

10-210-1  

 



Z = 10-2 Zsun (Fiducial)
Z = 10-1 Zsun

      
1D RHD simulation (Toyouchi et al. 2019)

Spherical accretionrBondiFd,IRrHIISuper-Edd. accretion occurs
only for Z < 10-2 Zsun

Fd,UV

Non-spherical accretion
Acc. rate ~ Edd. rate for IR radiative force

UV, X-rayIRü Unlike spherical accretion, the radiative force from dust
thermal emission cannot suppress the super-Edd. flow.
ü Similar to “flashlight effect”, well known for the formation ofmassive stars (e.g., York & Sonnhalter 2002).

     

Finsuper-Edd.!!

102

Z2F240 (40 %)

1
10

Z2F1

sub-Edd.

10-3

0.01 (0.1 %)10-2

Z1F250 (50 %)Z/Zsun10-1     

Fin = 100 (Fiducial)

Fin = 10      

Face-onEdge-onnHnHTgas
The inner part of disk is completely photoevaporated.

     Fin~ Edd.

102
110Z3F22 (2 %)sub-Edd.

10-3

super-Edd.!!

Z2F240 (40 %)Z2F10.01 (0.1 %)10-2

Z1F250 (50 %)Z/Zsun10-1  

   
Only a few percent of inflowing
gas can reach the central BH

Z = 10-2 Zsun (Fiducial)

Z = 10-3 Zsun         
Z = 10-3 Zsun

Z = 10-1 Zsun

For the lower gas metallicity, a larger amount of gas is lost as outflow.

         
Z = 10-3 Zsun

Z = 10-1 Zsun

For the lower metallicity, the disk becomes much thicker due to the less efficient metal coolingà More significant effect of photo-evaporation

  “Super-Eddington accretion is potentially possible.”ü high inflow rate from galactic disk
ü high gas metallicity

but, …
ü How often is such situation realized? (Yajima san’s talk)ü Is mass loss from the central slim disk negligible?
(Haojie’s & Takeo kun’s talk)

Cooperation with the HD simulations on the galacticand the central accretion disk scales is essential.