ÚkÂMŪŔŸťŧŢŘŁļŁ% m½BHŁŗşÓÆ*
arXiv:1610.03482

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INTRODUCTION

2high-z ¾PCBHŁ½
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•(Credit: ESO/M. Kornmesser)ĤñźũŢřŧŶĮŎëêT\ŻŀëêóàĀĝĚėŁ÷üįG<ãĐèĒèæàĀĚĜĞėĚĎĖ åàìêëëä•ŀŋëêêśŅľ

jKVëàśéûěĎíãĐèĒèæ úČęàåàìêêëäĝĞĜĚęĒàúćĈp YbŝŦųŖ•øĔĜĐĎĞàĎĚėėČěĝĐBHøĔĜĐĎĞàĎĚėėČěĝĐà÷ü ãĀĝĐĐď  ëêï ĀĝĚėäbÐnÑ Ĩ jKV ħ• ăĚěàýýýàĜĐĘęČęĞà÷ü ãĀĝĐĐď  ëêìàĀĝĚėäČĞĚĘĔĎçĎĚĚėĔęĒàēČėĚ
ăĚěàýýýàđĚĜĘČĞĔĚębÐnÑ ħ jKV ĨĘĔęĔēČėĚ

ăĚěàýýýàĜĐĘęČęĞà÷üł_bÐļİŐĮž3

Pop III remnant BHŁÓ(p]ÂMįkĿ?3ãăČĜĖâĄĔĎĚĞĞĔ ëëæàĀĔėĚĝČĠėĕĐĠĔĎåàêóä• ÂMŪŔŸťŧŢŘįk5ŀ(ı• ŪŔŸťŧŢŘĴŁĽİŁÓź÷ĚęďĔÓŻŁëéëêêàŀ• ßKVŗşļÙØFŁÊ­ŀōŏŪŔŸťŧŢŘį(ĮĿıĿŐ?3ŋãýęČģĚĝēĔåàëïŻp]ÂMįÚkĿ?3• ŪŔŸťŧŢŘį(ık5ĽÓįÆŉk5į$ĮőŐž• ÓłįŐž4METHOD

5µcŷ¶InH,1 = 105 cm 3ãüĚĝĚĖČġČåàìêëïŁśŸťœgÅŻ• ăÿćĆĂíèêà
simulation regionìøàĄüøàãēėėĎä• āĜ ĢàāĦ õàïëìĢëîî• E-ŗşŁ*HŷÇüæàüåæàüĐæàüĐåæàüĐååæàĐ• ÂMÁÄĜk5Ł ĜČģàĞĜČĎĔęĒBÐµ ãëìòàčĔęĝä• ÷üÍ'• ąğčĒĜĔď ĜČďĔČĞĔĚęàĘĚďĐė
θshadow
BHÂM( ãġČĞČĜČĔåàêêäRin´VG`
MBH = 103 M

T1 = 104 K?

źĪĽļ·lŻĝēČďĚġàĝĔĤĐěČĜČĘĐĞĐĜôĦĝēČďĚġrBRout÷ĚęďĔàĜČďĔğĝ

ãăĚěàýýýàýĀúŁoC»ÎŽ üĔĜČęĚåàëïä(⇠ 109 rSch )]ÂMŁŕŮŸŞ:simulation region?
• ßĿ Ý>ĮŎÙØFįh#• AļÊ­ĳőĻÕœYbθshadowRindisk windionizing photons
slim disk
BHrSchrtrinflow

photo-heating
shocked region

standard diskrcenrBRout

inflowdisk wind]ÂMŁ´VAccretion under anisotropic radiation
G`ŁůţŴ
ionizing photons

slim disk
BH

d withthechemistry is•@ļŁŪŲŢŘş
irection with the spheriLt cell, wheref =photons are
F(✓)
2
4⇡R
r radiation model,
as exinct the absorption of pho• large´VG`of itsuncertainties.
õàź!ÂMŻsfer througha cell, it ĢàźÕŁ(uŻisthe front side of the cellF(✓) = f the(✓)f(✓)
ry is updated indisk
cell shadow
ation using the informaally, -the®ī!ĮŎŁÂMflux on the rearto that fondiskthe(✓)
front=sidesin ✓ng into account the conionization as well as the- ÕŁ(ufied thefshadow
module (✓)
usedź2:.Żins. Firstly, we have modr module with the grayrSch

photo-heating

shocked region

standard disk

rtrrcenF(✓)ÕŁŜŕŠ✓shadowĦź´ļVÿĽĿŐōĬ³v*Ż

8

RESULTS

9F(✓)

ĦkÂMůţŴŁ¦u10kÂM

Figure 4. Structures of accretion flow before (left) and after (right) an accretion burst in Di model. From the top-left panel in clock-wise,
each panel represents the number density nH [cm−3 ], the pressure P [dyn cm−2 ], the neutral fraction of hydrogen xH and the temperature
T [K]. The arrows in the top-left panel represent the velocity v, which is shown only when |v| > 1 kms−1 . The central dashed black circle
represents the Bondi radius rB .

ŧŸşŤ\ŧŸşŤ&Ṁ ∼ 2 × 10−3 ṀB obtained by Milosavljević et al. (2009b),rB,HII is too small to be illustrated in it although we resolve
while a few times smaller than Ṁ ∼ 10−2 ṀB obtained byour simulation. The velocity field does not show 28aFigure 4. Structures of accretion flow before (left) and after (right) an accretionrB,HII
burstinin
Di model. From the top-left panel in clock-wis
Park & Ricotti (2012) althoughthediﬀerence
isinasame
systematic
inflow
structurebutratherseems
tobe
turbu−3−2

ach panel represents the number density n [cm], the pressure P [dyn cm], the neutral fraction of hydrogen x

and the temperaturŪŔŸťŧŢŘĿĴŁĽİÓźkÂMŻ8÷ĚęďĔÓż ṀBK. Sugimura et al.
Ṁ•¯Ł¦uœ"źăČĜĖâĄĔĎĚĞĞĔ ëëæàĀĔėĚĝČĠėĕĐĠĔĎåàêóä•Óįe)•S=ÓįCİıṀ ⇠ 0.17% ṀBźŪŔŸťŧŢŘĴŁëéïêêŻĲőļłăĚěàýýýàĜĐĘęČęĞà÷üłbÐļİĿī12F(✓)ĦÕĴÚkÂMůţŴŁ¦u13

0Accretion under anisotropic radiatioÕĴÚkÂMÓŁe)Wīµ et¤nŁ
K. Sugimuraal.

şŦŢūŝűŢŤęüĆăĢüdCęü

ă

Ć

Ģü

Figure 4. Structures of accretion flow before (left) and after (right) an accretion burst in Di model. From the top-left panel in clo
each panel represents the number density nH [cm−3 ], the pressure P [dyn cm−2 ], the neutral fraction of hydrogen xH and the temp
T [K]. The arrows in the top-left panel represent the velocity v, which is shown only when |v| > 1 kms−1 . The central dashed bla
represents the Bondi radius rB .

Ṁ ∼ 2 × 10−3 ṀB obtained by Milosavljević et al. (2009b),
while a few times smaller than Ṁ ∼ 10−2 ṀB obtained by

14 werB,HII is too small to be illustrated in it although
rB,HII in our simulation. The velocity field does notÓźÕĴÚkÂMŻŪŔŸťŧŢŘĿĴŁĽİ÷ĚęďĔÓż ṀB•ÓŁe)WŇŐ

•S=ÓłīṀ ⇠ 0.13% ṀBźkÂMŁ?3ĽŅņ4xŻĲőļŋăĚěàýýýàĜĐĘęČęĞà÷üłbÐļİĿī15F(✓)ĦÕĪŏÚkÂMůţŴŁ¦uãĥąüöøĂĉ õàîïVŁ?3ä16ÕĪŏÚkÂMź]ËœdCŻ
dCAccretion under anisotropic radiationăęü11tructures of accretion flow before (left) and after (right) an accretion burst in Di model. From the top-left panel in clock-wise,
epresents the number density nH [cm−3 ], the pressure P [dyn cm−2 ], the neutral fraction of hydrogen xH and the temperature
rrows in the top-left panel represent the velocity v, which is shown only when |v| > 1 kms−1 . The central dashed black circle
he Bondi radius rB .

0−3 ṀB obtained by Milosavljević et al. (2009b),
times smaller than Ṁ ∼ 10−2 ṀB obtained byotti (2012) although the diﬀerence is in a sameat between Milosavljević et al. (2009b) and Park2012). The diﬀerence might come from that ind chemistry in each work because Ṁ is sensitive
mal structure of the flow, as discussed in Park
2011, 2012). It might be also possible that themic scheme aﬀect Ṁ quantitatively, as our simuMilosavljević et al. (2009b) adopt Godunov typehile Park & Ricotti (2012) adopts a method withl viscosity. The quantitative diﬀerence mentioned
ever, is not likely to aﬀect the conclusion of ourrB,HII is too small to be illustrated in it although we resolve
rB,HII in our simulation. The velocity field does not show asystematic inflow structure but rather seems to be turbulent since the gas pressure dominate the gravity in the HIand HII regions with r > rB and r > rB,HII , respectively.
These snapshots are also very similar to those plotted in theearly works (Milosavljević et al. 2009b; Park & Ricotti 2011,2012).

ĆĢü18ŪŔŸťŧŢŘĿĴŁĽİÓźÕĪŏÚkÂMŻ ÷ĚęďĔÓż ṀB•ÓłIŀÃĺı•ßīÓṀ ⇠ 60% ṀBkÂMŁ?3Ł¡íêêŹaccretion rate Ṁ and the luminosity L for D models, normalized by the Bondi accretion rate ṀBrespectively. Top left:Ṁ (solid purple), Ṁ on average (dot-dashed purple) and L (solid orange) fo
ĲőĿŎăĚěàýýýàĜĐĘęČęĞà÷üłbÐļİŐl (Di model) are plotted. We overplot the result of the 1-dimensional calculation (dashed green)
in19
inner radiation model with the direction dependence of disk radiation without shadowing eﬀect (DnF(✓)ĦÕpŏÚkÂMůţŴŁ¦uãĥąüöøĂĉ ŀLĵŐG`ä
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ÕÝ>ŁCİĳĽÓṀ /ṀB• ÓŁůţŴ⌦inflowṀ =ṀB4⇡ṀlossĚğĞđėĚġĦĎĜBHÕÝ>ŁCİĳ ĊVċṀlossṀ• ÓłÕÝ>ļŁ÷ĚęďĔÓĽ@ÛĮŎŁŗşDź¬Żļ}ŇŐ
• ÕĮŎŁÓŀ^²Ŀª´VźĦĎĜïVäįG<ĔęđėĚġ⌦inflowṀB4⇡

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CONCLUSION

22ŇĽŊĽº¹p qļłĩìøàĄüøŝŬŰŵŸŝűŶœīĻÚkÂMŪŔŸťŧŢŘŁļŁ÷üÓœ¸ńķ
p ¼ÈÛ ÃŀÕŁG<œIĴķ?3ŀĩkĿ?3Ľ
{ńĻÚRŀßīÓįJĵŐĲĽįŒĮĹķp ÓłÕÝ>ĮŎŁ÷ĚęďĔÓĽÕÝ>±ÛĮŎŁŗşDŁ3ļ}ŇŏĩÕÝ>ĮŎŁÓį(uŀĿŐŁŀoÔ^²ĿÕŁCİĳźïVŻįĪŐ
p ź69ŁŗşKVŀłŐįŻÕĮŎŁ(ĿÓįJ×ŀ½ĲőŃĩăĚěàýýýàĜĐĘęČęĞà÷üłĤðŇļŀ¾PC÷üŀÆ*ĵŐ
ĲĽį0©
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Future workp 8§aĴĿĮĹķÇŁĬĸĩ¦uŀZÜĵŐ0©`įĪŐŋŁœ/ŏőķµ œĭĲĿĬ• «QÍ'ĩ8¿ĩíz`ĩ|¢$FĩFdiĿľp qļ ĮŎŁÂMŁÚk`ŁÍ²`įlŎĮŀĿĹķŁļĩ \ĩ Łœ¸ńŐŁįÍ²• !ÞŌÉ]',[ļŁÓŝűŢŘłJ×őŐŁĮž• ĲőŎŁwÅłÕœŐŁĮžÕłľŁıŎīŁCİĳĮž
p ŋĹĽCİĿşŚŸŴĽŁÒ`ŋlŎĮŀĵŐ^²įĪŐ• ľŁōĬĿ@ļ÷üłbÐĵŐŁĮž• %Ï~ŝŬŰŵŸŝűŶĿľĽ¥ň3ŒĶĻňŐž

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