controlpanel...seed bh eddington motivation: supermassive black holes at high z gw150914 : eddington...
TRANSCRIPT
�� �������������������
1
���, ���� (Tohoku University)
2
4
6
8
10
0 0.2 0.4 0.6 0.8 1
30 20 15 10 8 7 6
log 1
0 M
BH /
M⊙
cosmic age [Gyr]
redshift
Mini=30 M⊙ at z=30Mini=105 M⊙ at z=20
⋆
⋆⋆ ⋆⋆⋆⋆
⋆
⋆⋆
⋆⋆⋆
⋆⋆⋆⋆
⋆⋆
⋆⋆⋆⋆⋆⋆ ⋆⋆
⋆⋆⋆⋆
⋆⋆⋆
⋆⋆⋆⋆⋆
SMBH with 109 M8 at z ~ 7 (�����8��)
2
where tE� 50 Myr
MBH �MBH
BH
GMBHmp
R2=
�L
4�cR2
L = �Mc2
MBH = (1� �)M
���������������!3
MBH = Mini exp (t/tE)
Massive seed
BH��Eddington�������
Motivation:SuperMassive Black Holes at high z
GW150914�� : Eddington� : Eddington�60%
3
Massive Seed Formation
gas cloud protostar star BH
(Volonteri, 2012)
(1) First Star
(2) Direct Collapse
(3) �������
102-103 M8
~105 M8
~103 M8
4
Massive Seed Formation
(1) First Star103
(2) Direct Collapse
(3) ��
~~109
mihi-halo
��
atomic-cooling halo
��
��
�
high-z SMBHs
�
[M8
] 105
z=20-30 z=20-10
5
Massive Seed Formation
(1) First Star103
(2) Direct Collapse
~~109
mihi-halo
��
atomic-cooling halo
��
��
�
high-z SMBHs
��
[M8
]
(3) ��
���SMBH(z�7.5)�!Eddington��������(i) ������ %(ii) �� ��"$#�%
105
z=20-30 z=20-10
6
Direct Collapse��� #$������$���%(
higherdensity
TypicalPopIII� T�200K
UnderstrongUV:T�8000K
(Omukai.2001)
104
102
T[K]
noUVcase
(Omukai 01)
⇒���!��������� '"�&���#%��
M �MJ/t� � c3s/G � T
32
~ 0.1 – 1 M8 yr -1星の最終質量 ~ 105 M8
7
Direct Collapse����/2#�!%���2��39
higherdensity
TypicalPopIII� T�200K
UnderstrongUV:T�8000K
(Omukai.2001)
104
102
T[K]
noUVcase
(Omukai 01)
⇒���)-��� ��*&�+7.(6��/3�
M �MJ/t� � c3s/G � T
32
~ 0.1 – 1 M8 yr -1星の最終質量 ~ 105 M8
'"���2SMBH(1-10/ Gpc3)3 � (Dijkstra+2014)45���0SMBH(0.01-0.1/Mpc3) 8 �,613�*$50(
8
Direct Collapse�� �&(��� ���(���)2
/.01���(�'*+$-."(��%��
��'*,��$#�����2or
��� ���2
Omukai+2008/.0��!���'*,��
9
Direct Collapse;����
Latif+2016 Sakurai+2017
9:&��1��+��,7-0����2"8N���
dust�8�7.)9:&2collapse8����
⇒��3�576+)��' 42(*9:���
105
103
101
103 104 105 106
�$ [yr]
Tagawa+2019
⇒ runaway collision�103 M82�+��
1D/)���429:%�0�<���=02���8��
⇒�105 M82!� #�+��
10
Direct CollapseC����
Latif+2016 Sakurai+2017
AB)��7� .��/>15��� 8$@N�!�
dust��@�>3,AB)8collapse@��!�
⇒�9 <>=.,��*�:8+-AB���
105
103
101
103 104 105 106
�' [yr]
Tagawa+2019
⇒ runaway collision�103 M88�.��
1D4,���:8AB(�5�D��E58���@!�
⇒�105 M88#�"%�.��
&�'8$9!�03-6-
� 8��9��03-=
3��C&�'8��!�9;2�?>3-6-
11
Purpose of this work56#/collapse)2�137������4�'+-,%�! ���.(*3�� �/�����
4�03&
�� �
atomic-cooling halo
�
��$����103
�"
�
[M8
]
105
8
� Gadget2 (SPH + N-body)� barotropic-EOS
(Z/Z8 = 10-3, 10-4, 10-5, 5×10-6, 10-6 )
� multiple sink, merger (created at n = 2×1016 – 2×1017 cm-3)� sink radius
・ Initial Condition ⇒ Spherical Cloud (SC+16,18)
2
3
4
5 10 15
log T
[K]
log n [cm-3]
Z/Z8 = 10-6
5×10-6
10-5
10-4
10-3
Numerical Setup
12
30 pc7
8
9
10
11
12
log
< de
nsity
>
104AUz = 12.7
Spherical Cloud
10 Mpc
���nadib
Hosokawa+2013
Accretion Phase
13
Z = 10-6 Z8 Z = 10-4 Z8
���M>10 M8�massive sink, ���M<10 M8�small sink
Z = 10-3 Z8
Accretion Phase
14
Z = 10-6 Z8 Z = 10-4 Z8
�1M>10 M8,massive sink, ��1M<10 M8,small sink
Z = 10-3 Z8
"-/��$�%*#Massive star$ �(0(����)consistent)
Dust��+./�'&����+massive star$ �(Z/Z8 = 10-6)��)
����+.0��+./��*��$���+./��$ �(0!
Mass Evolution
15
@ Z/Z8<10-4 48metallicity69:3+1 M8 yr-17?A>4�&⇒ dust��8��=�"+���7�$"='�25-⇒ ��$�.��
@ Z/Z8=10-3 48+�$(��
.�/0�.<(�0.01 M8 yr-1)⇒%�!�69<��4+9;��4#�� .�1<,
⇒���7�&8)��6,(M ∝ T3/2)
⇒*����.��0 5000 10000
Time [yr]
10-3 Z8
Z < 10-4 Z8
@
16
Merger v.s. Accretion
0
0.2
0.4
0.6
0.8
1
Metallicity [Z8]
10-4 10-5 10-65×10-6
frac
tion
10-3
gas accretion
Mergers with M* < 100 M8
Mergers with M* > 100 M8
�����'��$!���!%'����� ��! '�⇒ )(*��!%&���"�����'����!%&���#���'�
Time [yr]
Z/Z8 = 10-4
10-5
5�10-6
10-610-3
Summary• ����D8<K�*�)��CE$�")���(�DA7B5P��E")'L&@?6
• Z/Z8 < 10-4 CF 6-84103 M8E�9��6
Ø NMO��DIJ�!F>KHEE5���F��D")�+>K6
• Z/Z8 = 10-3 CF 350 M8E�9��6
Ø *�% ��DIJ5IJ��C� 9#=K6Ø ���GE-��F�:;��/�2123.M8 yr-10
17�,
����
atomic-cooling halo
��
� ����103
�
[M8
]
105
Z/Z8 < 10-4
Z/Z8 > 10-3
18
Mass distribution (1��)
19
1
10
100
-2 0 2 4
Num
ber
log10 Mass [M⊙]
1
10
100
Num
ber
1
10
100
Num
ber
1
10
100
Num
ber
Z = 10-4 Z8
10-5 Z8
5×10-6 Z8
10-6 Z8
∝M -1
1
10
100
-2 0 2 4N
umbe
rlog10 Mass [M⊙]
1
10
100
Num
ber
1
10
100
Num
ber
1
10
100
Num
ber
1
10
100
-2 0 2 4
Num
ber
log10 Mass [M⊙]
1
10
100
Num
ber
1
10
100
Num
ber
1
10
100
Num
ber
-2 0 2 4 -2 0 2 4 -2 0 2 4log Mass [M8] log Mass [M8] log Mass [M8]
100
10
1
num
ber
Low mass star ���!Z/Z8>5�10-6���⇒ dust�� '&)(��"#�High mass star ���!'&)(� %' flow$�����#�⇒��� ��������#�
Collapse phase
20
10
12
14
16
log
< d
ensi
ty >
6
8
10
12
log
< d
ensi
ty >
2 4 6 8log < density >
2 4 6 8log < density >
106 au
106 au
5×104 au 200 au
10 12 14 16log < density >
200 au
10 12 14 162 4 6 8
10-3 Z8
10-5 Z8
10 12 14log < density >
(a)
(a)
(b)
(b)
(c)
(c)
10 12 14
log n [cm-3]
5×104 au
Z/Z8 < 10-4����� ������ ⇒ dust���small scale (< 103 au) ��������
21
Onset of the gravitational collapse
-1
0
1
2
3
2 4 6
log
M(<
R) /
MB
E
log M(<R) [M⊙]
Gravitationally unstable
Gravitationally stable
Z/Z8= 10-3
10-4
5
10
15
0 1 2 3 4
log
n [c
m-3
]
time [106 yr]
Z/Z8= 10-3 10-4
10-6
��������������������
⇒������� ������ �������
Mass distribution (1��)
28
1
10
100
1000
-6 -4 -2 0
Num
ber
log10 Mdot [M⊙ yr-1]
1
10
100
1000
Num
ber
1
10
100
1000
Num
ber
1
10
100
1000
Num
ber
-6
-4
-2
-2 0 2 4log10 Mass [M⊙]
-6
-4
-2
-6
-4
-2
-6
-4
-2
log 10Mdot[M
8yr-1]
Mass function�������
⇒ competitive accretion(e.g. Bonnel+2001),�����-1
⇒�����sink���������� ��
29
Supermassive star or dense cluster?���(Sakurai+2017)��������� ���������� ������
300 au
��
30
Detection rate of GWsNmerge = NDC fbinary fmerge
(Habouzit et al, 2016)
��9����,0SMS/���.*#+�"-�%��(6+#57�8!��,0���%$-4�&#% �/GW��,#'3$��,&5$1)6-#!
�/��24
(Haehnelt, 1994)
Dijkstra+2014
Agarwal+2012
Habouzit+2016
this work
Massive binaries
31
0
1000
2000
3000
sepa
ratio
n [A
U]
0
0.5
1
0 5000 10000
mas
s rat
io
Time [yr]
(a)
(b)
���metallicity����massive binary����binary�separation��������� (SC+19)�mass ratio�1�� �Z = 10-4 Z8