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2010112
1

Thermonuclear Supernova
(1.4 M ⦿ )
Core Collapse Supernova
(8-140 M ⦿ )
()
()=0
Pair Instability Supernova
(140-270M ⦿ )
(?)
2010112
2

THERMONUCLEAR SN
(1.38 M ⦿ )
P∝ρ 4/3
dP/dr∝M 4/3 r -4-1
∝GMρ/r 2 ∝M 2 r -3-2
Carbon burning
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3

→→→→
()
56 Ni()
Si, S,C, O
56
Ni( 56 Ni→ 56 Co→ 56 Fe)γ
~10 51 erg
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4

→→→→
→→
()
56 Ni()
Si, S,C, O
56
Ni( 56 Ni→ 56 Co→ 56 Fe)γ
~10 51 erg
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4

Nomoto, Thielemann, Yokoi 1984
1984ApJ...286..644N
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5

1000
()

Single degenerate or Double degenerate
M Ni >1.4 M ⦿
2?
SN
SN
()()
?
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7

CORE COLLAPSE
~1-2 M⦿
~ GM 2 /R
~5x10 53 erg
~10 51 -10 52 erg
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8

CORE COLLAPSE
~1-2 M⦿
~ GM 2 /R
~5x10 53 erg
~10 51 -10 52 erg
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8

ρ>10 12 g/cc :
ρ>:
+
ν e
200 km
wind
Janka et al. 2007
2010112
9

1.40
1000
1.30
10 M ⦿ , 15 M ⦿
radius [km]
100
10
-100 0 100 200 300
time [ms]
Janka et al. 2007
2010112
10

Si
T ≈
⎛⎛
⎜⎜
⎝⎝
3E
4πR 3 a
⎞⎞
⎟⎟
⎠⎠
1 4
T>5×10 9 K
T

1990ApJ...360..242S
1990ApJ...349..222T
SN 1987A
Nomoto, TS 1991
Thielemann, Hashimoto, Nomoto 1990
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12

Neutrino driven wind(?)
r-:
inelastic scattering
C: 12 C(ν, ν’p ) 11 B
He: 4 He(ν, ν’p) 3 H(α, γ) 7 Li
C,OWolf-Rayet(WC)
(~10 -5 M⦿)H, He, LiBeB
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13

2010112
14

2010112
15

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16

1998 FOSSIL IMPRINTS OF FIRST-GENERATION SN EJECTA
or the solar abundances is used. Then L primordial(T)
is
cted for the gas composed of only hydrogen and helium,
eir mass ratio X H:XHe
0.75:0.25 under the collisional
2 3
ion equilibrium. For n1
10 cm , equation (1) gives
5
K. Thus,
the ionization of hydrogen does not affect
amics.
mass
of hydrogen Msw
thus obtained with L(T)
ial(T) in equation (1) is approximated by the formula
(
4
Msw 5.1 # 10 M, )
E 0
51
10 ergs
)
0.97
(
9/7
c
0.062
s
# n 1 . (2)
1
10 km s
sw is insensitive to n1. The sound speed c s was assumed
1 4
0 km s (or T ∼ 10 K). This mass depends on E 0 and
different way than that of Cioffi et al. (1988) because
different cooling function used here. The cooling funcith
the primordial abundances is approximately
2010112
propor-
TABLE 1
Input Parameters in SN Models and Ca
Corresponding S
Name
WW95
M ms E 0
( M , ) (#10 51 ergs) [Mg/H]
Z12A . . .... 12 1.28 4.1
Z13A . . .... 13 1.29 3.6
Z15A . . .... 15 1.27 3.2
Z22A . . .... 22 1.26 2.8
Z25B . ..... 25 1.83 2.9
Z30B . ..... 30 2.06 2.5
Z35C . ..... 35 2.49 2.6
Z40C . ..... 40 3.01 2.6
n, f, and VSNR
denote the number den
stars, the IMF normalized to unity bet
mass limits, and the maximum volu
SNR, respectively. This condition re
efficiency for the first-generation sta 17

10
1
0.1
0.01
Nomoto model
Woosley model
0.001
10 20 30 40 50 60 70 80
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18

TS, Tsujimoto 1998
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19

L138
SHIGEYAMA
Fe
Fig. 2.—Top
TS,
panel:
Tsujimoto
the crosses are the observed
1998
[C/Mg] for stars plotted
against [Mg/H] (McWilliam et al. 1995). The open and filled circles show the
same quantities in the first-generation SNRs calculated from theoretical SN
models (WW95 [open circles]; T95 [filled circles]). The arrow indicates the
change in the abundance pattern of the model so as to reproduce the SN 1987A
observations (Thielemann et al. 1990 and references therein). Middle panel:
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20

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21

:
20(2)
(Tsujimoto, TS,
Yoshii 2000)
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22

1987A
20 M⦿
Ba
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23

1987A
20 M⦿
Ba
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23

1987A
20 M⦿
Ba
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23

1987A
20 M⦿
Ba
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23

1987A
20 M⦿
Ba
2010112
(Å)
23

1987A
20 M⦿
Ba
2010112
(Å)
23

1987A
20 M⦿
Ba
2010112
(Å)
23

1987A
20 M⦿
Ba
2010112
(Å)
23

1987A
20 M⦿
Ba
2010112
(Å)
23

1987A
20 M⦿
Ba
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23

Be/H∝Fe/H
Beprimary
Be
H, HeC, O
Be/H∝(Fe/H)^2
C, O
SAGA
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24

Thermonuclear SNe
Fe, Si, S
Core collapse SNe
(Li, Be, B), O, Ne, Mg, Si, S, Ti, Ca,, (r-process elements)
2010112
25

Thermonuclear SNe
Fe, Si, S
Core collapse SNe
(Li, Be, B), O, Ne, Mg, Si, S, Ti, Ca,, (r-process elements)
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25