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2010112<br />
1
Thermonuclear Supernova<br />
(1.4 M ⦿ )<br />
Core Collapse Supernova<br />
(8-140 M ⦿ )<br />
()<br />
()=0<br />
Pair Instability Supernova<br />
(140-270M ⦿ )<br />
(?)<br />
2010112<br />
2
THERMONUCLEAR SN<br />
<br />
<br />
(1.38 M ⦿ )<br />
<br />
P∝ρ 4/3<br />
dP/dr∝M 4/3 r -4-1<br />
∝GMρ/r 2 ∝M 2 r -3-2<br />
<br />
Carbon burning<br />
<br />
2010112<br />
3
→→→→<br />
<br />
()<br />
56 Ni()<br />
Si, S,C, O<br />
56<br />
Ni( 56 Ni→ 56 Co→ 56 Fe)γ<br />
~10 51 erg<br />
2010112<br />
4
→→→→<br />
<br />
→→<br />
()<br />
56 Ni()<br />
Si, S,C, O<br />
56<br />
Ni( 56 Ni→ 56 Co→ 56 Fe)γ<br />
~10 51 erg<br />
2010112<br />
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Nomoto, Thielemann, Yokoi 1984<br />
1984ApJ...286..644N<br />
<br />
2010112<br />
5
1000<br />
()<br />
<br />
Single degenerate or Double degenerate<br />
<br />
<br />
<br />
M Ni >1.4 M ⦿<br />
2?<br />
SN<br />
SN<br />
<br />
()()<br />
?<br />
2010112<br />
7
CORE COLLAPSE<br />
<br />
~1-2 M⦿<br />
~ GM 2 /R<br />
~5x10 53 erg<br />
<br />
<br />
~10 51 -10 52 erg<br />
<br />
2010112<br />
8
CORE COLLAPSE<br />
<br />
~1-2 M⦿<br />
~ GM 2 /R<br />
~5x10 53 erg<br />
<br />
<br />
~10 51 -10 52 erg<br />
<br />
2010112<br />
8
ρ>10 12 g/cc :<br />
<br />
ρ>: <br />
+<br />
ν e <br />
200 km<br />
<br />
wind<br />
Janka et al. 2007<br />
2010112<br />
9
1.40<br />
<br />
1000<br />
1.30<br />
10 M ⦿ , 15 M ⦿<br />
<br />
radius [km]<br />
100<br />
<br />
10<br />
<br />
-100 0 100 200 300<br />
time [ms]<br />
Janka et al. 2007<br />
2010112<br />
10
Si<br />
T ≈<br />
⎛⎛<br />
⎜⎜<br />
⎝⎝<br />
3E<br />
4πR 3 a<br />
⎞⎞<br />
⎟⎟<br />
⎠⎠<br />
1 4<br />
T>5×10 9 K <br />
T
1990ApJ...360..242S<br />
1990ApJ...349..222T<br />
SN 1987A <br />
Nomoto, TS 1991<br />
Thielemann, Hashimoto, Nomoto 1990<br />
2010112<br />
12
Neutrino driven wind(?)<br />
r-: <br />
inelastic scattering<br />
C: 12 C(ν, ν’p ) 11 B<br />
He: 4 He(ν, ν’p) 3 H(α, γ) 7 Li<br />
<br />
C,OWolf-Rayet(WC)<br />
(~10 -5 M⦿)H, He, LiBeB<br />
2010112<br />
13
2010112<br />
14
2010112<br />
15
2010112<br />
16
1998 FOSSIL IMPRINTS OF FIRST-GENERATION SN EJECTA<br />
or the solar abundances is used. Then L primordial(T)<br />
is<br />
cted for the gas composed of only hydrogen and helium,<br />
eir mass ratio X H:XHe<br />
0.75:0.25 under the collisional<br />
2 3<br />
ion equilibrium. For n1<br />
10 cm , equation (1) gives<br />
5<br />
K. Thus, <br />
the ionization of hydrogen does not affect<br />
amics.<br />
mass<br />
<br />
of hydrogen Msw<br />
thus obtained with L(T) <br />
ial(T) in equation (1) is approximated by the formula<br />
(<br />
4<br />
Msw 5.1 # 10 M, )<br />
E 0<br />
51<br />
10 ergs<br />
)<br />
0.97<br />
(<br />
9/7<br />
c<br />
0.062<br />
s<br />
# n 1 . (2)<br />
1<br />
10 km s<br />
sw is insensitive to n1. The sound speed c s was assumed<br />
1 4<br />
0 km s (or T ∼ 10 K). This mass depends on E 0 and<br />
different way than that of Cioffi et al. (1988) because<br />
different cooling function used here. The cooling funcith<br />
the primordial abundances is approximately<br />
2010112<br />
propor-<br />
TABLE 1<br />
Input Parameters in SN Models and Ca<br />
Corresponding S<br />
Name<br />
WW95<br />
M ms E 0<br />
( M , ) (#10 51 ergs) [Mg/H]<br />
Z12A . . .... 12 1.28 4.1<br />
Z13A . . .... 13 1.29 3.6<br />
Z15A . . .... 15 1.27 3.2<br />
Z22A . . .... 22 1.26 2.8<br />
Z25B . ..... 25 1.83 2.9<br />
Z30B . ..... 30 2.06 2.5<br />
Z35C . ..... 35 2.49 2.6<br />
Z40C . ..... 40 3.01 2.6<br />
n, f, and VSNR<br />
denote the number den<br />
stars, the IMF normalized to unity bet<br />
mass limits, and the maximum volu<br />
SNR, respectively. This condition re<br />
efficiency for the first-generation sta 17
10<br />
<br />
1<br />
0.1<br />
0.01<br />
Nomoto model<br />
Woosley model<br />
0.001<br />
10 20 30 40 50 60 70 80<br />
<br />
2010112<br />
18
TS, Tsujimoto 1998<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
2010112<br />
19
L138<br />
SHIGEYAMA<br />
Fe<br />
Fig. 2.—Top<br />
TS,<br />
panel:<br />
Tsujimoto<br />
the crosses are the observed<br />
1998<br />
[C/Mg] for stars plotted<br />
against [Mg/H] (McWilliam et al. 1995). The open and filled circles show the<br />
same quantities in the first-generation SNRs calculated from theoretical SN<br />
models (WW95 [open circles]; T95 [filled circles]). The arrow indicates the<br />
change in the abundance pattern of the model so as to reproduce the SN 1987A<br />
observations (Thielemann et al. 1990 and references therein). Middle panel:<br />
2010112<br />
20
2010112<br />
21
: <br />
<br />
20(2)<br />
(Tsujimoto, TS,<br />
Yoshii 2000)<br />
2010112<br />
22
1987A<br />
<br />
20 M⦿<br />
Ba <br />
<br />
2010112<br />
23
1987A<br />
<br />
<br />
<br />
20 M⦿<br />
Ba <br />
<br />
2010112<br />
23
1987A<br />
<br />
<br />
<br />
20 M⦿<br />
Ba <br />
<br />
2010112<br />
23
1987A<br />
<br />
20 M⦿<br />
Ba <br />
<br />
2010112<br />
23
1987A<br />
<br />
20 M⦿<br />
<br />
Ba <br />
<br />
2010112<br />
(Å)<br />
23
1987A<br />
<br />
20 M⦿<br />
<br />
Ba <br />
<br />
2010112<br />
(Å)<br />
23
1987A<br />
<br />
20 M⦿<br />
<br />
Ba <br />
<br />
2010112<br />
(Å)<br />
23
1987A<br />
<br />
20 M⦿<br />
<br />
Ba <br />
<br />
2010112<br />
(Å)<br />
23
1987A<br />
<br />
20 M⦿<br />
<br />
Ba <br />
<br />
2010112<br />
(Å)<br />
23
1987A<br />
<br />
20 M⦿<br />
Ba <br />
<br />
2010112<br />
23
Be/H∝Fe/H<br />
Beprimary<br />
Be<br />
<br />
H, HeC, O<br />
Be/H∝(Fe/H)^2<br />
C, O<br />
SAGA<br />
2010112<br />
24
Thermonuclear SNe<br />
<br />
Fe, Si, S<br />
Core collapse SNe<br />
<br />
(Li, Be, B), O, Ne, Mg, Si, S, Ti, Ca,, (r-process elements)<br />
2010112<br />
25
Thermonuclear SNe<br />
<br />
Fe, Si, S<br />
Core collapse SNe<br />
<br />
(Li, Be, B), O, Ne, Mg, Si, S, Ti, Ca,, (r-process elements)<br />
<br />
2010112<br />
25