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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: 2010112 20
2010112 21
- Page 1 and 2: 2010112 1
- Page 3 and 4: THERMONUCLEAR SN (1.38 M ⦿ ) P
- Page 5 and 6: →→→→ →→ () 56 Ni() Si
- Page 7 and 8: 1000 ()
- Page 9 and 10: CORE COLLAPSE ~1-2 M⦿ ~ GM 2 /R
- Page 11 and 12: ρ>10 12 g/cc : ρ>: + ν e 200
- Page 13 and 14: Si T ≈ ⎛⎛ ⎜⎜ ⎝⎝ 3E 4
- Page 15 and 16: Neutrino driven wind(?) r-: inelas
- Page 17 and 18: 2010112 15
- Page 19 and 20: 1998 FOSSIL IMPRINTS OF FIRST-GENER
- Page 21: TS, Tsujimoto 1998
- Page 25 and 26: 1987A 20 M⦿ Ba 2010112 23
- Page 27 and 28: 1987A 20 M⦿ Ba 2010112 23
- Page 29 and 30: 1987A 20 M⦿ Ba 2010112 (Å)
- Page 31 and 32: 1987A 20 M⦿ Ba 2010112 (Å)
- Page 33 and 34: 1987A 20 M⦿ Ba 2010112 (Å)
- Page 35 and 36: Be/H∝Fe/H Beprimary Be H, HeC, O
- Page 37: Thermonuclear SNe Fe, Si, S Core c
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
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