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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
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