Nuclear Reactions in Stars & in the Laboratory
Nuclear Reactions in Stars & in the Laboratory
Nuclear Reactions in Stars & in the Laboratory
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The Gamow Range of Stellar Burn<strong>in</strong>g<br />
The Gamow w<strong>in</strong>dow or <strong>the</strong> range of relevant cross section<br />
for “non-resonant” processes is calculated:<br />
Check derivation <strong>in</strong> book<br />
3/ 2<br />
⎛ bkT ⎞<br />
E0 = ⎜ ⎟ = 0.122⋅<br />
1 2<br />
T<br />
⎝ 2 ⎠<br />
(<br />
2 2<br />
)<br />
1/3 2/3<br />
Z Z A MeV<br />
9<br />
ΔE<br />
=<br />
4 6<br />
E0kT<br />
= 0.2368⋅<br />
1 2<br />
T9<br />
3<br />
(<br />
2 2<br />
)<br />
1/ 6 5/<br />
Z Z A MeV<br />
with A “reduced mass number” and T 9<br />
<strong>the</strong> temperature <strong>in</strong> GK
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