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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Maxwell Boltzmann Distribution<br />
In stellar material of temperature T particles follow ideal gas law<br />
Φ(<br />
v)<br />
4<br />
=<br />
3/<br />
2<br />
2<br />
m v<br />
⎛ m ⎞ −<br />
2<br />
⎜ ⎟<br />
∫<br />
2kT<br />
π v e ( v dv =<br />
with<br />
4<br />
⎜<br />
2 kT<br />
⎟<br />
⎝ π ⎠<br />
Φ ) 1<br />
arbitrary units<br />
3<br />
2<br />
1<br />
max at<br />
E=kT<br />
example: <strong>in</strong> terms<br />
of energy<br />
E=1/2 m v 2<br />
0<br />
0 20 40 60 80<br />
energy (keV)
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