Hot and Dense Nuclear Matter - Department of Physics and Astronomy
Hot and Dense Nuclear Matter - Department of Physics and Astronomy
Hot and Dense Nuclear Matter - Department of Physics and Astronomy
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Late stage hadrochemistry<br />
• Assume all distributions described by one temperature T <strong>and</strong> one<br />
(baryon) chemical potential μ<br />
(Chemical Equilibrium):<br />
• One ratio (e.g., ⎯p-bar / p ) determines μ / T :<br />
• A second ratio (e.g., K / π ) provides T μ<br />
• Then predict all other hadronic yields <strong>and</strong> ratios:<br />
−( E −μ)/ T 3<br />
dn ~ e d p<br />
− ( E + μ)/<br />
T<br />
p e<br />
= = e<br />
−( E −μ)/<br />
T<br />
p e<br />
−2 μ / T<br />
<strong>Hot</strong> <strong>and</strong> <strong>Dense</strong> <strong>Nuclear</strong> matter 13
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