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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The “Flow” Is Large<br />
• Value <strong>of</strong> v 2 in<br />
dn/dφ ~ 1 + 2 v 2 cos (2 φ) + ..<br />
saturates at ~ 0.2<br />
• Hydrodynamic calculations<br />
show this collective flow is<br />
– characteristic <strong>of</strong><br />
a strongly interacting<br />
state <strong>of</strong> matter with<br />
very low viscosity<br />
10<br />
5<br />
0<br />
−5<br />
−10<br />
−10 −5 0 5 10<br />
10<br />
5<br />
10<br />
5<br />
0<br />
−5<br />
−10<br />
−10 −5 0 5 10<br />
10<br />
5<br />
– established in the<br />
earliest (geometrically<br />
asymmetric) stage<br />
<strong>of</strong> the collision<br />
– The flow is as strong as it<br />
can be<br />
0<br />
−5<br />
−10<br />
−10 −5 0 5 10<br />
0<br />
−5<br />
−10<br />
−10 −5 0 5 10<br />
<strong>Hot</strong> <strong>and</strong> <strong>Dense</strong> <strong>Nuclear</strong> matter 29