ASTR 610 Theory of Galaxy Formation Lecture 16
ASTR 610 Theory of Galaxy Formation Lecture 16
ASTR 610 Theory of Galaxy Formation Lecture 16
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The Origin <strong>of</strong> Exponential Disks<br />
If there is no angular momentum loss (or redistribution) during the disk formation<br />
process, then the disk surface density pr<strong>of</strong>ile is a direct reflection <strong>of</strong> the specific<br />
angular momentum distribution <strong>of</strong> the proto-galaxy.<br />
Σ d (R) M bar (j bar ) M DM (j DM )<br />
In <strong>Lecture</strong> 9 we have seen that the specific angular momentum distributions <strong>of</strong><br />
dark matter haloes are well fit by the Universal pr<strong>of</strong>ile:<br />
P(j) = µj 0<br />
(j + j 0 ) 2 M(< j)=M vir<br />
µj<br />
(j + j 0 )<br />
If picture <strong>of</strong> detailed specific angular momentum conservation is correct then<br />
M d (
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