Changes between Version 6 and Version 7 of TriggeredStarFormation

Timestamp:

01/07/14 18:19:05 (11 years ago)

Author:

Shule Li

Comment:

—

TriggeredStarFormation

@@ -54 +54 @@
 
 The two algorithms give different results for the non-rotating case when the isothermal approximation $\gamma = 1.0001$ is used. As shown in the following movie for K = 0.1, parallel rotation for Krumholz algorithm and Federrath algorithm. For the Federrath case, after the bounded material enters the post-shock region, the disk disappears due to an "explosion". [[BR]]
+[[Image(http://www.pas.rochester.edu/~shuleli/meeting0819/acomp.png,40%)]][[BR]][[BR]]
+Movies: [[BR]]
 parallel rotation, Krumholz: [[BR]]
 http://www.pas.rochester.edu/~shuleli/tsf_paper/parrot.gif
@@ -74 +76 @@
 [[BR]][[BR]]
 
+There is also a difference in asymptotic star mass due to the difference in accretion routines. [[BR]][[BR]]
+[[Image(http://www.pas.rochester.edu/~shuleli/0520/starmass.png,40%)]]
+
 '''MHD Triggering'''[[BR]]
 When added magnetic field to the cloud, the triggering behavior can be very different. Here, we suppose the initial rotation to be zero first, and look at the case where there is a global uniform magnetic field along .
@@ -84 +89 @@
 
 
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