Meeting Update 1007

Triggered Star FormationI've been running simulations according to Boss' setup:
​http://www.pas.rochester.edu/~shuleli/triggered/bosspaper2.pdf
I'll post three new movies Monday morning.

Qual I'm currently making the ppt, 15 pages done (total 45 pages?).

Papers Done with the revision of HEDLA proceeding.
​http://www.pas.rochester.edu/~shuleli/triggered/shuleconf2012_AF.pdf
Got the referee's response for the ApJ paper, which is pretty positive. The following points require some thought: (the rest points are trivial to improve)

2) On page 7 they state that they have used the Dalgarno and McCray (1972) cooling function. This is a bit old: it would have been more realistic to use Wolfire et al. (1994) to get a cooling function. They could also have included heating to get an equilibrium temperature (as in Van Loo et al. MNRAS, 406, 1260, 2010), rather than just switching off the cooling at 50K.

3) The choice of parameters for the cloud on page 8 seems somewhat eccentric. A density of 100 and a temperature of 100 is fine since this is roughly what Wolfire et al. would predict for thermal equilibrium, but the size seems very small. The translucent clumps in molecular clouds have these properties, but they are much bigger (~1 pc instead of 150 a.u.). Objects this small are only interesting if they have much higher densities.

The cloud size only affects the ratio of the cooling time to the other timescales. A more realistic simulation would have a very short cooling time: so short that one might as well assume that the gas is in thermal equilibrium.

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