Changes between Version 21 and Version 22 of u/erica/radtimescales


Ignore:
Timestamp:
04/04/16 12:57:12 (9 years ago)
Author:
Erica Kaminski
Comment:

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  • u/erica/radtimescales

    v21 v22  
    159159[[latex($\boxed{t_{fs}=\frac{L}{c}\approx\frac{1.5e+17}{3e+10}= 57 ~days}$)]]   
    160160
     161Given these timescales, the diffusion wave probably won't be strongly peaked, yet will be broad -- traveling close to the speed of light. If my 'assumptions' were correct about a pre-stellar core (their average size and mass), then given their 'average density' and the rosseland mean opacity, we see that they are in the optically thin limit for diffusion. Given cores are not optically thin, this means that either the density assumption is way off (they should be centrally concentrated), or setting the scale height = box radius is off (perhaps for an optically thick core the scale height should be greater than the core size (so that the energy is roughly constant throughout the core).
     162
     163Tackling this slightly differently could be like confining the core to a smaller dimension so that we were ensuring we would be in the optically thick limit. That is, beginning by constraining [[latex($\lambda\approx 1/3$)]]. Then, we should be able to predict the timescale over which we would see a well-defined 'diffusion wave' propagate through the grid.
     164
    161165''' Coupling time estimate '''
    162166