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<tt>Dear Michiel -<br>
<br>
Please consult<br>
<br>
<a class="moz-txt-link-freetext"
href="http://adsabs.harvard.edu/abs/1975MNRAS.172...55F">http://adsabs.harvard.edu/abs/1975MNRAS.172...55F</a><br>
<br>
and many papers on radiative SNRs and radiative shocks that
followed.<br>
<br>
Tomek<br>
--</tt><br>
<div class="moz-cite-prefix">On 07/31/17 08:23, Michiel Bustraan
wrote:<br>
</div>
<blockquote type="cite" cite="mid:1501503817951.81084@astro.su.se">
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<p>Dear FLASH Users,<br>
</p>
<p><br>
</p>
<p>I've been using the cooling module in my supernova simulations,
and have been seeing some unusual results.<br>
</p>
<p><br>
</p>
<p>My simulations involve a shock moving radially outward into a
circumstellar medium.<br>
</p>
<p>My runs without cooling have good results, with the structure
of the shock matching those in the literature.<br>
</p>
<p>The attached plots are the density, temperature, and radial
velocity from a run without cooling.<br>
</p>
<p><br>
</p>
<p>I've been looking into the cooling module and implementing a
fairly simple cooling function.<br>
</p>
<p>While the cooling seems to be exactly as I would expect (I plot
the variable solnData(COOL_VAR,i,j,k) = abs(dedt) against my
cooling function),<br>
</p>
<p>the impact the cooling has on the shock doesn't seem right.<br>
</p>
<p><span style="font-size: 12pt;">The cooling causes an extreme
narrowing of the shell between the forward and reverse shock,
while the reverse shock almost disappears into the shell.</span><br>
</p>
<p><br>
</p>
<p>I wanted to ask if anyone else encountered something like this
using the cooling module.<br>
</p>
<p><br>
</p>
<p>Also, just for assurance, I wanted to check what the cooling
module actually calculates.<br>
</p>
<p>Am I correct that the variable dedt, defined by the cooling
function in cool_deriv, in the Cool.F90 file, should be the
cooling rate (Lambda [erg cm^3 s^-1]) multiplied by the number
density squared?<br>
</p>
<p>And the variable EINT_VAR is the internal energy per mass [erg
g^-1]? Meaning it has to be multiplied by mass density to be the
energy density.<br>
</p>
<p><br>
</p>
<p>I know the question is a bit vague, but any advice would be
appreciated.<br>
</p>
<p><br>
</p>
<p>Thank you,<br>
</p>
<p>Michiel Bustraan<br>
</p>
</blockquote>
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