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You have very high densities in your circumstellar medium, which might produce extremely short cooling times because of that quadratic density dependence. Compare your cooling time (E/Edot) to your dynamical time. I strongly suspect your SNR is already in
the momentum-driven snowplow phase, the hot interior having cooled extremely quickly.
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<div class="">- Mordecai</div>
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<div class="">On Jul 31, 2017, at 14:23, Michiel Bustraan <<a href="mailto:michiel.bustraan@astro.su.se" class="">michiel.bustraan@astro.su.se</a>> wrote:</div>
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Dear FLASH Users,<br class="">
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I've been using the cooling module in my supernova simulations, and have been seeing some unusual results.<br class="">
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My simulations involve a shock moving radially outward into a circumstellar medium.<br class="">
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My runs without cooling have good results, with the structure of the shock matching those in the literature.<br class="">
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The attached plots are the density, temperature, and radial velocity from a run without cooling.<br class="">
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I've been looking into the cooling module and implementing a fairly simple cooling function.<br class="">
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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 class="">
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the impact the cooling has on the shock doesn't seem right.<br class="">
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<span style="font-size: 12pt;" class="">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 class="">
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I wanted to ask if anyone else encountered something like this using the cooling module.<br class="">
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Also, just for assurance, I wanted to check what the cooling module actually calculates.<br class="">
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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 class="">
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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 class="">
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I know the question is a bit vague, but any advice would be appreciated.<br class="">
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Thank you,<br class="">
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Michiel Bustraan<br class="">
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<span id="cid:DDB67F4A-8633-4773-87EA-CFD9F8D9BD5C@ita.uni-heidelberg.de"><density_1d_20.png></span><span id="cid:6602BC47-572A-41E2-8191-AFD2CA6729DC@ita.uni-heidelberg.de"><temp_1d_20.png></span><span id="cid:B13ACC32-3D3C-4715-B533-D05DF5265CD8@ita.uni-heidelberg.de"><velx_1d_20.png></span></div>
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--<br class="">
Mordecai-Mark Mac Low <span class="Apple-tab-span" style="white-space: pre;"> </span>
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mmaclow (Skype, Hangout) <span class="Apple-tab-span" style="white-space: pre;">
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