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<p>Dear Roland,</p>
<p>Thank you for your suggestion and information!</p>
<p><br>
</p>
<p>Best regards,</p>
<p>Chia-Hui</p>
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<div id="x_divRplyFwdMsg" dir="ltr"><font face="Calibri, sans-serif" color="#000000" style="font-size:11pt"><b>寄件者:</b> Roland Haas <rhaas@illinois.edu><br>
<b>寄件日期:</b> 2018年10月5日 下午 11:49:50<br>
<b>收件者:</b> 林家暉<br>
<b>副本:</b> Einstein Toolkit Users<br>
<b>主旨:</b> Re: [Users] mass estimation of neutron star</font>
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<div class="PlainText">Hello Chia-Hui,<br>
<br>
<a href="https://stellarcollapse.org">https://stellarcollapse.org</a> is your best starting point. Please have a<br>
look at the page for the publications listed there on<br>
<a href="https://www.stellarcollapse.org/node/17">https://www.stellarcollapse.org/node/17</a> in particular for the leakage code:<br>
<br>
<a href="https://sntheory.org/ottetal2013">https://sntheory.org/ottetal2013</a><br>
<a href="https://stellarcollapse.org/cc3dgrmhd">https://stellarcollapse.org/cc3dgrmhd</a><br>
<br>
and the code page for the Zelmani codes (Leakage and M1 as well as<br>
version of GRHydro):<br>
<br>
<a href="https://stellarcollapse.org/Zelmani">https://stellarcollapse.org/Zelmani</a><br>
<br>
where both the newest public version of the leakage and the M1 codes are<br>
available for download.<br>
<br>
For the R-process please look at<br>
<br>
<a href="http://sntheory.org/lippunerroberts2015">http://sntheory.org/lippunerroberts2015</a><br>
<br>
and Jonas' skynet code page:<br>
<br>
<a href="https://bitbucket.org/jlippuner/skynet">https://bitbucket.org/jlippuner/skynet</a><br>
<br>
Yours,<br>
Roland<br>
<br>
> Dear Roland,<br>
> <br>
> Thanks for your reply.<br>
> <br>
> For the previous question about r-process, I found a document(<a href="https://stellarcollapse.org/media/micra2013/moesta.pdf">https://stellarcollapse.org/media/micra2013/moesta.pdf</a>) saying that GRHydro could consider neutrino leakage. But I have no ideal
how to implement it. Is there any suggested way to deal with neutrino leakage with GRHydro (or other thorns) ?<br>
> <br>
> Thank you.<br>
> <br>
> Best regards,<br>
> <br>
> Chia-Hui<br>
> <br>
> ________________________________<br>
> 寄件者: Roland Haas <rhaas@illinois.edu><br>
> 寄件日期: 2018年10月2日 下午 09:11:21<br>
> 收件者: 林家暉<br>
> 副本: Einstein Toolkit Users<br>
> 主旨: Re: [Users] mass estimation of neutron star<br>
> <br>
> Hello Chia-Hui,<br>
> <br>
> > In addition , I would like to ask question about computation<br>
> > consumption. For the BNS merger (using .par file in the gallery<br>
> > file), it costs about 5000 core hours (48 cores for 100 hours) for<br>
> > the completed simulation (to iteration=15000). Is it reasonable? And<br>
> > is there some way to save the computational resources ? <br>
> If you want to save overall resources you could reduce the number of<br>
> cores used (assuming you do not run out of memory). For example running<br>
> on 32 cores will make it run slower but not by a factor of 48/32 so<br>
> that the total resources (number-of-cores * hours-used) goes down.<br>
> <br>
> You could also try reducing (slightly!) the resolution eg by a factor<br>
> of 1.25 which would make the simulation cheaper (but also loose<br>
> significantly in accuracy). Finally you could try and make the<br>
> simulation domain smaller, which safes a bit but not a whole lot<br>
> usually.<br>
> <br>
> You can also try and see if reducing the amount of output produced<br>
> makes any difference (though that is unlikely). This is the<br>
> outXXX_every parameters and generally everything with an _every in its<br>
> name.<br>
> <br>
> Yours,<br>
> Roland<br>
> <br>
> --<br>
> My email is as private as my paper mail. I therefore support encrypting<br>
> and signing email messages. Get my PGP key from <a href="http://pgp.mit.edu">http://pgp.mit.edu</a> .<br>
<br>
<br>
<br>
-- <br>
My email is as private as my paper mail. I therefore support encrypting<br>
and signing email messages. Get my PGP key from <a href="http://pgp.mit.edu">http://pgp.mit.edu</a> .<br>
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