<div dir="ltr">producing NS-NS binaries with mass ratios different from one is a bit problematic sometimes. There is this trick though that can help (if it was not yet implemented in the current LORENE version):<div><br></div><div>In the file C++/Source/Binaire/binaire_orbite.C, there is a routine fonc_binaire_axe on lines 799-854 that uses a secant method to determine the values for x_rot, the rotation axis of the binary, and omega, the angular momentum. Unfortunately, the secant method that tries to set the guesses for omega for each star equal to each other, om_star1=om_star2 calculates<br><br>0= om_star1 - om_star2<br><br>but either or both of these can yield a division by zero as they are calculated. We've found it helps stabilize things by solving<br><br>0 = 1.0/om_star1 - 1.0/om_star2 <br><br>which can be done by modifying line 852 accordingly. This particularly helps with divergent mass ratios. Note that this is a different file than C++/Source/Binary/binary_orbite.C, which I believe has its own problems.<br></div><div><br></div><div><br></div><div>Otherwise the FUKA branch of KADATH is very robust: <a href="https://bitbucket.org/fukaws/">https://bitbucket.org/fukaws/</a></div><div><br></div><div>Please note that I never tried to compute binaries with a mass ratio of 7.</div><div><br></div><div>Cheers,</div><div>Bruno</div><div><br></div></div><br><div class="gmail_quote"><div dir="ltr" class="gmail_attr">Il giorno mer 1 mar 2023 alle ore 12:14 Konrad Topolski <<a href="mailto:topolski@itp.uni-frankfurt.de">topolski@itp.uni-frankfurt.de</a>> ha scritto:<br></div><blockquote class="gmail_quote" style="margin:0px 0px 0px 0.8ex;border-left:1px solid rgb(204,204,204);padding-left:1ex">Hi Jimmy<br><br>The lower mass that you are asking Lorene for is not realized for neutron stars (lower mass limit >~1.0M_sun)<br>and would rather approach the mass for a brown dwarf. This lower mass and the upper theoretical limit places an upper constraint<br>on the mass ratio to be around q~2. For initial data generation, this limit is of course equation of state - dependent.<br><br>Consistent with this fact and the theoretical constructions of the equations of state,<br>such a mass ratio is not achievable in the context of neutron stars. <br><br>Out of the most extreme configurations I've seen,<br>FUKA initial data solver (publicly available) is known to achieve q~2.2 and<br>at least q~2.1 is achieved for SGRID code, LORENE q~1.82, judging<br>from the CoRe database.<br><br>I do not have much experience with Lorene, but it might not be straightforward to achieve even the<br>theoretically admissible vicinity of q~2.0 due to domain decomposition issues.<br>Perhaps someone with more experience with it could clarify what's realizable with publicly available version of Lorene.<br><br>Best regards<br>Konrad Topolski<br><br>W dniu: Środa, Marzec 01, 2023 08:52 CET, 白济民 <<a href="mailto:beki-cat@sjtu.edu.cn" target="_blank">beki-cat@sjtu.edu.cn</a>> napisał(a):<br> <blockquote type="cite" cite="http://1879165524.7522765.1677657153716.JavaMail.zimbra@sjtu.edu.cn">Hi everyone:<br>I intend to use Lorene to generate an unequal mass binary NS system with large q (with mass 1.4 Mo vs 0.2 Mo), that is, a very light NS orbiting around a standard mass NS. However, Lorene code seems to fail to generate .resu file at such large q and I wonder how can that be possible within Lorene. Is it still under development or can it be done by varying parameter settings in the corresponding parcoal file in Lorene/Codes/Bin_star directory?<br><br>I also wonder if there is a systematic procedure to adjust the parameter settings of parcoal to generate the initial data of a BNS system with small q?<br>Thanks in advance!<br>Best,<br>Jimmy<br>_______________________________________________<br>Users mailing list<br><a href="mailto:Users@einsteintoolkit.org" target="_blank">Users@einsteintoolkit.org</a><br><a href="http://lists.einsteintoolkit.org/mailman/listinfo/users" target="_blank">http://lists.einsteintoolkit.org/mailman/listinfo/users</a></blockquote><br><br><br>
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</blockquote></div><br clear="all"><div><br></div>-- <br><div dir="ltr" class="gmail_signature"><div dir="ltr"><div><div dir="ltr"><div><div dir="ltr"><div dir="ltr"><p><font color="#000000">Pr<font face="arial, sans-serif">of. Bruno Giacomazzo<br>Department of Physics<br>University of Milano-Bicocca<br></font></font><span style="color:rgb(0,0,0)"><font face="arial, sans-serif">Piazza della Scienza 3<br></font></span><span style="color:rgb(0,0,0)"><font face="arial, sans-serif">20126 Milano<br></font></span><span style="font-size:12.8px;color:rgb(0,0,0)">Italy</span></p><p><font color="#000000"><span style="font-size:12.8px">email: </span><span style="font-size:12.8px"><a href="mailto:bruno.giacomazzo@unimib.it" target="_blank">bruno.giacomazzo@unimib.it</a><br></span><span style="font-size:12.8px">phone: (+39) 02 6448 2321</span></font><br><font color="#000000"><span style="font-size:12.8px">web: </span></font><span style="color:rgb(0,0,0);font-size:12.8px"><a href="http://www.brunogiacomazzo.org/" style="font-size:12.8px" target="_blank">http://www.brunogiacomazzo.org</a></span></p><p><font color="#000000">---------------------------------------------------------------------<br><span style="font-size:12.8px">There are only 10 types of people in the world:<br></span><span style="font-size:12.8px">Those who understand binary, and those who don't<br></span><span style="font-size:12.8px">----------------------------------------------------------------------<br></span></font></p></div></div></div></div></div></div></div>