Hi Beyhan, As there are many subtleties to measuring angular momentum in GR, email is a very inefficient means to communicate. If you'd like to, I would be willing to try and address your question over a Google Hangout.
-Zach * * * Prof. Zachariah Etienne Physics & Astronomy Dept. West Virginia University http://astro.phys.wvu.edu/zetienne/ http://blackholesathome.net <https://blackholesathome.net> On Wed, Mar 4, 2020 at 11:22 AM Beyhan Karakaş <[email protected]> wrote: > Dear to whom it may concern, > > I am interested in determining the spin of the remnant which are > resulted from binary neutron star (initially are in irrotational > configuration) merger . How could the method to determine the final spin > differ (if it does) in case of remnant is a black hole or a neutron star. > For the former case, I suppose QuasiLocalMeasures parameter > "begin_qlm_calculations_after" along with AHFinderDirect parameter > "find_after_individual" should be set to the time/iteration that the black > hole formed. If this is not the case, please clarify how could it be > determined? In addition, is there a way to find the evolution of the spin > and orbital eccentricity of the binary? > > Best regards, > > Beyhan. > _______________________________________________ > Users mailing list > [email protected] > http://lists.einsteintoolkit.org/mailman/listinfo/users >
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