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General relativistic magnetohydrodynamic simulations of binary neutron star mergers with the APR4 equation of state

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Published 29 July 2016 • © 2016 IOP Publishing Ltd
, , Citation A Endrizzi et al 2016 Class. Quantum Grav. 33 164001 DOI 10.1088/0264-9381/33/16/164001

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Supplementary data

GW data. GW amplitudes are given assuming a source at 100 Mpc from the detector. Retarded time expressed in ms (milliseconds). h+ and hx have no spherical harmonics contribute included. The value stored is for the single mode l = m = 2. (295 KB, 5 x ASC)

Initial data. Each initial data tarball contains:

Movie 1. Three movies for the logarithm of the rest mass density on meridional and equatorial plane for the three magnetized models in cartesian coordinates. Evolution time in milliseconds. (4.92 MB, MP4)

Movie 2. (14.9 MB, MP4)

Movie 3. (13.6 MB, MP4)

Movie 4. Movie for the logarithm of the rest mass density on equatorial plane for the unequal mass, magnetized model with unwarped coordinates. Evolution time in milliseconds. (27.3 MB, MP4)

Movie 5. Movie for the rest mass density in cartesian coordinates. Evolution time in milliseconds. The white opaque surface identify (roughly) the surface of the compact objects, while the other transparent layers show the ejected mass + disk structure. Non-magnetized unequal mass model is shown in this movie. (4.62 MB, WEBM)

GW data. GW amplitudes are given assuming a source at 100 Mpc from the detector. Retarded time expressed in ms (milliseconds). h+ and hx have no spherical harmonics contribute included. The value stored is for the single mode l = m = 2. (295 KB, 5 x ASC) Initial data. Each initial data tarball contains: EOS.dat file containing the table (LORENE readable) used for the production of initial data. LORENE parameter files for initial configuration (par_init.d), eos (par_eos1.d, par_eos2.d), grid (par_grid1.d, par_grid2.d), binary computation (parcoal.d). LORENE model summary (calcul.d). LORENE convergence results for the model (both stars) (resconv1.d, resconv2.d). LORENE output file (input for Cactus) (resu.d) (29.2 MB, 3 x TAR) Movie 1. Three movies for the logarithm of the rest mass density on meridional and equatorial plane for the three magnetized models in cartesian coordinates. Evolution time in milliseconds. (4.92 MB, MP4) Movie 2. (14.9 MB, MP4) Movie 3. (13.6 MB, MP4) Movie 4. Movie for the logarithm of the rest mass density on equatorial plane for the unequal mass, magnetized model with unwarped coordinates. Evolution time in milliseconds. (27.3 MB, MP4) Movie 5. Movie for the rest mass density in cartesian coordinates. Evolution time in milliseconds. The white opaque surface identify (roughly) the surface of the compact objects, while the other transparent layers show the ejected mass + disk structure. Non-magnetized unequal mass model is shown in this movie. (4.62 MB, WEBM) Movie 6. Same as movie 5 for the magnetized unequal mass model. (11.3 MB, WEBM)