Relastro @ ITP - Goethe University, Frankfurt | Crustal magnetic field amplification in BNS mergers: Co-rotating sources of magnetic energy @relastroitp-goetheuniversi1616 | Uploaded 1 year ago | Updated 4 hours ago
The movie shows the merger and post-merger evolution of two equal mass
neutron star binaries with a total mass of approximately 2.5 solar
masses. The orbital rotation of the binary is counteracted by rotating by (half of) the phase angle of the gravitational wave strain, to achieve an approximately co-rotating frame. The 2D slices of the sources and sinks of magnetic-energy density are shown for the xy-plane. Red color coding shows the regions where the magnetic energy is increasing at the expense of the available kinetic energy while blue color coding shows the locations of decreasing magnetic energy corresponding to regions where the magnetic field is doing work on the fluid. The contours of constant baryonic density are shown in dashed (10^13 g cm^-3) and solid (7x10^14 g cm^-3) green lines. The two configurations differ by having different magnetic-field topologies, i.e. the left column shows the standard full-configuration with magnetic fields permeating the whole stellar structure while the right column shows the crust-configuration where magnetic fields are concentrated only in the crust after having been expelled from the core.
Publications:
arxiv.org/abs/2211.13661
Credits:
Michail Chabanov, Konrad Topolski, Samuel Tootle, Elias Most, Luciano Rezzolla
Links:
Relativistic Astrophysics group page: https://relastro.uni-frankfurt.de/
JETSET page: jetset-erc.org
ELEMENTS page: https://elements.science
The movie shows the merger and post-merger evolution of two equal mass
neutron star binaries with a total mass of approximately 2.5 solar
masses. The orbital rotation of the binary is counteracted by rotating by (half of) the phase angle of the gravitational wave strain, to achieve an approximately co-rotating frame. The 2D slices of the sources and sinks of magnetic-energy density are shown for the xy-plane. Red color coding shows the regions where the magnetic energy is increasing at the expense of the available kinetic energy while blue color coding shows the locations of decreasing magnetic energy corresponding to regions where the magnetic field is doing work on the fluid. The contours of constant baryonic density are shown in dashed (10^13 g cm^-3) and solid (7x10^14 g cm^-3) green lines. The two configurations differ by having different magnetic-field topologies, i.e. the left column shows the standard full-configuration with magnetic fields permeating the whole stellar structure while the right column shows the crust-configuration where magnetic fields are concentrated only in the crust after having been expelled from the core.
Publications:
arxiv.org/abs/2211.13661
Credits:
Michail Chabanov, Konrad Topolski, Samuel Tootle, Elias Most, Luciano Rezzolla
Links:
Relativistic Astrophysics group page: https://relastro.uni-frankfurt.de/
JETSET page: jetset-erc.org
ELEMENTS page: https://elements.science
