PsiMeudon

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$/AEI1998\$ $/AEI2001\$ $/NCSA1995\$ $/NCSA1999\$ $/Others\$
$/BlackHoles\$ $/BrillWaves\$ $/NeutronStars\$
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Weyl Scalar fields from Orbiting Binary Neutron Stars

Shown are red/orange volumetric isovalues of Re{\Psi_4} and blue volumetric isovalues of Re{\Psi_0}, together with isosurfaces of the neutron star's density (red).

In an asymptotically spherically symmetric case Re{\Psi_4} can be interpreted as the outgoing component of the even-parity gravitational waves and Re{\Psi_0} as the ingoing component. This interpretation clearly breaks down in non-spherically symmetric regions, as in particular in the near region around orbiting neutron stars.

However, some similar behaviour seems to take place here, too, as the orange Re{\Psi_4}-filaments turn to flow outwards and the blue Re{\Psi_0}-filaments turn to flow inward. In the inner region, a Re{\Psi_4} and a Re{\Psi_0}-bulge appear to be in corotation with the neutron stars, with the Re{\Psi_4}-bulge beeing somewhat advanced as compared to the Re{\Psi_0}-bulge.

Some dipole-like wave structure appears to leave the computation domain early during evolution, leaving mainly noisy ripples of drifting structurs behind.

Simulation code:

AEI , WashU
Meudon Initial Data: Silvano Bonazzola, Eric Gourgoulhon and Jean-Alain Marck
(see gr-qc/9810072 and gr-qc/9904040)

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