Resistive GRMHD simulations of rotating neutron stars show resistivity changes magnetic field geometries, suppresses instabilities, and lowers GW emission amplitude while maintaining a consistent 9:1 poloidal-to-toroidal energy ratio over 100 ms.
Equilibrium models of relativistic stars with a toroidal magnetic field
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abstract
We have computed models of rotating relativistic stars with a toroidal magnetic field and investigated the combined effects of magnetic field and rotation on the apparent shape (i.e. the surface deformation), which could be relevant for the electromagnetic emission, and on the internal matter distribution (i.e. the quadrupole distortion), which could be relevant for the emission of gravitational waves. Using a sample of eight different cold nuclear physics equations of state, we have computed models of maximum field strength, as well as the distortion coefficients for the surface and the quadrupolar deformations. Surprisingly, we find that non-rotating models admit arbitrary levels of magnetization, accompanied by a growth of size and quadrupole distortion to which we could not find a limit. Rotating models, on the other hand, are subject to a mass-shedding limit at frequencies well below the corresponding ones for unmagnetized stars. Overall, the space of solutions can be split into three distinct classes for which the surface deformation and the quadrupole distortion are either prolate and prolate, oblate and prolate, or oblate and oblate, respectively. We also derive a simple formula expressing the relativistic distortion coefficients, which allows one to compute the surface deformation and the quadrupole distortion up to significant levels of rotation and magnetization, essentially covering all known magnetars. Such a formula replaces Newtonian equivalent expressions that overestimate the magnetic quadrupole distortion by about a factor of 6 and are inadequate for strongly relativistic objects like neutron stars.
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Axial modes of anisotropic neutron stars show mass-scaled frequency and damping time with nearly universal quadratic dependence on compactness, insensitive to EOS and anisotropy model.
Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.
citing papers explorer
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General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars
Resistive GRMHD simulations of rotating neutron stars show resistivity changes magnetic field geometries, suppresses instabilities, and lowers GW emission amplitude while maintaining a consistent 9:1 poloidal-to-toroidal energy ratio over 100 ms.
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On the non-radial oscillations of realistic anisotropic neutron stars: Axial modes
Axial modes of anisotropic neutron stars show mass-scaled frequency and damping time with nearly universal quadratic dependence on compactness, insensitive to EOS and anisotropy model.
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Impact of Anisotropy on Neutron Star Structure and Curvature
Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.