Patrick Chi-Kit Cheong, Antonios Tsokaros, Milton Ruiz, Fabrizio Venturi, Juno Chun Lung Chan, Anson Ka Long Yip, and Kōji Uryū
Date: September 17, 2024 arXiv:2409.10508
Abstract
We present the first general-relativistic \emph{resistive} magnetohydrodynamics simulations of self-consistent, rotating neutron stars with mixed poloidal and toroidal magnetic fields. Specifically, we investigate the role of resistivity in the dynamical evolution of neutron stars over a period of up to 100 ms and its effects on their quasi-equilibrium configurations. Our results demonstrate that resistivity can significantly influence the development of magnetohydrodynamic instabilities, resulting in markedly different magnetic field geometries. Additionally, resistivity suppresses the growth of these instabilities, leading to a reduction in the amplitude of emitted gravitational waves. Despite the variations in magnetic field geometries, the ratio of poloidal to toroidal field energies remains consistently 9:1 throughout the simulations, for the models we investigated. ā
Juno Chun Lung Chan, Patrick Chi-Kit Cheong, Milton Ruiz, Antonios Tsokaros, Kōji Uryū, Fabrizio Venturi, and Anson Ka Long Yip
Uniformly rotating magnetar, model A2 in arXiv:2111.00013. Evolution with resistivity $\eta= 10^{-6}$ (nearly ideal MHD)
Same as above, zoomout.
Uniformly rotating magnetar, model A2 in arXiv:2111.00013. Evolution with resistivity $\eta= 10^{-4}$
Same as above, zoomout.
Uniformly rotating magnetar, model A2 in arXiv:2111.00013. Evolution with resistivity $\eta= 10^{-2}$
Same as above, zoomout.