Evolution of neutron stars with toroidal magnetic fields: Axisymmetric simulation in full general relativity

Simple item page
dc.creatorKiuchi, Kenta
dc.creatorShibata, Masaru
dc.creatorYoshida, Shijun
dc.date2008-05-18
dc.date.accessioned2026-07-07T12:14:32Z
dc.date.available2026-07-07T12:14:32Z
dc.descriptionWe study the stability of neutron stars with toroidal magnetic fields by magnetohydrodynamic simulation in full general relativity under assumption of axial symmetry. Nonrotating and rigidly rotating neutron stars are prepared for a variety of magnetic field configuration. For modeling the neutron stars, the polytropic equation of state with the adiabatic index $Γ=2$ is used for simplicity. It is found that nonrotating neutron stars are dynamically unstable for the case that toroidal magnetic field strength varies $\propto \varpi^{2k-1}$ with $k\geq 2$ (here $\varpi$ is the cylindrical radius), whereas for $k=1$ the neutron stars are stable. After the onset of the instability, unstable modes grow approximately in the Alfvén time scale and, as a result, a convective motion is excited to change the magnetic field profile until a new state, which is stable against axisymmetric perturbation, is reached. We also find that rotation plays a role in stabilization, although the instability still sets in in the Alfvén time scale when the ratio of magnetic energy to rotational kinetic energy is larger than a critical value $\sim 0.2$. Implication for the evolution of magnetized protoneutron stars is discussed.
dc.descriptionaccepted to PRD
dc.identifierhttps://arxiv.org/abs/0805.2712
dc.identifierhttp://arxiv.org/abs/0805.2712
dc.identifierPhys.Rev.D78:024029,2008
dc.identifierdoi:10.1103/PhysRevD.78.024029
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/211225
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleEvolution of neutron stars with toroidal magnetic fields: Axisymmetric simulation in full general relativity
dc.typetext

Files

Collections

arXiv