CENTER FOR COMPUTATION & TECHNOLOGY

I will present results on the effect of magnetic field on the dynamics of the classical bar-mode instability of differentially rotating relativistic star models. In particular, I will show what happen to a seed purely poloidal Magnetic field super-imposed to matter unstable-equilibrium configuration and on its fate during the matter-unstable phase. We observed the growth of a toroidal magnetic field that rapidly overcome the original poloidal field as a consequence of Magneto Rotational effects.  The growth, of almost an order of magnitude, of the poloidal component during the unstable phase is observed.

Overall, we find that magnetic field seems to have a low effect on the dynamical bar-mode deformation for fields as big as 10^15 Gauss while
magnetic fields of order 10^16 Gauss suppress the purely hydrodynamical instabilities. The results are obtained performing full 3D Ideal
Magneto-hydrodynamics simulation in full General Relativity on a time scale of around 40 ms.

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