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2011MNRAS.414.2069T - Mon. Not. R. Astron. Soc., 414, 2069-2086 (2011/July-1)
Relativistic expansion of magnetic loops at the self-similar stage – II. Magnetized outflows interacting with the ambient plasma.
TAKAHASHI H.R., ASANO E. and MATSUMOTO R.
Abstract (from CDS):
We also carried out magnetohydrodynamic (MHD) simulations of the evolution of magnetic loops to study the stability and the generality of our analytical solutions. We used the analytical solutions as the initial condition and the inner boundary conditions. We confirmed that our solutions are stable over the simulation time and that numerical results nicely recover the analytical solutions. We then carried out numerical simulations to study the generality of our solutions by changing the power-law index δ of the ambient plasma density ρ0∝r–δ. We alter the power-law index δ from δ ≃ 3.5 in the analytical solutions. The analytical solutions are used as the initial conditions inside the shock in all simulations. We observed that the shock Lorentz factor increases with time when the power-law index is larger than 3, while it decreases with time when the power-law index is smaller than 3. The shock Lorentz factor Γs can be expressed as Γs∝t(δ–3)/2 where δ is the power-law index of the ambient plasma. These results are consistent with the analytical studies by Shapiro.
Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS
Journal keyword(s): hydrodynamics - magnetic fields - stars: flare - stars: magnetic fields - stars: neutron
Simbad objects: 1
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