%0 Conference Paper
%D 2014
%T Solutions of the Wind Equation in Relativistic Magnetized Jets
%A Millas, D.
%A Katsoulakos, G.
%A Lingri, D.
%A Karampelas, K.
%A Vlahakis, N.
%K 95.30.Qd
%K 98.58.Fd
%K 98.62.Nx
%K galactic winds and fountains
%K Jets
%K Jets and bursts
%K Jets outflows and bipolar flows
%K magnetohydrodynamics
%K Magnetohydrodynamics and plasmas
%K outflows
%K relativity
%X We study the bulk acceleration in relativistic axisymmetric magnetized outflows, by solving the momentum equation along the flow, the so-called wind equation. The solutions for the bulk Lorentz factor depend on the geometry of the field/streamlines through the "bunching function" S. We investigate the general characteristics of the S function and how its choice affects the acceleration. In our study, various fast rise and slow decay examples are selected for S, with a global maximum near the fast magnetosonic critical point, as required from the regularity condition. For each case we determine the terminal Lorentz factor γ_{∞} and the acceleration efficiency γ_{∞}/μ, where μ is the total energy-to-mass flux ratio (which equals the maximum possible Lorentz factor of the outflow). With proper choices of S we can achieve efficiencies greater than 50%. Last, we examine the shape of the field/streamlines with respect to the choice of the S function. The results of this work, depending on the choices of μ, can be applied to relativistic GRB or AGN jets.
%V 28
%P 1460200
%8 2014/03/1
%G eng
%U https://ui.adsabs.harvard.edu/abs/2014IJMPS..2860200M
%! International Journal of Modern Physics Conference Series