TY - CONF
T1 - Solutions of the Wind Equation in Relativistic Magnetized Jets
Y1 - 2014
A1 - Millas, D.
A1 - Katsoulakos, G.
A1 - Lingri, D.
A1 - Karampelas, K.
A1 - Vlahakis, N.
KW - 95.30.Qd
KW - 98.58.Fd
KW - 98.62.Nx
KW - galactic winds and fountains
KW - Jets
KW - Jets and bursts
KW - Jets outflows and bipolar flows
KW - magnetohydrodynamics
KW - Magnetohydrodynamics and plasmas
KW - outflows
KW - relativity
AB - 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.
VL - 28
UR - https://ui.adsabs.harvard.edu/abs/2014IJMPS..2860200M
JO - International Journal of Modern Physics Conference Series
ER -