@conference {21904,
	title = {Solutions of the Wind Equation in Relativistic Magnetized Jets},
	volume = {28},
	year = {2014},
	month = {2014/03/1},
	pages = {1460200},
	abstract = {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<SUB>$\infty$</SUB> and the acceleration efficiency γ<SUB>$\infty$</SUB>/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.},
	keywords = {95.30.Qd, 98.58.Fd, 98.62.Nx, galactic winds and fountains, Jets, Jets and bursts, Jets outflows and bipolar flows, magnetohydrodynamics, Magnetohydrodynamics and plasmas, outflows, relativity},
	url = {https://ui.adsabs.harvard.edu/abs/2014IJMPS..2860200M},
	author = {Millas, D. and Katsoulakos, G. and Lingri, D. and Karampelas, K. and Vlahakis, N.}
}
