Helically symmetric astrophysical jets
Astrophysical jets are modeled outside of their accretion disks by the helically symmetric MHD equilibria. The derived equilibria are smooth, have no current sheets, and no discontinuities. The obtained exact solutions to the MHD equilibrium equations generalize the Chandrasekhar equipartition solution and depend upon two arbitrary functions, alpha(psi) and the plasma density rho(psi)>/=0, and 2K+2 arbitrary parameters gamma,a(N),a(mn),b(mn). The total kinetic and magnetic energy of the jet and its mass are finite in any layer c(1)<z<c(2). In view of a rapid decreasing of the magnetic field B in the transversal direction, the modeled jets are highly collimated.
Bogoyavlenskij
OI
Department of Mathematics, Queen's University, Kingston, K7L 3N6 Canada and Steklov Mathematical Institute, Moscow 117 966, Russia.