Astronomy and Astrophysics – Astronomy
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24..321b&link_type=abstract
Astronomy Letters, Volume 24, Issue 3, May 1998, pp.321-331; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 381
Astronomy and Astrophysics
Astronomy
10
Scientific paper
Using the MHD approximation, we numerically solve the problem of a steady plasma outflow from the magnetospheres of astrophysical objects at large distances from them for nonrelativistic and relativistic plasma. We use the previously obtained solutions for the flow zone that is closest to the central object as the boundary conditions immediately behind the fast magnetosonic surface. An analysis of our solutions at large distances shows that they approach their asymptotic limits logarithmically slowly. How the asymptotic limit is approached depends on the field line. For a nonrelativistic plasma, the asymptotic limit near the rotation axis is approached relatively rapidly, with the formation of a jet whose characteristics are excellently described by the analytical formula derived from an analysis of the asymptotic behavior. Near the equator, the asymptotic limit is reached at infinitely large distances. For a relativistic plasma, the distance at which a jet flow is formed near the rotation axis is r_coll ~ sqrt[sigma/gamma_0^2 exp(gamma_0^3/2sigma)], where sigma is the energy flux density of the electromagnetic field per particle, and gamma_0 is the Lorentz factor of the particles. Numerical estimates indicate that these distances are much greater than the sizes of synchrotron nebulae around pulsars. We conclude that radio pulsars cannot produce jets through magnetic collimation of plasma.
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