Titlebook: Astrophysical Jets and Their Engines; Wolfgang Kundt Book 1987 D. Reidel Publishing Company, Dordrecht, Holland 1987 Accretion.Galaxy.Quas

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Magnetic Equilibria of Jets,ly at the head of a jet. Propagating equilibria probably involve a compressed current region surrounded by a plasma halo carrying a return current. Magnetic fields will generally be twisted, with the azimuthal field B. confining the hotter synchrotron-bright inner region, where the axial field B. is

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Stability of Magnetic Jet Equilibria,s exceed the Alfven speed. Traditional MHD modes (kink, pinch) have reduced growth rates in flowing jets. If the confining field threads a surrounding dense cocoon, this lowers the growth rates for wavelengths exceeding the jet radius, since motions must drag this cocoon mass along with the perturba

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Zeitgenössische Bezüge in Frankreichc Nuclei (=AGN), Young Stellar Objects (=YSO), Binary Neutron Stars and Binary White Dwarfs. This similarity is remarkable in view of the vastly different environments and contrasts with the heterogenous models which have been advanced for their description.

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Carolin Meister,Wilhelm Roskammipolar flows and jets from compact stars are similar and driven by the cores of accretion disks. Some difficulties of the black-hole model are discussed, in particular the problem of the missing ashes. The (super-)massive magnetised core model of an accretion disk (=SMC) is revisited.

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https://doi.org/10.1057/9781137323408features in all wavelengths from radio to gamma rays; the jets of Sco X-1 and Cyg X-3 are only evident in the radio region. Observational features for the three systems, as X-ray binaries, are summarised and compared. A possible common model for the central engine, involving a fast spinning neutron

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