THE JET DISK SYMBIOSIS .1. RADIO TO X-RAY-EMISSION MODELS FOR QUASARS

Starting from the assumption that radio jets and accretion disks are s ymbiotic features present in radio loud and radio quiet quasars we sca le the bulk power of radio jets with the accretion power by adding mas s- and energy conservation of the whole jet-disk system to the standar d Blandford and Konigl theory for compact radio cores. The jet is desc ribed as a conically expanding plasma with maximal sound speed c/root 3 enclosing relativistic particles and a magnetic field. Relativistic speeds of gamma(j) beta(j) greater than or similar to 5 make an additi onal confinement unnecessary and the shape is solely given by the Mach cone. The model depends on only few parameters and can be constrained by observations. Thus we are able to show that radio and X-ray fluxes (SSC emission) of cores and lobes and typical dimensions of radio lou d quasars are consistent with a jet being produced in the central engi ne. We present a synthetic broadband spectrum from radio to X-ray for a jet-disk system. The only way to explain the high efficiency of radi o loud objects is to postulate that these objects consist of 'maximal jets' with 'total equipartition' where the magnetic energy flow of the jet is comparable to the kinetic jet power and the total jets power i s a large fraction of the disk power. As the number of electrons is li mited by the accretion flow, such a situation is only possible when th e minimum Lorentz factor of the electron distribution is gamma(e,min) greater than or similar to 100 (E greater than or similar to 50MeV) or /and a large number of pairs are present. Such an electron/positron po pulation would be a necessary consequence of hadronic interactions and may lead to some interesting effects in the low frequency serf-absorb ed spectrum. Emission from radio weak quasars can be explained with an initially identical jet. The difference between radio loud and radio weak could be due to a different efficiency in accelerating relativist ic electrons on the sub-parsec scale only. Finally we demonstrate that in order to appease the ravenous hunger of radio loud jets its produc tion must be somehow linked to the dissipation process in the inner pa rt of the disk.