On the interaction of jets with the dense medium of the early universe

Details On the interaction of jets with the dense medium of the early universe On the interaction of jets with the dense medium of the early universe

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002phdt.........2k&link_type=abstract

PhD Thesis, Naturwissenschaftlich-Mathematische Gesamtfakultät der Universität Heidelberg, Germany. IX + 134 p. (2002)

Mathematics

2

Radio Sources, Jets, Magnetohydrodynamics

Scientific paper

In recent years, radio galaxies have been found at redshifts above five. They differ in higher radio power and emission line characteristics from sources nearby. To understand these centers of proto-galaxy-clusters, hydrodynamic jets with cooling were simulated. After validation of the 3D code NIRVANA by comparison with literature simulations, an adiabatic 2D parameter study in the relevant regime (density contrast jet/medium η ˜ 10-2 - 10-5) was performed. Characteristic cocoon shape and broadenings were found. The radial expansion can be analytically approximated by a spherical blast wave with constant energy injection. In a non-equilibrium simulation the bow shock cooled to 104K during jet propagation time (external density 1 cm-3). After global cooling and compression, the bow shock turned into a big absorber which fragmented, and should form stars in typically 104 globular clusters of 106Msolar. Filamentation and fragmentation was confirmed at high resolution. Absorbers in far-off radio galaxies and globular cluster excesses in nearby CD galaxies can be explained that way. With literature parameters of Cygnus A, a 3D simulation, for the first time with counter-jet was performed. The bow shock shows two clearly separated phases, also evident in observation. Basic jet parameters have been derived. The simulation shows characteristic X-ray features (rings) which were identified and interpreted in two sources (M87).

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