Two-Dimensional Simulations of Relativistic Extragalactic Jets Crossing an ISM/ICM Interface

Details Two-Dimensional Simulations of Relativistic Extragalactic Jets Crossing an ISM/ICM Interface Two-Dimensional Simulations of Relativistic Extragalactic Jets Crossing an ISM/ICM Interface

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pasj...51..449z&link_type=abstract

Publications of the Astronomical Society of Japan, v.51, p.449-457.

Astronomy and Astrophysics

Astronomy

7

Astrophysical Jets, Hydrodynamics, Intergalactic Medium, Numerical Methods, Relativity

Scientific paper

We have performed two-dimensional relativistic hydrodynamical simulations of initially conical axisymmetric jets using a newly developed relativistic magnetohydrodynamic simulation code. The simulation code employs a simplified total variation diminishing method. These jets emerge from the atmospheres of active galaxies and then cross a pressure-matched interface into a hotter, but less-dense, intraclustermedium, whereupon they are accelerated and collimated. We compared the nonrelativistic and relativistic jets to find any relativistic effects in this kind of propagation processes. The simulation results show that there are clear relativistic effects as well as interface impacts in several aspects. Compared with a nonrelativistic jet propagating in a uniform medium, three results are notable: (1) when a jet propagates from a higher density medium region to lower density region, the variation in the amplitude of the Mach disk between concave and convex is greater; nonrelativistic jets show this feature more obviously; (2) the interface causes the jet to undergo a quasi-periodical shrinkage and expansion, which may correspond to a chain of knots in an extragalactic jet; (3) the jet head advance velocity formula, v_h={v_0sqrt eta }/({1+sqrt eta }), should be replaced by v_h={v_0gamma_0 sqrt eta }/{(1+gamma_0 sqrt eta )}, where v_0 and gamma_0 are the velocity of the inflowing jet fluid and its Lorentz factor, respectively, and eta is the initial ratio of jet density to medium density.

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