Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.322..166l&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 322, Issue 1, pp. 166-176.
Astronomy and Astrophysics
Astronomy
7
Methods: Numerical, Ism: Clouds, Ism: Jets And Outflows, Galaxies: Active, Galaxies: Individual: Mrk 573, Galaxies: Seyfert
Scientific paper
The narrow-line regions of some Seyfert galaxies show evidence for nuclear jets interacting with the rotating interstellar gas; this is shown by point-symmetric emission-line structures in, for example, Mrk 573 and NGC 3393. We study this situation with numerical simulations of a jet in a sidewind of uniform density but linearly increasing velocity as one moves from the source. We use a new three-dimensional hydrodynamic code on a binary adaptive grid. We consider two different models, one with a cocoon expansion speed higher and one with expansion speed lower than the ISM speed. We find that the model with high cocoon expansion speed is similar to results from previous calculations without a sidewind, except for minor asymmetries. However, model B with the slow expansion speed and fast wind speed shows considerable qualitative differences. The jet hits and bounces off the dense cooling envelope, which is dragged by the sidewind into the straight path of the jet. The path of the jet within the cocoon is straight as long as the extended hot cocoon acts as a shield. Once the jet hits the cold envelope of the cocoon it is bent directly by the ram pressure of the ambient medium and follows a parabola of the third degree, which we derive as an analytical approximation for the path. The region where the jet hits the envelope is the start of strong radio emission. This point moves towards the source with age of the jet and its bending angle. We therefore find a possible observable correlation between the distance of the first strong radio knot and the overall bending of jets in Seyfert galaxies. A comparison of our results with observations of Mrk 573 shows that the essential structural and spectral features can be reproduced by choosing an appropriate viewing angle and evolutionary stage. Looking approximately along the original jet direction a structure is found which strongly resembles an ionization cone. Hence caution should prevail when interpreting these sorts of structure within the narrow-line region of Seyfert galaxies.
Lim Andrew J.
Steffen Wolfgang
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