The structure of knots in variable stellar jets-II. Asymmetric knots

Details The structure of knots in variable stellar jets-II. Asymmetric knots The structure of knots in variable stellar jets-II. Asymmetric knots

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.272..785f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 272, Issue 4, pp. 785-799.

Astronomy and Astrophysics

Astronomy

37

Shock Waves, Stars: Pre-Main-Sequence-, Ism: Jets And Outflows

Scientific paper

Recent observations of jets associated with young stars (Herbig-Haro jets) shows that knots of optical emission in such jets move at about the same speed as the jet fluid. It now seems to be generally accepted that this means that the knots are caused by variations in the ejection velocity at the source. In a previous paper, we presented numerical simulations of the flow in one of these knots when the density of the external medium was so small that the dynamic pressure due to the motion of the knot was negligible compared to the pressure in the knot. In the present work, we consider cases in which the external medium exerts a significant dynamic pressure, and show that this has a considerable effect on the flow in the knot and eventually disrupts the knot completely.

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