Kelvin-Helmholtz instability in three dimensional radiative jets

Details Kelvin-Helmholtz instability in three dimensional radiative jets Kelvin-Helmholtz instability in three dimensional radiative jets

2000-06-15

arxiv.org/abs/astro-ph/0006212v1

Astronomy and Astrophysics

Astrophysics

15 pages containing 13 postscript figures; uses A&A macros. To appear in Astronomy and Astrophysics

Scientific paper

The analysis of the stability properties of astrophysical jets against Kelvin-Helmholtz (or shear-layer) instabilities plays a basic role in the understanding the origin and physical characteristics of these objects. Numerical simulations by Bodo et al. (1998) have shown that the three-dimensional non-linear evolution of KH instabilities in supersonic jets is substantially faster than in the two-dimensional case, leading to a cascade of modes towards smaller scales and a very effective mixing and momentum transfer to the ambient medium. On the other hand, Rossi et al. (1997) and Micono et al. (1998) found, in two dimensions, that radiative losses tend to reduce and delay mixing effects and momentum transfer to the ambient medium. In this paper, as a logical next step, we investigate the effects of radiative losses on the stability of 3D supersonic jets, assuming that the internal jet density is initially lower, equal and higher than the ambient medium, respectively. We find that light and equal-density radiative jets evolve in a qualitatively similar fashion with respect to the corresponding adiabatic ones. Conversely, we note substantial differences in the evolution of heavy jets: they remain more collimated and do not spread out, while the momentum gained by the ambient medium stays within ~ 5 jet radii.

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