Simulations of the supersonic radiative jet propagation in plasmas

Details Simulations of the supersonic radiative jet propagation in plasmas Simulations of the supersonic radiative jet propagation in plasmas

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aps..apr8he022r&link_type=abstract

American Physical Society, 2008 APS April Meeting and HEDP/HEDLA Meeting, April 11-15, 2008, abstract #8HE.022

Astronomy and Astrophysics

Astrophysics

Scientific paper

The supersonic plasma jets are ubiquitous in astrophysics. We focus our attention on the jets emanated Herbig-Haro objects. They have velocities of a few hundred km/s and extending for a parsec. The interaction of the jets with the surrounding matter produces two structures at the jet head: the bow shock and the Mach disk. The radiative cooling of these shocks affects strongly the jet dynamics. A tool to understand the physics of these jets is the laboratory experiment. The supersonic jet-plasma interaction with surrounding plasma was studied on the PALS laser facility [1]. A collimated high-Z plasma jet with a velocity exceeding 400 km/s was generated and propagated over a few millimeters length. The jet radiative cooling is an important mechanism of jet formation, and propagation similarly to what was shown in the astrophysical context [2]. We study the jet propagation in plasmas and structure of the interaction zone using 2D ALE radiative code CHIC. A comparison between the adiabatic and radiative jets for various relative density ratios is performed. The bow shock and Mach disk evolution and their dependence are studied. A multigroup treatment of the radiative transport makes important differences in the shock structure, compared to the model [2] of radiative losses. [1] Nicolaï, Ph., 2006 et al. Phys. of Plasmas 13, 062701 [2] Blondin, J. M. et al., 1990 Astr. Phys. J. 360, 370

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