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Radiative MHD simulations of the jets from RW Aurigae

Published online by Cambridge University Press:  24 February 2011

Ovidiu Teşileanu ,
Andrea Mignone ,
Silvano Massaglia  and
Matthias Stute
Ovidiu Teşileanu
Affiliation:
RCAPA, University of Bucharest, Str. Atomistilor nr. 405, 077125 Magurele, Romania email: [email protected]
Andrea Mignone
Affiliation:
Dipartimento di Fisica Generale, University of Turin, via P. Giuria 1, 10125 Torino, Italy
Silvano Massaglia
Affiliation:
Dipartimento di Fisica Generale, University of Turin, via P. Giuria 1, 10125 Torino, Italy
Matthias Stute
Affiliation:
Dipartimento di Fisica Generale, University of Turin, via P. Giuria 1, 10125 Torino, Italy
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Abstract

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The MHD simulations of stellar jets recently included complex models of radiative emission computation, allowing for better predictions in terms of emission line ratios. Employing also Adaptive Mesh Refinement, the large-scale propagation of jets could be followed. The simulation of multiple shockwaves originating in perturbations close to the jet origin and travelling along the jet beam allows for the construction of synthetic emission maps at various wavelengths, to be directly compared to observations. We apply this procedure for the jets originating from RW Aurigae.

Keywords

atomic processesMHDplasmasradiation mechanisms: thermalshock wavesstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 410 - 411
Copyright
Copyright © International Astronomical Union 2011

References

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Woitas, J., Ray, T. P., Bacciotti, F., Davis, C. J., & Eislöffel, J. 2002, ApJ, 580, 336CrossRefGoogle Scholar