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Astron. Astrophys. 362, 780-785 (2000)
A numerical simulation of the W 50-SS 433 system
P.F. Velázquez * and
A.C. Raga
Instituto de Astronomía (UNAM), Ap. Postal 70-264, CP: 04510, México D.F., México (pablov, raga@astroscu.unam.mx)
Received 12 July 2000 / Accepted 25 August 2000
Abstract
We present results of numerical simulations performed to study the evolution and interaction of jets propagating inside of Supernova Remnants (SNRs). There are new observations which show this kind of jet/SNR interaction (Dubner et al. 1998, Gaensler et al. 1998). From our numerical simulations, we compute synchrotron emission maps, in order to directly compare the numerical results with the radio maps.
Our aim is to explain the strange morphologies some SNRs exhibit in the radio-continuum, such as the case of SNR W 50 in which a shell is interacting with the jets from the SS 433 source. In recent radio images (at 328 and 1465 MHz, Dubner et al. 1998), the SNR W 50 shows a helical structure in its Eastern lobe.
Our numerical results are consistent with the radio-continuum observations, and reveal that a probable origin for the helical structure in the Eastern lobe of W 50, is the generation of incident and reflected secondary shock waves in the jet beam. Furthermore the simulations show that the cocoon gas is pushing out the SNR shell, filling up its interior, and increasing the expansion velocity of the shell.
Key words: ISM: supernova
remnants 
stars: supernovae: individual:
W 50
ISM: jets and
outflows
hydrodynamics
methods: numerical
* P.F.V. is a Post-doctoral Fellow of the Secretaría de Relaciones Exteriores de México, Programa Cuauhtémoc II
Send offprint requests to: A.C. Raga
Contents
- 1. Introduction
- 2. The model
- 3. Results
- 4. Discussion
- Acknowledgements
- References
© European Southern Observatory (ESO) 2000
Online publication: October 24, 2000
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