R Aquarii spectra revisited by SUMA

Abstract

We analyse the optical spectra and the UV spectral evolution of the jets and of the HII region inside the R Aquarii binary system by the code SUMA which consistently accounts for shock and photoionization. The temperature of the hot star results 80,000 K as for a white dwarf. We find that the shock velocity in the NE jet increased between 1983 and 1989. The spectral evolution between 1989 and 1991 of the SW jet indicates that a larger contribution from low density-velocity matter affects the 1991 spectra. The evolution of the UV spectra from 8/11/1980 to 26/5/1991 in the HII region indicates that the reverse shock is actually a standing shock. The results obtained by modelling the line spectra are cross-checked by the fit of the continuum SED. It is found that a black-body temperature of 2800 K reproduces the radiation from the red giant. A black-body emission component corresponding to 1000 K is emitted by dust in the surrounding of the red giant. Model calculations confirm that the radio emission is of thermal origin. We found that the NE jet bulk emission is at a distance of about 2 (15) cm from the internal system, while the distance of the SW jet bulk is about 6 (14) cm. The distance of the reverse shock from the hot source in the internal region is < 9 (13) cm.

arXiv comment9 pages, MN LaTeX style (including 6 Tables) + 5 PostScript figures. To appear in The Monthly Notices of the Royal Astronomical Society

References in corpus (5)

• Temporal Variations of Mid-IR Spectra in Late-Type Stars
• The X-ray R Aquarii: A Two-sided Jet and Central Source
• Near and mid-IR sub-arcsecond structure of the dusty symbiotic star R Aqr
• Modeling RR Tel through the Evolution of the Spectra
• Internal and external shock fronts in He2-104

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