Proper motion analysis of the jet of R Aquarii

Details Proper motion analysis of the jet of R Aquarii Proper motion analysis of the jet of R Aquarii

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...424..157m&link_type=abstract

Astronomy and Astrophysics, v.424, p.157-164 (2004)

Astronomy and Astrophysics

Astrophysics

4

Stars: Binaries: Symbiotic, Stars: Individual: R Aqr, Ism: Jets And Outflows

Scientific paper

We have observed the jet of R Aquarii at high resolution with the VLA in 1992.83 and in 1999.78. Observations in the first epoch have resolved the base of the jet which shows a helical structure. We cannot detect the expected new jet component at either epoch. This does not disprove the idea of periodic ejection. Either the timing inferred from the acceleration models, or the assumed periastron passage is incorrect. Alternatively, a single new component cannot be resolved due to the dense core. Proper motion analysis of the jet components shows that previously derived acceleration models do not fit our new data. Indeed, the first ˜ 1 arcsec of the jet, both to north-east and south-west, appears fixed and has slowly moving shocks at the termination points, whereas the positions of the outer components fit best a ballistic orbit. We propose that the components are formed due to enhanced matter flow at periastron, accelerated during the first 1 arcsec and then ejected as bullets. Component A at a distance of ˜ 4 arcsec from the core has broken into two parts, similar to what was previously assumed to have happened to the outermost components B and D. The disruption is probably a consequence of a reverse shock or a collision with a cloud.

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