High-resolution spectroscopy of the inner R Aquarii nebula - Evidence for bow shock excitation by collimated wind from the symbiotic system

Details High-resolution spectroscopy of the inner R Aquarii nebula - Evidence for bow shock excitation by collimated wind from the symbiotic system High-resolution spectroscopy of the inner R Aquarii nebula - Evidence for bow shock excitation by collimated wind from the symbiotic system

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...257..228s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 257, no. 1, p. 228-244.

Astronomy and Astrophysics

Astrophysics

19

Nebulae, Shock Waves, Stellar Spectrophotometry, Stellar Winds, Symbiotic Stars, Electron Density (Concentration), Emission Spectra, H Ii Regions, Line Spectra, Stellar Mass Ejection

Scientific paper

High-resolution long slit spectra of the R Aquarii nebula are discussed. The data confirm that the nebula consists of two expanding hour glass-like shells which have a common bipolar axis and are attributed to two different ejection events. Major changes have ocurred between 1983 and 1987. The spike features observed represent condensations of the inner shell. It is suggested that the brightening of jet-like features in the inner nebula is due mainly to shock excitation. Observed line widths indicate that bow shocks are produced by supersonic wind from the symbiotic system. The distribution of the shock-excited features suggests that the wind flow is bipolar and highly collimated. The spectroscopic data confirm line emission from the central compact H region which appears to be expanding at a velocity of 40 km/s. The expansion may be bipolar with higher velocities in the polar directions.

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