The simultaneous detection of 22- and 321-GHz H2O maser emission towards the symbiotic Mira R Aquarii

Details The simultaneous detection of 22- and 321-GHz H2O maser emission towards the symbiotic Mira R Aquarii The simultaneous detection of 22- and 321-GHz H2O maser emission towards the symbiotic Mira R Aquarii

1997-09-27

arxiv.org/abs/astro-ph/9709281v1

Astronomy and Astrophysics

Astrophysics

6 pages, 5 figures, LaTeX, uses mn.sty, accepted for MNRAS

Scientific paper

10.1046/j.1365-8711.1998.01237.x

We report high spatial and spectral resolution measurements of masers towards R Aqr and H1-36, both of which are examples of the sub-class of symbiotic stars that contain a long-period Mira-type variable. Our observations have resulted in the first detection of 321-GHz H2O maser action towards a symbiotic Mira - R Aqr. Comparison with simultaneous 22-GHz H2O maser data suggests the masers do not have the same properties as those in the circumstellar envelopes of field Miras. R Aqr's 22-/321-GHz peak flux density and luminosity ratios are low, as is the line-width ratio. Continuum and spectral-line maps indicate that the 22-GHz maser and free-free emission are aligned. Three mechanisms can reproduce the data with varying degrees of success. All three lead naturally to normal levels of maser emission in SiO and 321-GHz H2O and anomalously weak OH and 22-GHz H2O masers. In the most convincing model, UV radiation and a fast wind from the companion remove the Mira's envelope of dusty, molecular gas, leaving a relatively small cavity of dense, neutral material within a large, ionized nebula. Excitation temperatures suggest that 321-GHz masers are normally excited close to the Mira whilst 22-GHz masers are more remote; in R Aqr, therefore, the 22-GHz masers do not form under optimum conditions. Instead, we see weak and narrow lines that form closer to the Mira, consistent with our high-resolution maps.

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