Observations of late-type stars in the waver vapor radio line. II: The long-period variable RR Aquilae

Details Observations of late-type stars in the waver vapor radio line. II: The long-period variable RR Aquilae Observations of late-type stars in the waver vapor radio line. II: The long-period variable RR Aquilae

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998arep...42..346b&link_type=abstract

Astronomy Reports, Volume 42, Issue 3, May 1998, pp.346-361

Astronomy and Astrophysics

Astronomy

8

Scientific paper

Results of observations of the Mira Ceti variable RR Aql in the 1.35-cm water-vapor line are presented. The observations were carried out on the 22-m radio telescope of the Pushchino Radio Astronomy Observatory in 1980-1997 (JD 2444306-2445689 and 2446587-2450631). The observations are compared with published data on the visual light curve of RR Aql and its emission in the OH and H2O lines. Sixteen variability cycles of RR Aql (P = 394.78d) are covered. Profiles of the H2O maser emission lines for 81 epochs are presented. Beginning from 1989, a rise of the H2O maser activity in RR Aql was observed, especially soon after its visual maximum in September 1992, when the peak flux density in the H2O line exceeded 500 Jy. By the beginning of 1994, the maser intensity again faded to a level <100 Jy. As in a number of other Mira variables, RR Aql shows a correlation of the H2O line flux density with its brightness variations: in general, the maser intensity follows the optical variability with some phase lag. However, the delay (up to 200d, or nearly 0.5p) is longer than in other H2O-maser Mira variables (on average 0.1p-0.3p). A model is considered in which the maser variability is the result of the joint influence of a shock wave propagating in the circumstellar envelope and variability of the radio continuum of the stellar photosphere. There are indications that the variations of the integrated H2O line flux and mean radial velocity of the maser emission have a quasi-periodic character over a time scale of 14-15 years. Estimates of the distance to RR Aql are critically re-examined. A new estimate is obtained based on the M_V_P relationships: r = 400 pc.

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