Variability of the H2O maser associated with the Mira variable RS Virginis

Details Variability of the H2O maser associated with the Mira variable RS Virginis Variability of the H2O maser associated with the Mira variable RS Virginis

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...376..928l&link_type=abstract

Astronomy and Astrophysics, v.376, p.928-940 (2001)

Astronomy and Astrophysics

Astrophysics

6

Stars: Variables: General, Circumstellar Matter, Stars: Individual: Rs Vir, Radio Lines: Stars, Masers, Shock Waves

Scientific paper

The results of observations of the H2O maser emission (lambda = 1.35 cm) of the Mira-type variable star RS Vir are presented. The observations were carried out in 1981-2001 (JD=2 444 900-2 451 995) on the RT-22 radio telescope of the Pushchino Radio Astronomy Observatory (Russia). The variability curve of the H2O maser emission integrated flux F(H2O) of RS Vir correlates with its visual light curve with some phase delay Delta varphi =(0.05-0.35)P (P is the star's period). The delay variations seem to be periodic at a timescale of 19-20 years (``superperiod'' of the maser variations). If the variability of the H2O maser RS Vir is caused by periodic action of pulsation-driven shock waves, the shock travel time from the photosphere to the inner boundary of the H2O maser shell can be as long as (3-5)P. Another explanation is that maser variations may be connected with changing gas density in the masering region of the circumstellar envelope. In particular, long-term maser variations (the ``superperiod'') may be caused by changing mass loss rate dot M.

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