Variations of the v = 0, 1, 2, and 3, J = 1-0 SiO Masers of R Cassiopeia

Details Variations of the v = 0, 1, 2, and 3, J = 1-0 SiO Masers of R Cassiopeia Variations of the v = 0, 1, 2, and 3, J = 1-0 SiO Masers of R Cassiopeia

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...678.1324m&link_type=abstract

The Astrophysical Journal, Volume 678, Issue 2, pp. 1324-1328.

Astronomy and Astrophysics

Astronomy

1

Stars: Circumstellar Matter, Masers, Stars: Individual (R Cassiopeia)

Scientific paper

The v=0, 1, 2, and 3, J=1-0 SiO maser spectra of R Cassiopeia have been observed with high phase resolution over a time span of approximately 2.6 stellar periods. A time lag cross-correlation analysis has been performed on the entire data set and on two subsets of the data. The analysis indicates that the variations in the emission of the v=1 and 2 states were most highly correlated at lag zero during the entire period of observation. During one complete cycle of the star, the v=0, J=1-0 emission was most highly correlated with the v=1 and 2 at a lag of -1, indicating that the v=0 emission varied in advance of the excited vibrational state emission. The lags represented 0.1 pulsation periods of the star, or a 43 day time period for these analyses. During a second cycle of the star the v=0 and v=2 emissions did not exhibit a maximum near the phase of 0.2 and were not highly correlated with the v=1 emission. The lags represented 0.05 periods of the star for this analysis. The v=0 emission generally had relatively low contrast between its maximum and minimum and had several relative maxima during a stellar period. The v=3 emission was observed to occur at various phases of the star. These observations further constrain possible models of maser pumping.

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