An Algol type binary with a δ Scuti component: RZ Cassiopeiae revisited

Details An Algol type binary with a δ Scuti component: RZ Cassiopeiae revisited An Algol type binary with a δ Scuti component: RZ Cassiopeiae revisited

Nov 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006an....327..905s&link_type=abstract

Astronomische Nachrichten, Vol.327, Issue 9, p.905

Astronomy and Astrophysics

Astronomy

7

Stars: Binaries: Eclipsing, Stars: Variables: Δ Scuti, Stars: Individual: Rz Cassiopeiae

Scientific paper

We present new BV photometry and spectroscopic observations of RZ Cassiopeiae. The light and radial velocity curves were formed by the new observations which have been analyzed simultaneously by using the Wilson-Dewinney code. The non-synchronous rotational velocity v1sin i = 76 ± 6 km s-1, deduced for the primary component from the new spectroscopic observations, was also incorporated in the analysis. A time-series analysis of the residual light curves revealed the multi-periodic pulsations of the primary component of RZ Cas. The main peak in the frequency spectrum was observed at about 64.197 c d-1 in both B and V bands. The pulsational constant was calculated to be 0.0116 days. This value corresponds to high overtones (n˜6) of non-radial mode oscillations. We find significant changes in the pulsational amplitude of the primary component from year to year. The peak-to-peak pulsational amplitude of the main frequency displays a decrease from 0.013 m in 2000 to 0.002 m in 2001 and thereafter we have found an increase again in the amplitude to 0.01 m in the year 2002. We propose the mass transfer from the cool secondary to the pulsating primary as a possible explanation for such remarkable changes in the pulsational behavior of the primary component.

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