Photometric and spectroscopic observations of the 53 Persei type stars: Zeta Cassiopeiae

Details Photometric and spectroscopic observations of the 53 Persei type stars: Zeta Cassiopeiae Photometric and spectroscopic observations of the 53 Persei type stars: Zeta Cassiopeiae

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...287..509s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 287, no. 2, p. 509-516

Astronomy and Astrophysics

Astrophysics

4

Binary Stars, Line Spectra, Radial Velocity, Stellar Luminosity, Variable Stars, Periodic Variations, Power Spectra, Stellar Magnitude, Stellar Spectrophotometry

Scientific paper

We present the results of photometric and spectroscopic observations of the star zeta Cas. The luminosity fluctuations are inside 0.004 magnitude in the u, v, and b Stroemgren's filters. For a given night the radial velocity measurements vary inside 1 km/s. We suppose that the observed night to night radial velocity variations are due to a close binarity. The orbital period could be 11.53 days with a 2K amplitude equal 3.6 km/s. The full width at half maximum (FWHM) measurements of the 4552 A SiIII are variable from night to night inside 0.08 A. After detrending for this variation, a peak appears in the power spectrum at 0.27 day with a half amplitude of 0.01 A possibly due to a non radial g mode. We do not detect the 0.9 d. period determined by Smith (1980). So the only short time variable parameter is the shape of the line profile. This is the main characteristic of a 53 Per type star.

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