Light variability of Sigma Scorpii

Details Light variability of Sigma Scorpii Light variability of Sigma Scorpii

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...140..223g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 140, no. 2, Nov. 1984, p. 223-229.

Astronomy and Astrophysics

Astronomy

7

Binary Stars, Light Curve, Stellar Oscillations, Variable Stars, Ultraviolet Astronomy

Scientific paper

The light variability of the spectroscopic binary and Beta Cephei star Sigma Scorpii is studied in view of Van Hoof's (1966) observations, which when subjected to period analyses in individual years reveal two oscillations whose periods and mean light curves do not exhibit any detectable year-to-year variation. Period analyses of the light observations grouped in orbital phase intervals show that the largest amplitude oscillation found in the individual years is the only oscillation in observations grouped along the binary orbit. The light variability of Sigma Sco can be modelled by two mathematically equivalent, but physically different, models: two intrinsic pulsations with constant periods and amplitudes, or one intrinsic pulsation in which mean light curve amplitude and shape are modulated by tidal action.

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