Photometric behaviour of the Be star EW Lacertae

Details Photometric behaviour of the Be star EW Lacertae Photometric behaviour of the Be star EW Lacertae

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119...73j&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Astronomy and Astrophysics

Astrophysics

2

B Stars, Light Curve, Periodic Variations, Stellar Spectrophotometry, Ubv Spectra, Nocturnal Variations, Spectrum Analysis

Scientific paper

The data of Harmanec et al. (1980) are used, together with night-to-night and short term UBV light curve variation observations obtained during 1982-1984, in order to study the long term photometric variability of EW Lac. Three minima appear in the UBV light curves with interval between minima of about 50-60 days; the depths of the minima are different each time and tend to become deeper with time in all UBV curves. These erratic light changes are thought to be related to the ending of the active phase of the shell, as suggested by Koruge and Suzuki (1984).

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