44 times of minimum and first ephemeris for the EW star FZ Orionis.

Details 44 times of minimum and first ephemeris for the EW star FZ Orionis. 44 times of minimum and first ephemeris for the EW star FZ Orionis.

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983geoce...8.....f&link_type=abstract

GEOS Circular on Eclipsing Binaries, No. EB 8, 6 p. (1983)

Physics

Periods:Beta Lyrae Stars, W Uma Stars, Eclipsing Binaries:Ephemerides

Scientific paper

FZ Ori is an under-studied star. The 1.597? day period, given in the GCVS (1969) is erroneous. This conclusion is supported by the present analysis of 1229 visual estimates made by the author in 111 nights from 1976 to 1982. 44 minima (standard deviation 13.5 mn) have been observed, leading to the following ephemeris: Min I = hel. JD 2,444,024.4583(+/-14) + 0.3999866(+/-18) E (95% level of confidence for the error bands). FZ Ori is an EW-type star. Owing to the great number of observations, it has been possible to discriminate the primary minima from the secondary ones, despite their rather close amplitudes. The range of the v-variations is a rough estimation. The probable v-magnitudes are: Max 10.7, Min I 11.3, Min II 11.25.

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