LO Andromedae: a new close eclipsing binary system.

Details LO Andromedae: a new close eclipsing binary system. LO Andromedae: a new close eclipsing binary system.

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983geoce..11.....b&link_type=abstract

GEOS Circular on Eclipsing Binaries, No. EB 11, 7 p. (1983)

Computer Science

Periods:W Uma Stars

Scientific paper

Discovered in 1963 by R. Weber, LO And was first regarded as a pulsating star. A first ephemeris was computed using the visual observations of A. Gautschy made in 1979. Photoelectric measures made by R. Diethelm confirmed the shortness of the period. Since 1981, about 4300 estimates from the GEOS observers have led to the conclusion that the star is an EW-type eclipsing binary. That conclusion agrees well with the mean B-V of LO And. From 104 minima, the following elements were calculated: Min I = hel. JD 2,445075.6353(+/-8) + 0.3804326(+/-28) E (95% level of confidence for the error bands). It has not been possible to discriminate with certainty, between primary and secondary minimum. LO And varies from 11.20 to 11.75 v with a secondary minimum around 11.70 v. Further observations are needed.

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