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Up: HL Aurigae: A

1. Introduction

HL Aur was discovered to be a variable star by Hoffmeister (1949). Kippenhahn (1953) classified it as a tex2html_wrap_inline987 Lyr-type star with the primary and secondary eclipse depths of 1.10 mag and 0.35 mag respectively. He deduced the first ephemeris and an orbital period of tex2html_wrap_inline989. Kippenhahn (1955) also published 15 times of minimum and a complete photographic light curve. Almost at the same time, a total of 14 times of minimum were secured by Pfau (1955), and he also obtained an ephemeris similar to that given by Kippenhahn (1955).

Subsequent times of minimum have been published by many authors (Tsesevitch 1956; Quester 1978; Locher 1979; Fernandes 1983; Moscher & Kleikamp 1989, 1990), but most of them being visual or photographic observations except those by Fernandes which were photoelectric. After an observational information of HL Aur supplied by us (1994), Gray & Samec (1995) published photoelectric UBV light curves and four times of minimum. Götz & Wenzel (1961) gave its spectral type to be F4. In general, little attention was paid to this system in the past.

In our search of probable near-contact binary systems, the short period eclipsing binary HL Aur was put on the observational program. In this paper, we present our first photoelectric light curves of HL Aur as well as a photometric analysis.

Copyright by the European Southern Observatory (ESO)