An observational study of the eclipsing nova-like variable BH Lyncis ( PG 0818 + 513)

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Abstract
We present photometric and spectroscopic observations of the novalike variable BH Lyn. The continuum and line light curves exhibit deep eclipses which recur with a period of 3.74 hr. The spectra have single-peaked Balmer and He I emission lines which exhibit a double-peaked structure near the inferior conjunction of the emission-line source. The high-excitation lines of He IIλ4686 Å and C III/N IIIλλ4640–4650 Å are very weak. Radial velocity measurements show large phase shifts in all the emission lines. We construct light-center and Doppler maps of the system which suggest that the line emission is largely non-disc in origin; for this reason we do not present a full system parameter determination. We compare and contrast BH Lyn with a number of other eclipsing nova-like variables; namely, V1315 Aql, SW Sex, DW UMa and PG 0027 + 260. The objects show basically the same behaviour, and we therefore conclude that the emission lines must be produced by a similar (unknown) mechanism. The few differences that are exhibited by BH Lyn can be attributed to the fact that the major part of our data was obtained during a temporary period of low mass transfer rate.

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