New variability types

The new variability types (ZZO, AM, R, BE, LBV, BLBOO, EP, SRS, LPB) have been added in the Name-Lists 67- 77 and in the GCVS vol.V.

ZZO - ZZ Cet type variables of the DO spectral type showing HeII and CIV absorbtion lines in their spectra.
AM - AM Her type variables; close binary systems consisting of a dK-dM type dwarf and of a compact object with strong magnetic field, characterized by variable linear and circular polarization of light. The total range of light variations may reach 4-5 mag V.
R - Close binary systems characterized by the presence of strong reflection (re-radiation) of the light of the hot star illuminating the surface of the cooler companion. Light curves are sinusoidal with the period equal to Porb, maximum brightness coinciding with the passage of the hot star in front of the companion. The eclipse may be absent. The range of light variation is about 0.5-1.0mag V (KV Vel).
BE - It becomes more and more clear that, although the majority of Be stars are photometrically variable, not all of them could be properly called GCAS variables. Quite a number of them show small-scale variations not necessarily related to shell events; in some cases the variations are quasi-periodic. By now we are not able to present an elaborated system of classification for Be variables, but we adopt a decision that in the cases when a Be variable cannot be readily described as a GCAS star we give simply BE for the type of variability.
EP - Stars showing eclipses by their planets. Prototype: V0376 Peg.
SRS - Semiregular pulsating red giants with short period (several days to month), probably high-overtone pulsators. Prototype: AU Ari.
LPB - For comparatively long-period pulsating B stars (periods exceeding (LBV) one day).
BLBOO - The so-called "anomalous Cepheids", i.e. stars with periods characteristic of comparatively long-period RRAB variables, but considerably brighter by luminosity (BL Boo = NGC 5466 V19).

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