Abstract
BL Her Stars are primarily Population II Cepheids with periods between one and three days. On the H-R diagram they are about 1mbrighter than the RR Lyrae variables but below the W Virginis variables. They are not as blue as the so-called anomalous Cepheids. Typically these stars are metal deficient, but notable exceptions are the prototype BL Her and V553 Cen with solar type abundances (Smith, et al. 1978). Their evolutionary status given by Sweigart and Gross (1976) puts them on the immediate post-horizontal-branch stage with energy supplied by both He and H burning shells.
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