2006BaltA..15..207M

Light curve solutions show HW Vir and PG1336-018 to be remarkably similar eclipsing binaries. The subdwarf-B (sdB) primary of PG1336-018 is a pulsator but pulsation is not detected in the sdB primary of HW Vir. Ultraviolet spectra were used to obtain carbon and silicon abundances in the sdB primary of HW Vir; in due course these should be compared with those in the sdB primary of PG1336-018 to see if pulsation in the latter could be explained by the κ-mechanism, arising from higher metal abundances and microscopic diffusion.