2006BaltA..15..255K

We have re-observed four rapidly-pulsating sdB stars during 2003 and 2004 and compared the results to earlier observations. The class prototype, EC 14026-2647 (=V361 Hya), had a weak frequency which has apparently disappeared, whilst a new frequency has appeared. In EC 20338-1925, the strongest frequency (6806 µHz; ampl. 0.026 mag) has reduced to about 0.004 mag, and weaker frequencies have come and gone. Between 1997 and 2004, the complex pulsator, PG 1605+072 (=V338 Ser), has had its strongest frequency (f₁) halve in amplitude, f₃ and f₄ double in amplitude, whilst f₂ has remained essentially constant. Finally, HS 2149+0847 (=V384 Peg) shows no significant change between 2003 and 2004, but we have increased the number of known frequencies from two to six.