Speaker
Mr
Daniel Nhlapo
(North West University, Mafikeng Campus)
Description
beta Cephei stars are hot massive B stars that pulsate with periods of between 1.6 and 7.7 hours. They oscillate because of seismic waves that travel through these stars. Seismic waves have been used to infer interior conditions and properties of stars. In order for this technique to be used successively, the pulsation modes need to be identified. In this poster we present a mode-identification technique that compares theory with CCD photometric data obtained on the 30inch telescope at Sutherland SAAO observing station.
Primary author
Mr
Daniel Nhlapo
(North West University, Mafikeng Campus)
Co-authors
Dr
Andrzej Pigulski
(Wroclaw University)
Prof.
Rodney Medupe
(North West University, Mafikeng Campus)
