Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001phdt........41d&link_type=abstract
PhD thesis, Katholieke Universiteit Leuven, 2001, 428 pages
Other
23
Stars: Early-Type, Stars: Variables: General, Stars: Oscillations, Stars: Binaries: Spectroscopic, Line: Profiles
Scientific paper
Slowly pulsating B stars are multi-periodic pulsators with oscillation periods of the order of days. Their pulsation modes penetrate deep into the stellar interior, making these objects very promising from an asteroseismic point of view. In this work, we studied a selection of 17 bright southern slowly pulsating B stars covering the whole theoretical instability strip of such pulsators. At least 9 of our target stars turn out to be spectroscopic binaries. There is a large variety in the observed orbits. With this work, we provide for the first time a global study for a class of main-sequence g-mode pulsators. The observed intrinsic variations were interpreted in terms of non-radial pulsations. At least 2 of our studied variables turn out to be spotted chemically peculiar stars instead of pulsating B stars. For another two targets, no intrinsic frequency was found. For 9 of the remaining 13 targets, the expected multi-periodic character is confirmed. For the cool slowly pulsating B stars, we observe a higher main frequency than for the hot slowly pulsating B stars. The observed pulsational behaviour suggests that the pulsations of slowly pulsating B stars are nearly adiabatic. No evidence for an interaction between rotation and pulsation is found, nor for amplitude damping by rotation. We briefly describe the numerous future prospects that result from our study.
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