000002640 001__ 2640
000002640 005__ 20160701171708.0
000002640 037__ $$aASTROimport-797
000002640 100__ $$aDe Cat, P.
000002640 245__ $$aA new era of asteroseismology: hot stars
000002640 260__ $$c2006
000002640 520__ $$aTo fully understand the evolution of stars, detailed information on the processes acting in the stellar interior is needed. Since the stellar interior is not directly accessible, asteroseismologists thankfully use the indirect information contained in stellar oscillations to probe the stellar interiors. There are two families of modes carrying information of different parts of the stellar interior: pressure modes (p-modes; mainly propagating in the envelope) and gravity modes (g modes; mainly propagating in the core). For a unique asteroseismic modelling, a large number of well-identified modes are needed. Different classes of oscillating stars are found across the Hertzsprung-Russell diagram. The β Cephei and δ Scuti stars (pulsating in low order p and g modes with periods of the order of hours) and the slowly pulsating B and γ Doradus stars (pulsating in high order g modes with periods of the order of days) are situated along the upper part of the main sequence. In this talk, we will outline their seismic potential and highlight their most important seismic results based on well-chosen examples. It becomes clear that long-term (and preferably multi-site) campaigns are needed to overcome the obstacles of ground-based observations. On the other hand, the high-quality data delivered by the MOST satellite has already led to important results for main-sequence pulsating stars. The future of asteroseismology is therefore bright with upcoming space missions like CoRoT. 
000002640 773__ $$c19$$pIAU Joint Discussion$$v17$$y2006
000002640 85642 $$ahttp://esoads.eso.org/abs/2006IAUJD..17E..19D
000002640 905__ $$apublished in
000002640 980__ $$aNONREF