Poster abstract details

Time Dependent Convection models predict a range in frequency that
is stable to pulsations, between the simultaneously excited high-order
g modes ($\gamma$ Doradus) and low-order p and g modes ($\delta$ Scuti).
On the other hand theoretical studies (Samadi et al. 2002) find that in those
models, stochastically excited modes are likely to be observed.
The primary target in the seismo-field of CoRoT, HD49434, shows
excited intermediate order modes. Are those modes stochastically
excited confirming some theoretical studies and contradicting others?
Using the statistical method described in Pereira et al. (2007), which
searches for signatures of stochastic excitation in stellar pulsations,
we investigate the nature of those modes with possible implications on
the identification of their excitation mechanism.