Poster abstract

Some regions of star formation (Perseus, Serpens, Ophiucus, Lupus...) are now measured at different wavelengths. (Enoch et al. 09) and (Evans et al. 09) calculated the total luminosity and the mean frequency of the spectrum emitted by a lot of protostars. Both these quantities give respectively the bolometric luminosity and the bolometric temperature and are plotted in the bolometric diagram (Myers & Ladd 93). The measures show a large spread in this diagram. This spread is often explain by the episodic accretion: the pre-stellar core is not accreting matter at a continuous accreting rate but at an irregular accretion rate, with a succession of high accretion rate (bursts) and low accretion rate (quiescent phases). The episodic accretion was also recently proposed by Baraffe et al. 09 to explain the spread in HR diagrams after 1Myr.
The existing models (Young et al. 05 Myers et al. 98) used a continuous accreting rate to predict the evolution of the protostar in the diagram. Like the previous works, we simulate the evolution of a protostar and the evolution of the bolometric luminosity and temperature with a star-disk-envelope system. Unlike the existing models, we simulate the evolution of the accreting protostar (radius and luminosity) with the Lyon stellar evolution code. The effect of the accretion on the protostars is not negligeable on the bolometric luminosity and the bolometric temperature.