Testing the Evolution of Young Stars with FU Orionis Objects

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FU Orionis objects (FUors) play a central role in the study of the evolution of young stars. They undergo accretion outbursts that can bring up to about 0.01 solar masses per outburst, therefore providing a significant amount of mass in the pre-main sequence life of a star. Spitzer IRS observations of FUors have shown either silicate features in absorption and ice bands or silicates in emission with no ice bands. This led some authors to propose an evolutionary paradigm in which the former FUors are younger than the latter FUors. The FUor phase might be a common but rarely observed phase (about 20 FUors known) of most young low-mass stars and might be the link between Class I and Class II sources. So far, Spitzer has obtained IRS spectra of about half of the FUor catalog, focusing on its most famous class members. With this short Spitzer proposal, we aim to observe FUors that have not yet been observed with the IRS or had no high-resolution module spectra. We will study the composition and evolution of dust grains and of ices in FUors surrounded by envelopes, and we aim at detecting faint molecular hydrogen and atomic lines with the high-resolution module spectra. The IRS spectra will probe the stellar environment, and thus test the above evolutionary paradigm and the different theories for the origin of FUor outburst. The Spitzer IRS observations of our sample of FUors will therefore provide additional insights about a significant phase in the life of young stars with the aim to better describe the evolutionary sequence from Class I star to Class II sources.

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