The aim of this project is determining the angular momentum history of Pre Main Sequence (PMS) stars in young clusters. Assuming a conservation of angular momentum, as these stars contract during formation, they should all be rotating rapidly after a very short amount of time (~2 Myrs). However, rotation periods of young cluster members show that most of these stars rotate much more slowly than expected. For many years, the precise mechanism which prevents these stars from spinning up has been debated, with no conclusive observational evidence to support one mechanism over another.
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