The low-mass young stellar population in Orion OB1

Details The low-mass young stellar population in Orion OB1 The low-mass young stellar population in Orion OB1

2002-02-19

arxiv.org/abs/astro-ph/0202350v1

Astronomy and Astrophysics

Astrophysics

3 pages, 2 Figures, LaTeX (style and macro file included). To appear in Proceedings of the X Latin American Regional Meeting o

Scientific paper

We present recent results from our ongoing large scale variability survey of the Orion OB1 Association. In an area of ~ 25 square degrees we have unveiled new populations of low-mass young stars over a range of environments, and ages from 1-2 Myr in Ori OB 1b to roughly 10 Myr in Ori OB 1a. There is a lack of strong Ha emission and near-IR excesses in the young stars of Ori OB 1a, suggesting that accretion stops and disks dissipate for most solar type stars in a few Myr, probably caused by of the onset of planet formation. The absence of dust and gas in Ori OB 1a is consistent with the picture of star formation as a rapid process, in which molecular clouds dissipate in just a few Myr after the first stars are born.

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