Non coeval young multiple systems? On the pairing of protostars and T Tauri stars
arXiv:astro-ph/0306014
Abstract
We summarize here the observed properties of ``infrared companions'' to T Tauri stars and argue that their observational properties are identical to those of Class I sources. They may therefore be embedded protostars in a much earlier evolutionary phase than T Tauri stars, in which case these multiple systems are significantly non-coeval as opposed to the majority of young binary systems. They would have formed through a different mechanism than core fragmentation. The only distinction between IRCs and Class I sources is that they lie within a few tens of AU of a T Tauri star, and so they cannot be at the center of a vast optically thick envelope as is believed to be the case for protostars. We discuss whether systems with an IRC are really candidates for non-coeval multiple systems.
8 pages, 1 figure, to appear in the conference proceedings of "Open Issues in Local Star Formation and Early Stellar Evolution", held in Ouro Preto (Brazil), April 5-10, 2003
References in corpus (7)
- Observational Constraints on the Formation and Evolution of Binary Stars
- Accretion Disks Around Young Objects. II. Tests of Well-Mixed Models with Ism Dust
- The Spectral Energy Distribution of HH30 IRS: Constraining The Circumstellar Dust Size Distribution
- Resolved Near-Infrared Spectroscopy of the Mysterious Pre-Main Sequence Binary Systems T Tau S
- No Fossil Disk in the T Tauri Multiple System V773 Tau
- A Luminous Infrared Companion in the Young Triple System WL 20
- Evidence for Extinction and Accretion Variability in T Tau S