Non coeval young multiple systems? On the pairing of protostars and T Tauri stars
| dc.creator | Duchene, Gaspard | |
| dc.creator | Ghez, Andrea | |
| dc.creator | McCabe, Caer | |
| dc.date | 2003-05-31 | |
| dc.date.accessioned | 2026-07-07T02:08:39Z | |
| dc.date.available | 2026-07-07T02:08:39Z | |
| dc.description | 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. | |
| dc.description | 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 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0306014 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0306014 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/6137 | |
| dc.subject | Astrophysics | |
| dc.title | Non coeval young multiple systems? On the pairing of protostars and T Tauri stars | |
| dc.type | text |