The Rotation of Young Low-Mass Stars and Brown Dwarfs
| dc.creator | Herbst, W. | |
| dc.creator | Eisloeffel, J. | |
| dc.creator | Mundt, R. | |
| dc.creator | Scholz, A. | |
| dc.date | 2006-03-24 | |
| dc.date.accessioned | 2026-07-07T07:01:16Z | |
| dc.date.available | 2026-07-07T07:01:16Z | |
| dc.description | We review the current state of our knowledge concerning the rotation and angular momentum evolution of young stellar objects and brown dwarfs from a primarily observational view point. Periods are typically accurate to 1% and available for about 1700 stars and 30 brown dwarfs in young clusters. Discussion of angular momentum evolution also requires knowledge of stellar radii, which are poorly known for pre-main sequence stars. It is clear that rotation rates at a given age depend strongly on mass; higher mass stars (0.4-1.2 M$_\odot$) have longer periods than lower mass stars and brown dwarfs. On the other hand, specific angular momentum is approximately independent of mass for low mass pre-main sequence stars and young brown dwarfs. A spread of about a factor of 30 is seen at any given mass and age. The evolution of rotation of solar-like stars during the first 100 Myr is discussed. A broad, bimodal distribution exists at the earliest observable phases ($\sim$1 Myr) for stars more massive than 0.4 M$_\odot$. The rapid rotators (50-60% of the sample) evolve to the ZAMS with little or no angular momentum loss. The slow rotators continue to lose substantial amounts of angular momentum for up to 5 Myr, creating the even broader bimodal distribution characteristic of 30-120 Myr old clusters. Accretion disk signatures are more prevalent among slowly rotating PMS stars, indicating a connection between accretion and rotation. Disks appear to influence rotation for, at most, $\sim$5 Myr, and considerably less than that for the majority of stars. If the dense clusters studied so far are an accurate guide, then the typical solar-like star may have only $\sim$1 Myr for this task. It appears that both disk interactions and stellar winds are less efficient at braking these objects. | |
| dc.description | Review chapter for Protostars and Planets V. 15 page and 8 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0603673 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0603673 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/108223 | |
| dc.subject | Astrophysics | |
| dc.title | The Rotation of Young Low-Mass Stars and Brown Dwarfs | |
| dc.type | text |