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Disk Braking in young Stars: Probing Rotation in Chamaeleon i and Taurus-Auriga
Stockholm University, Faculty of Science, Department of Astronomy.
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2009 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 695, p. 1648-1656Article in journal (Refereed) Published
Abstract [en]

We present a comprehensive study of rotation, disk, and accretion signatures for 144 T Tauri stars in the young (~2 Myr old) Chamaeleon I and Taurus-Auriga star-forming regions based on multi-epoch high-resolution optical spectra from the Magellan Clay 6.5 m telescope supplemented by mid-infrared photometry from the Spitzer Space Telescope. In contrast to previous studies in the Orion Nebula Cluster and NGC 2264, we do not see a clear signature of disk braking in Tau-Aur and Cha I. We find that both accretors and non-accretors have similar distributions of vsin i. This result could be due to different initial conditions, insufficient time for disk braking, or a significant age spread within the regions. The rotational velocities in both regions show a clear mass dependence, with F-K stars rotating on average about twice as fast as M stars, consistent with results reported for other clusters of similar age. Similarly, we find the upper envelope of the observed values of specific angular momentum j varies as M 0.5 for our sample which spans a mass range of ~0.16-3 M sun. This power law complements previous studies in Orion which estimated j vprop M 0.25 for lsim2 Myr stars in the same mass regime, and a sharp decline in j with decreasing mass for older stars (~10 Myr) with M < 2 M sun. Furthermore, the overall specific angular momentum of this ~10 Myr population is five times lower than that of non-accretors in our sample, and implies a stellar braking mechanism other than disk braking could be at work. For a subsample of 67 objects with mid-infrared photometry, we examine the connection between accretion signatures and dusty disks: in the vast majority of cases (63/67), the two properties correlate well, which suggests that the timescale of gas accretion is similar to the lifetime of inner disks.

Place, publisher, year, edition, pages
2009. Vol. 695, p. 1648-1656
Keywords [en]
accretion, accretion disks, circumstellar matter, stars: evolution, stars: formation, stars: pre-main sequence, stars: rotation, stars: statistics
Research subject
Astronomy
Identifiers
URN: urn:nbn:se:su:diva-35865DOI: 10.1088/0004-637X/695/2/1648/ISI: 000265018300078ISBN: 0004-637X (print)OAI: oai:DiVA.org:su-35865DiVA, id: diva2:288208
Available from: 2010-01-20 Created: 2010-01-20 Last updated: 2017-12-12Bibliographically approved

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