English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The low spin rates measured for solar-type stars at an age of a few Myr (~10%of the break-up velocity) indicate that some mechanism of angular momentumregulation must be at play in the early pre-main sequence. We characterize therotation properties for members of the region NGC 2264 (~3 Myr), andinvestigate the accretion-rotation connection at an age where about 50% of thestars have already lost their disks. We examined a sample of 500 clustermembers whose photometric variations were monitored in the optical for 38consecutive days with CoRoT. Light curves were analyzed for periodicity usingthe Lomb-Scargle periodogram, the autocorrelation function and thestring-length method. The period distribution obtained for the cluster consistsof a smooth distribution centered around P=5.2 d with two peaks at P=1-2 d and3-4 d. A separate analysis of CTTS and WTTS indicates that the P=1-2 d peak isassociated with the latter, while both groups contribute to the P=3-4 d peak.The comparison between CTTS and WTTS supports the idea of a rotation-accretionconnection: their respective rotational properties are statistically different,and CTTS rotate on average more slowly than WTTS. We also observe a cleardearth of fast rotators with strong accretion signatures (large UV fluxexcess). This is consistent with earlier findings that fast rotators in youngstar clusters are typically devoid of dusty disks. Our sample shows someevidence of a mass dependence in the rotation properties of NGC 2264 members,lower-mass stars spinning on average faster. This study confirms that disksinfluence the rotational evolution of young stars. The idea of disk-locking maybe consistent with the picture of rotation and rotation-accretion connectionthat we observe for the NGC 2264 cluster. However, the origin of the severalsubstructures that we observe in the period distribution deserves furtherinvestigation.

CSI 2264: Investigating rotation and its connection with disk accretion in the young open cluster NGC 2264