Rotation in NGC 2264: a study based on CoRoT photometric observations

TL;DR

This study analyzes the rotational periods of stars in the NGC 2264 cluster using CoRoT photometric data, revealing differences in rotation between accreting and non-accreting young stars.

Contribution

It provides the first extensive analysis of stellar rotation in NGC 2264 using CoRoT data, highlighting differences between classical and weak-line T-Tauri stars.

Findings

Different rotational distributions for classical and weak-line T-Tauri stars

Evidence of rotational evolution in early stellar development

Insights into star formation processes in NGC 2264

Abstract

Rotation is one of the key stellar parameters which undergo substantial evolution during the stellar lifetime, in particular during the early stages. Stellar rotational periods can be determined on the basis of the periodic modulation of starlight produced by non-uniformities on the surface of the stars, due to manifestation of stellar activity. We present the results of an extensive search for rotational periods among NGC 2264 cluster members, based on photometric monitoring using the CoRoT satellite, with a particular attention to the distribution of classical and weak-line T-Tauri stars. NGC 2264 is one of the nearest and best studied star forming region in the solar neighbourhood, with an estimated age of 3 Myr, and is the object of a recent simultaneous multiband campaign including a new CoRoT observation with the aim to assess the physical origin of the observed variability. We find that the rotational distributions of classical and weak-line T-Tauri star are different, suggesting a difference in the rotational properties of accreting and non-accreting stars.