The Monitor project: rotation of low-mass stars in NGC 2362 – testing the disc regulation paradigm at 5 Myr

Irwin, Jonathan; Hodgkin, S. T.; Aigrain, S.; Bouvier, J.; Hebb, Leslie; Irwin, M. J.; Moraux, E.

doi:10.1111/j.1365-2966.2007.12725.x

Cited by 94 publications

(154 citation statements)

References 35 publications

(73 reference statements)

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“…Irwin et al (2008) did not find such a correlation between rotational period and amplitude of the modulation in the 5 Myr old cluster NGC 2362. It is worth to note that their sample only extends down to about 0.1 M , with a high fraction of objects even more masive than 0.4 M .…”

Section: Rotational Period and Ptp Amplitude Correlation In The Onc Amentioning

confidence: 70%

“…Several authors have investigated the rotational properties of solar mass and low mass stars in clusters of various ages (e.g. Stauffer & Hartmann 1987;Prosser et al 1993Prosser et al , 1995Terndrup et al 2000;Scholz & Eislöffel 2004b;Irwin et al 2008). In young clusters and star forming regions, an enormous spread in rotational periods has been observed at all stellar masses (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Rotational studies in the Orion Nebula Cluster: from solar mass stars to brown dwarfs

Rodríguez-Ledesma

Mundt²,

Eislöffel

2009

A&A

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Aims. Rotational studies at a variety of ages and masses are important for constraining the angular momentum evolution of young stellar objects (YSO). Of particular interest are the very low mass (VLM) stars and brown dwarfs (BDs), because of the significant lack of known rotational periods in that mass range. We aim to extend previous studies well down into the substellar regime, providing for the first time information on rotational periods for a large sample of young VLM stars and BDs. Methods. This extensive rotational period study of YSOs in the 1 Myr old Orion Nebula Cluster (ONC) is based on a deep photometric monitoring campaign using the Wide Field Imager (WFI) camera on the ESO/MPG 2.2 m telescope on La Silla, Chile. Time series data was obtained with about 95 data points spread over 19 nights. Accurate I-band photometry of 2908 stars was obtained within a magnitude range of 13 to 21 mag, i.e. extending three magnitudes deeper than previous studies in the ONC. Two different power spectral analysis techniques were used to search for periodic variability. In addition, the χ 2 variability test was used for the detection of irregular variables. Results. We found 487 periodic variables with estimated masses between 0.5 M and 0.015 M , 124 of which are BD candidates. This is by far the most extensive and complete rotational period data set for young VLM stars and BDs. In addition to the periodic variables, 808 objects show non-periodic brightness variations. We study the dependence of the period distribution on mass and variability level and compare this with known objects in the ONC with masses up to 1.5 M and with the ∼2 Myr old cluster NGC 2264. We find that substellar objects rotate on average faster than the VLM stars. In addition, our rotational data suggest a dependence of the rotational periods on position within the field, which can be explained by a possible age spread in the ONC with a somewhat younger central region. The results of a comparison between the period distributions of the ONC and NGC 2264 favours this hypothesis. In addition, periodic variables with larger peak-to-peak amplitudes rotate on average slower than those with small peak-to-peak amplitude variations, which can possibly be explained by different magnetic field topologies.

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Section: Rotational Period and Ptp Amplitude Correlation In The Onc Amentioning

confidence: 70%

Section: Introductionmentioning

confidence: 99%

Rotational studies in the Orion Nebula Cluster: from solar mass stars to brown dwarfs

Rodríguez-Ledesma

Mundt²,

Eislöffel

2009

A&A

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“…This trend has been hinted at previously by Dahm et al (2012) using v sin is, and by Scholz et al (2015) for brown dwarfs, but have been conclusively demonstrated in this paper. It is also evident in other young clusters such as the Orion Nebula Cluster (Herbst et al 2001), NGC2264 (Lamm et al 2005), NGC2362 (Irwin et al 2008a), and σOri (Cody & Hillenbrand 2010), among others. Despite its ubiquity, its origin and evolution remain unclear and appear contradictory at times.…”

Section: Discussionmentioning

confidence: 87%

M Dwarf Rotation from the K2 Young Clusters to the Field. I. A Mass–Rotation Correlation at 10 Myr

Somers

Stauffer

Rebull

et al. 2017

ApJ

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Recent observations of the low-mass (0.1-0.6 M  ) rotation distributions of the Pleiades and Praesepe clusters have revealed a ubiquitous correlation between mass and rotation, such that late Mdwarfs rotate an order-of-magnitude faster than early Mdwarfs. In this paper, we demonstrate that this mass-rotation correlation is present in the 10Myr Upper Scorpius association, as revealed by new K2 rotation measurements. Using rotational evolution models, we show that the low-mass rotation distribution of the 125Myr Pleiades cluster can only be produced if it hosted an equally strong mass-rotation correlation at 10Myr. This suggests that physical processes important in the early pre-main sequence (PMS; star formation, accretion, disk-locking) are primarily responsible for the Mdwarf rotation morphology, and not quirks of later angular momentum (AM) evolution. Such early mass trends must be taken into account when constructing initial conditions for future studies of stellar rotation. Finally, we show that the average Mstar loses ∼25%-40% of its AM between 10 and 125Myr, a figure accurately and generically predicted by modern solar-calibrated wind models. Their success rules out a lossless PMS and validates the extrapolation of magnetic wind laws designed for solar-type stars to the low-mass regime at early times.

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“…Irwin et al (2008) suggest that this varying slope for masses between 0.1-0.5M was a result of cluster evolution with age.…”

Section: Cygob2 Inside the Picture Of Pms Rotational Evolutionmentioning

confidence: 85%

Near-infrared time-series photometry in the field of Cygnus OB2 association

Roquette

Bouvier

Alencar

et al. 2017

A&A

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Context. In the last decades, the early pre main sequence stellar rotational evolution picture has been constrained by studies targetting different regions at a variety of ages with respect to young star formation. Observational studies suggest a dependence of rotation with mass, and for some mass ranges a connection between rotation and the presence of a circumstellar disk. Not still fully explored, though, is the role of environmental conditions on the rotational regulation.Aims. We investigate the rotational properties of candidate members of the young massive association Cygnus OB2. By evaluating their rotational properties, we address questions regarding the effect of environment properties on PMS rotational evolution.Methods. We studied JHK-band variability in 5083 candidate members (24% of them are diskbearing stars). The selection of variable stars was done using Stetson variability index, and period search was performed using Lomb-Scargle periodogram for periods between 0.83-45 days. Period detections were verified by using False Alarme Probability levels, the Saunders statistics, string/rope length method, and visual verification of folded light curves.Results. We identified 1224 periodic variable stars (24% of the candidate member sample, 8% of the disk-bearing sample, and 28% of the non-disked sample). Monte Carlo simulations were performed in order to evaluate completeness and contamination of the periodic sample, out of which 894 measured periods were considered reliable. Our study was considered reasonably complete for periods between 2 and 30 days. Conclusions. The general scenario for the rotational evolution of young stars seen in other regions is confirmed by Cygnus OB2 period distributions, with disked stars rotating on average slower than non-disked stars. A mass-rotation dependence was also verified, but as in NGC 6530, very low mass stars (M ≤ 0.4M ) are rotating on average slower than higher mass stars (0.4 M < M ≤ 1.4M ). We observed an excess of slow rotators among the lower mass population. The disk and mass-rotation connection was also analysed by taking into account the incident UV radiation arising from O stars in the association. Results compatible with the disk-locking scenario were verified for stars with low UV incidence, but no statistical significant relation between rotation and disk presence was verified for stars with high UV incidence suggesting that massive stars can have an important role on regulating the rotation of nearby low mass stars.Key words. infrared: stars -stars: variables: T Tauri -stars: low-mass -stars: formation -stars: pre main sequence -stars: rotation Use \titlerunning to supply a shorter title and/or \authorrunning to supply a shorter list of authors.

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The Monitor project: rotation of low-mass stars in NGC 2362 – testing the disc regulation paradigm at 5 Myr

Cited by 94 publications

References 35 publications

Rotational studies in the Orion Nebula Cluster: from solar mass stars to brown dwarfs

Rotational studies in the Orion Nebula Cluster: from solar mass stars to brown dwarfs

M Dwarf Rotation from the K2 Young Clusters to the Field. I. A Mass–Rotation Correlation at 10 Myr

Near-infrared time-series photometry in the field of Cygnus OB2 association

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