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

Somers, Garrett; Stauffer, J. R.; Rebull, L. M.; Cody, Ann Marie; Pinsonneault, Marc H.

doi:10.3847/1538-4357/aa93ed

Cited by 30 publications

(29 citation statements)

References 92 publications

(192 reference statements)

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“…A full theoretical treatment of gyrochronology requires evolutionary stellar models that include a variety of physical effects (see Gallet & Bouvier (2013) for an overview). Models of angular momentum evolution have usually been calibrated using rotation periods in star clusters, which have known ages and are easily characterized (Krishnamurthi et al 1997;Gallet & Bouvier 2013;Somers et al 2017). The calibrating clusters are typically young (< 1 Gyr), with the behavior at old ages anchored by the Sun.…”

Section: Introductionmentioning

confidence: 99%

Rapid Rotation in the Kepler Field: Not a Single Star Phenomenon

Simonian

Pinsonneault

Terndrup

2019

ApJ

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Tens of thousands of rotation periods have been measured in the Kepler fields, including a substantial fraction of rapid rotators. We use Gaia parallaxes to distinguish photometric binaries (PBs) from single stars on the unevolved lower main sequence, and compare their distribution of rotation properties to those of single stars both with and without APOGEE spectroscopic characterization. We find that 59% of stars with 1.5 day < P < 7 day lie 0.3 mag above the main sequence, compared with 28% of the full rotation sample. The fraction of stars in the same period range is 1.7 ± 0.1% of the total sample analyzed for rotation periods. Both the photometric binary fraction and the fraction of rapid rotators are consistent with a population of non-eclipsing short period binaries inferred from Kepler eclipsing binary data after correcting for inclination. This suggests that the rapid rotators are dominated by tidally-synchronized binaries rather than single-stars obeying traditional angular momentum evolution. We caution against interpreting rapid rotation in the Kepler field as a signature of youth. Following up this new sample of 217 candidate tidally-synchronized binaries will help further understand tidal processes in stars.

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Section: Introductionmentioning

confidence: 99%

Rapid Rotation in the Kepler Field: Not a Single Star Phenomenon

Simonian

Pinsonneault

Terndrup

2019

ApJ

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“…In Somers et al (2017), we have provided a preliminary comparison; in a future paper, we plan to critically assess the ability of the entire K2 clusters period data to constrain angular momentum losses from the winds of low-mass stars.…”

Section: Evolution Of P Versus (V − K S ) 0 Across Clustersmentioning

confidence: 99%

“…These data sets improve upon what was available up until now by not only providing larger samples, but more importantly providing rotation periods from F stars down to nearly the hydrogen-burning mass limit, and doing so for nearly complete sets of stars (within the K2 FOV) for each of the clusters. In Somers et al (2017), we have recently used the USco and Pleiades rotational data for the M dwarfs in those two clusters to highlight the strong dependence of rotation on mass for M<0.5 M ☉ at early ages and how those data constrain angular momentum loss from winds prior to the ZAMS. Here we provide a qualitative summary of the rotational velocity evolution of stars over the full mass range of our data for the age sequence from USco to the Pleiades to Praesepe.…”

Section: Evolution Of P Versus (V − K S ) 0 Across Clustersmentioning

confidence: 99%

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Rotation of Low-mass Stars in Upper Scorpius and ρ Ophiuchus with K2

Rebull

Stauffer

Cody

et al. 2018

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146

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We present an analysis of K2 light curves (LCs) for candidate members of the young Upper Sco (USco) association (∼8 Myr) and the neighboring ρ Oph embedded cluster (∼1 Myr). We establish ∼1300 stars as probable members, ∼80% of which are periodic. The phased LCs have a variety of shapes which can be attributed to physical causes ranging from stellar pulsation and stellar rotation to disk-related phenomena. We identify and discuss a number of observed behaviors. The periods are ∼0.2-30 days with a peak near 2 days and the rapid period end nearing breakup velocity. M stars in the young USco region rotate systematically faster than GK stars, a pattern also present in K2 data for the older Pleiades and Praesepe systems. At higher masses (types FGK), the well-defined period-color relationship for slowly rotating stars seen in the Pleiades and Praesepe systems is not yet present in USco. Circumstellar disks are present predominantly among the more slowly rotating M stars in USco, with few disks in the subday rotators. However, M dwarfs with disks rotate faster on average than FGK systems with disks. For four of these disked M dwarfs, we provide direct evidence for disk locking based on the K2 LC morphologies. Our preliminary analysis shows a relatively mass-independent spin-up by a factor of ∼3.5 between USco and the Pleiades, then mass-dependent spin-down between Pleiades and Praesepe.

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“…From v sin i and stellar radius, we estimated a rotation period of 0.2 days for 2MASS J1457-3543. Recent studies on M dwarfs belonging to Pleiades and Praesepe clusters (Somers et al 2017) and low-mass stars residing in USC and ρ Ophiuchus (Rebull et al 2018) suggest that rotation periods…”

Section: Mass J1457-3543mentioning

confidence: 99%

Characterization of very wide companion candidates to young stars with planets and disks

Majidi

Desidera

Alcalá

et al. 2020

A&A

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Discovering wide companions of stellar systems allows us to constrain the dynamical environment and age of the latter. We studied four probable wide companions of four different stellar systems. The candidates were selected mainly based on their similar kinematic properties to the central star using Gaia DR2. The central stars are V4046 Sgr, HIP 74865, HIP 65426, and HIP 73145, and their probable wide companions are 2MASS J18152222-3249329, 2MASS J15174874-3028484, 2MASS J13242119-5129503, and 2MASS J14571503-3543505 respectively. V4046 Sgr is a member of β-Pictoris Moving Group while the rest of the stellar systems are acknowledged as members of the Scorpius-Centaurus association. The selected stellar systems are particularly interesting because all of them are already known to possess a low-mass companion and/or a spatially resolved disk. Identifying wider companions of these stars can improve their eligibility as benchmarks for understanding the formation channels of various triple systems, and can help us to determine the orbits of their possibly undiscovered inner, wider companions in case of higher multiplicity. By analyzing the X-shooter spectra of the wide companion candidates of these stars, we obtained their stellar parameters and determined their ages. We find that 2MASS J15174874-3028484 (0.11 M⊙, 7.4 ± 0.5 Myr), an already recognized pre-main sequence (PMS) member of Scorpius-Centaurus association, is a highly probable wide companion of HIP 74865. 2MASS J13242119-5129503 (0.04 M⊙, 16 ± 2.2 Myr) is ruled out as a plausible wide companion of HIP 65426, but confirmed to be a new sub-stellar member of the Scorpius-Centaurus association. 2MASS J14571503-3543505 (0.02 M⊙, 17.75 ± 4.15 Myr) is a probable sub-stellar member of the same association, but we cannot confirm whether or not it is gravitationally bound to HIP 73145. 2MASS J18152222-3249329 (0.3 M⊙, older than 150 Myr) is determined to be a mildly active main sequence star, much older than members of β-Pictoris Moving Group, and unbound to V4046 Sgr despite their similar kinematic features. PMS wide companions such as 2MASS J15174874-3028484 might have formed through cascade fragmentation of their natal molecular core, hinting at high multiplicity in shorter separations which can be confirmed with future observations.

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

Cited by 30 publications

References 92 publications

Rapid Rotation in the Kepler Field: Not a Single Star Phenomenon

Rapid Rotation in the Kepler Field: Not a Single Star Phenomenon

Rotation of Low-mass Stars in Upper Scorpius and ρ Ophiuchus with K2

Characterization of very wide companion candidates to young stars with planets and disks

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