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Cited by 279

The DOI matches its Crossref record; 109 of the 109 references it cites were found in a registry or an index.

THE ROTATION AND GALACTIC KINEMATICS OF MID M DWARFS IN THE SOLAR NEIGHBORHOOD

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Newton, Elisabeth R., Irwin, Jonathan, Charbonneau, David, Berta-Thompson, Zachory K., Dittmann, Jason A., West, Andrew A.·2016·The Astrophysical Journal
DOI 10.3847/0004-637x/821/2/93
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Abstract

Rotation is a directly observable stellar property, and it drives magnetic field generation and activity through a magnetic dynamo. Main-sequence stars with masses below approximately 0.35 M ⊙ (mid-to-late M dwarfs) are fully convective, and are expected to have a different type of dynamo mechanism than solar-type stars. Measurements of their rotation rates provide insight into these mechanisms, but few rotation periods are available for these stars at field ages. Using photometry from the MEarth Project, we measure rotation periods for 387 nearby, mid-to-late M dwarfs in the northern hemisphere, finding periods from 0.1 to 140 days. The typical rotator has stable, sinusoidal photometric modulations at a semi-amplitude of 0.5%–1%. We find no period–amplitude relation for stars below 0.25 M ⊙ and an anticorrelation between period and amplitude for higher-mass M dwarfs. We highlight the existence of older, slowly rotating stars without H α emission that nevertheless have strong photometric variability. We use parallaxes, proper motions, radial velocities, photometry, and near-infrared metallicity estimates to further characterize the population of rotators. The Galactic kinematics of our sample is consistent with the local population of G and K dwarfs, and rotators have metallicities characteristic of the solar neighborhood. We use the W space velocities and established age–velocity relations to estimate that stars with P < 10 days have ages of on average <2 Gyr, and that those with P > 70 days have ages of about 5 Gyr. The period distribution is dependent on mass: as the mass decreases, the slowest rotators at a given mass have longer periods, and the fastest rotators have shorter periods. We find a lack of stars with intermediate rotation periods, and the gap between the fast and slow rotators is larger for lower masses. Our data are consistent with a scenario in which these stars maintain rapid rotation for several gigayears, then spin down quickly, reaching periods of around 100 days by a typical age of 5 Gyr.

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Metadata

Authors
Newton, E. R., Irwin, J., Charbonneau, D., Berta-Thompson, Z. K., Dittmann, J. A., & West, A. A.
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2016-04-14
Volume
821
Issue
2
Pages
93
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.3847/0004-637x/821/2/93
OpenAlex
W1927747930
Cited by
279
References
109
FWCI
14.16
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: THE ROTATION AND GALACTIC KINEMATICS OF MID M DWARFS IN THE SOLAR NEIGHBORHOOD. https://app.cochat.ai/papers/10.3847/0004-637x/821/2/93
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Newton, E. R., Irwin, J., Charbonneau, D., Berta-Thompson, Z. K., Dittmann, J. A., & West, A. A. (2016). THE ROTATION AND GALACTIC KINEMATICS OF MID M DWARFS IN THE SOLAR NEIGHBORHOOD. The Astrophysical Journal. https://doi.org/10.3847/0004-637x/821/2/93

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

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