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Multiplicity among M dwarfs

Fischer, Debra A., Marcy, Geoffrey W.·1992·The Astrophysical Journal

Abstract

Surveys of M dwarfs within 20 pc are examined to determine the incidence of stellar companions. Observational data are drawn from high-quality surveys, including IR-array imaging, precise velocities, IR speckle interferometry, and visual imaging, and their respective incompleteness is determined. The number of companions per AU of semimajor axis is computed and found to decline monotonically toward larger semimajor axes. The period distribution exhibits a unimodal broad maximum with a peak in the range 9-220 yr, corresponding to separations of 3-30 AU, similar to that for G dwarf binaries. Fifty-eight percent of nearby M dwarf primaries are found to be single, and 42 +/- 9 percent have companions. The M-dwarf binary frequency is lower than that for G dwarfs (about 57 percent), owing partly to the smaller range of companion masses included, i.e., companions less massive than the M- or G-type primary.

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Metadata

Authors
Fischer, D. A., & Marcy, G. W.
Venue
The Astrophysical Journal
Published
1992-09
Volume
396
Pages
178
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2070606946
Cited by
671
References
0
FWCI
3.93
Type
journal article
Language
en
Open access
closed

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CoChat. (2026). Citation check: Multiplicity among M dwarfs. https://app.cochat.ai/papers/10.1086/171708
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Fischer, D. A., & Marcy, G. W. (1992). Multiplicity among M dwarfs. The Astrophysical Journal. https://doi.org/10.1086/171708

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