Stellar Multiplicity
Gaspard Duch\^ene (1,2), Adam Kraus (3) ((1) UC Berkeley, (2), Institut de Plan\'etologie et d'Astrophysique de Grenoble, (3), Harvard-Smithsonian CfA)
TL;DR
This review summarizes recent empirical findings on stellar multiplicity, highlighting how the frequency and characteristics of multiple star systems depend on mass and evolutionary stage, aiding star formation models.
Contribution
It compiles and analyzes robust observational data on stellar multiplicity across different star types and stages, providing a comprehensive overview for future research.
Findings
Multiplicity varies with primary mass and evolutionary stage.
Recent instrumentation has enabled more complete and unbiased surveys.
Clear trends identified to inform star formation theories.
Abstract
Stellar multiplicity is an ubiquitous outcome of the star formation process. Characterizing the frequency and main characteristics of multiple systems and their dependencies on primary mass and environment is therefore a powerful tool to probe this process. While early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the last two decades now enable robust analyses. In this review, we summarize our current empirical knowledge of stellar multiplicity for Main Sequence stars and brown dwarfs, as well as among populations of Pre-Main Sequence stars and embedded protostars. Clear trends as a function of both primary mass and stellar evolutionary stage are identified that will serve as a comparison basis for numerical and analytical models of star formation.
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