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The Origin of the Stellar Mass Distribution and Multiplicity

dc.contributor.authorLee Y.-N.
dc.contributor.authorOffner S.S.R.
dc.contributor.authorHennebelle P.
dc.contributor.authorAndré P.
dc.contributor.authorZinnecker H.
dc.contributor.authorBallesteros-Paredes J.
dc.contributor.authorInutsuka S.-I.
dc.contributor.authorKruijssen J.M.D.
dc.date.accessioned2020-09-02T22:21:19Z
dc.date.available2020-09-02T22:21:19Z
dc.date.issued2020
dc.identifier10.1007/s11214-020-00699-2
dc.identifier.citation216, 4, -
dc.identifier.issn00386308
dc.identifier.urihttps://hdl.handle.net/20.500.12728/5067
dc.descriptionIn this chapter, we review some historical understanding and recent advances on the Initial Mass Function (IMF) and the Core Mass Function (CMF), both in terms of observations and theories. We focus mostly on star formation in clustered environment since this is suggested by observations to be the dominant mode of star formation. The statistical properties and the fragmentation behaviour of turbulent gas is discussed, and we also discuss the formation of binaries and small multiple systems. © 2020, Springer Nature B.V.
dc.language.isoen
dc.publisherSpringer
dc.subjectCore mass function
dc.subjectInitial mass function
dc.subjectMultiplicity
dc.subjectStellar cluster
dc.subjectFunctions
dc.subjectDominant mode
dc.subjectInitial mass
dc.subjectMass functions
dc.subjectSmall multiples
dc.subjectStar formations
dc.subjectStatistical properties
dc.subjectStellar mass
dc.subjectStars
dc.titleThe Origin of the Stellar Mass Distribution and Multiplicity
dc.typeReview


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