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dc.contributor.authorChrysostomou, A.
dc.contributor.authorLucas, P.W.
dc.date.accessioned2011-02-14T13:35:55Z
dc.date.available2011-02-14T13:35:55Z
dc.date.issued2005
dc.identifier.citationChrysostomou , A & Lucas , P W 2005 , ' The formation of stars ' Contemporary Physics , vol. 46 , no. 1 , pp. 29-40 . https://doi.org/10.1080/0010751042000275277
dc.identifier.issn0010-7514
dc.identifier.otherPURE: 181006
dc.identifier.otherPURE UUID: f5698e52-1fa9-45c4-b382-88a7406153a8
dc.identifier.otherdspace: 2299/5328
dc.identifier.otherScopus: 12344254725
dc.identifier.urihttp://hdl.handle.net/2299/5328
dc.descriptionOriginal article can be found at: http://www.informaworld.com Copyright Informa / Taylor and Francis Group [Full text of this article is not available in the UHRA]
dc.description.abstractWe review the process of star formation, detailing the theories underlying the stability of molecular clouds and their collapse to protostars, and discussing the empirical evidence and models which inform them. We give emphasis to the role that the magnetic field plays in influencing the stability of molecular clouds and hence the star formation rate. The end result of star formation is a mass function which appears constant within our Galaxy. A relative abundance of low mass stars is observed over high mass stars and most of the stars that do form are found to exist as members of a binary system. The origin of binarity is reviewed as is the discovery, formation and observations of some of the lowest mass stars known, the brown dwarfs.en
dc.language.isoeng
dc.relation.ispartofContemporary Physics
dc.subjectAstronomy
dc.titleThe formation of starsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionofrecordhttps://doi.org/10.1080/0010751042000275277
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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