Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/94515
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dc.contributor.authorFalceta-Gonçalves, D.en
dc.contributor.authorKowal, G.en
dc.contributor.authorFalgarone, E.en
dc.contributor.authorChian, A.en
dc.date.issued2014en
dc.identifier.citationNonlinear Processes in Geophysics, 2014; 21(3):587-604en
dc.identifier.issn1023-5809en
dc.identifier.issn1607-7946en
dc.identifier.urihttp://hdl.handle.net/2440/94515-
dc.description.abstractTurbulence is ubiquitous in the insterstellar medium and plays a major role in several processes such as the formation of dense structures and stars, the stability of molecular clouds, the amplification of magnetic fields, and the re-acceleration and diffusion of cosmic rays. Despite its importance, interstellar turbulence, like turbulence in general, is far from being fully understood. In this review we present the basics of turbulence physics, focusing on the statistics of its structure and energy cascade. We explore the physics of compressible and incompressible turbulent flows, as well as magnetised cases. The most relevant observational techniques that provide quantitative insights into interstellar turbulence are also presented. We also discuss the main difficulties in developing a three-dimensional view of interstellar turbulence from these observations. Finally, we briefly present what the main sources of turbulence in the interstellar medium could be.en
dc.description.statementofresponsibilityD. Falceta-Gonçalves, G. Kowal, E. Falgarone, and A. C.-L. Chianen
dc.language.isoenen
dc.publisherCopernicus Publicationsen
dc.rights© Author(s) 2014. CC Attribution 3.0 License.en
dc.titleTurbulence in the interstellar mediumen
dc.typeJournal articleen
dc.identifier.doi10.5194/npg-21-587-2014en
pubs.publication-statusPublisheden
dc.identifier.orcidChian, A. [0000-0002-8932-0793]en
Appears in Collections:Mathematical Sciences publications

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