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dc.contributor.authorMukhopadhyay, Banibrata
dc.contributor.authorAfshordi, Niayesh
dc.contributor.authorNarayan, Ramesh
dc.date.accessioned2019-09-22T14:23:41Z
dc.date.issued2006
dc.identifier.citationMukhopadhyay, Banibrata, Niayesh Afshordi, and Ramesh Narayan. 2006. “Growth of Hydrodynamic Perturbations in Accretion Disks: Possible Route to Non-Magnetic Turbulence.” Advances in Space Research 38 (12): 2877–79. https://doi.org/10.1016/j.asr.2005.09.048.
dc.identifier.issn0273-1177
dc.identifier.issn1879-1948
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384862*
dc.description.abstractWe study the possible origin of hydrodynamic turbulence in cold accretion disks such as those in star-forming systems and quiescent cataclysmic variables. As these systems are expected to have neutral gas, the turbulent viscosity is likely to be hydrodynamic in origin, not magnetohydrodynamic. Therefore, MRI will be sluggish or even absent in such disks. Although there are no exponentially growing eigenmodes in a hydrodynamic disk because of the non-normal nature of the eigenmodes, a large transient growth in the energy is still possible, which may enable the system to switch to a turbulent state. For a Keplerian disk, we estimate that the energy will grow by a factor of 1000 for a Reynolds number close to a million.
dc.language.isoen_US
dc.publisherElsevier
dash.licenseLAA
dc.titleGrowth of hydrodynamic perturbations in accretion disks: Possible route to non-magnetic turbulence
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalAdvances in Space Research
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:23:41Z
dash.workflow.comments1Science Serial ID 691
dc.identifier.doi10.1016/j.asr.2005.09.048
dash.source.volume38;12
dash.source.page2877-2879


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