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Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Nordic Institute for Theoretical Physics (Nordita).
2011 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 737, no 2, 62- p.Article in journal (Refereed) Published
Abstract [en]

The large-scale dynamics of plasmas is well described within the framework of magnetohydrodynamics (MHD). However, whenever the ion density of the plasma becomes sufficiently low, the Hall effect is likely to become important. The role of the Hall effect has been studied in several astrophysical plasma processes, such as magnetic reconnection, magnetic dynamo, MHD turbulence, or MHD instabilities. In particular, the development of small-scale instabilities is essential to understand the transport properties in a number of astrophysical plasmas. The magneto-rotational instability (MRI), which takes place in differentially rotating accretion disks embedded in relatively weak magnetic fields, is just one example. The influence of the large-scale velocity flows on small-scale instabilities is often approximated by a linear shear flow. In this paper, we quantitatively study the role of the Hall effect on plasmas embedded in large-scale shear flows. More precisely, we show that an instability develops when the Hall effect is present, which we therefore term as the Hall magneto-shear instability. As a particular case, we recover the so-called MRI and quantitatively assess the role of the Hall effect on its development and evolution.

Place, publisher, year, edition, pages
2011. Vol. 737, no 2, 62- p.
Keyword [en]
instabilities, magnetohydrodynamics (MHD), plasmas
National Category
Natural Sciences
URN: urn:nbn:se:su:diva-68292DOI: 10.1088/0004-637X/737/2/62ISI: 000294013600016OAI: diva2:477975
authorCount :3Available from: 2012-01-15 Created: 2012-01-03 Last updated: 2012-01-15Bibliographically approved

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Brandenburg, Axel
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