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Magnetorotational instability in plasmas with mobile dust grains
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10.1063/1.4794342
/content/aip/journal/pop/20/3/10.1063/1.4794342
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/3/10.1063/1.4794342
View: Figures

Figures

Image of FIG. 1.
FIG. 1.

The normalized growth rate versus χ. It is assumed and for a Keplerian system. S stands for . The criterion (25) shows the critical value for an instability is S = 3 when . Hence the solid curve for S = 3.5 has zero growth rate from to . For the solid and dashed (S = 1.0) curves, γ increases first and then decreases as χ climbs. For the dotted (S = 0.1) and dashed-dotted (S = 0.01) curves, γ decreases from the beginning as χ grows.

Image of FIG. 2.
FIG. 2.

The growth rate γ normalized by versus ϵ. It is assumed and for a Keplerian system. Zhou's plotting area is around , where the growth rate is “obviously suppressed when considering dusty plasmas.” 22

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/content/aip/journal/pop/20/3/10.1063/1.4794342
2013-03-04
2014-04-17
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Magnetorotational instability in plasmas with mobile dust grains
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/3/10.1063/1.4794342
10.1063/1.4794342
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