Nonlinear drag force in dusty plasmas
Creators
- 1. Max Planck Institute for Extraterrestrial Physics, 85741 Garching (Germany)
- 2. Department of Physical Sciences, University of Naples 'Federico II' and INFN section of Napoli (Italy)
- 3. General Physics Institute Russian Academy of Science, 119991 Moscow (Russian Federation)
Description
The condition for large angle scattering in ion-grain collisions, which determine the nonlinear part of the ion drag force, coincides with the condition for the grain screening to be nonlinear (eφ/Ti>1 where φ is the electrostatic grain potential and Ti is the ion mean energy), a condition met in many laboratory experiments. A self-consistent treatment of the nonlinear ion-drag force therefore requires a correct treatment of nonlinear screening. A model to account for the nonlinearity is presented and the drag force calculated, showing that it can be substantially larger than that for linear screening. An important physical feature found in the present investigation is that nonlinear screening corresponds to almost full screening inside a finite radius and that large angle scattering occurs only inside this radius. The nonlinear ion-drag force is found to have a strong dependence on the grain size, ratio of ion to electron temperatures, and ion density
Additional details
Identifiers
- DOI
- 10.1063/1.2130312;
Publishing Information
- Journal Title
- Physics of Plasmas
- Journal Volume
- 12
- Journal Issue
- 11
- Journal Page Range
- p. 112311-112311.9
- ISSN
- 1070-664X
- CODEN
- PHPAEN
INIS
- Country of Publication
- United States
- Country of Input or Organization
- International Atomic Energy Agency (IAEA)
- INIS RN
- 37085556
- Subject category
- S70: PLASMA PHYSICS AND FUSION TECHNOLOGY;
- Descriptors DEI
- ELECTRON COLLISIONS; ELECTRON TEMPERATURE; GRAIN SIZE; ION COLLISIONS; ION DENSITY; ION TEMPERATURE; NONLINEAR PROBLEMS; PLASMA; PLASMA DENSITY; PLASMA POTENTIAL; SCATTERING
- Descriptors DEC
- COLLISIONS; ELECTRIC POTENTIAL; MICROSTRUCTURE; SIZE
Optional Information
- Notes
- (c) 2005 American Institute of Physics