The solar wind is a weakly collisional non homogeneous plasma; gradients associated to density, velocity shears and current sheets are often observed. In situ observations also show that the solar wind plasma is far from thermal equilibrium and particle distribution functions are not isotropic. The presence of a temperature anisotropy can be the source of free energy for kinetic instabilities and their unstable fluctuations may grow and propagate in the plasma. However, how these fluctuations evolve in a non homogeneous medium and how they interact and influence local coherent structures, is still an open question. We report preliminary numerical simulations that describe the evolution of current sheets in a non thermal plasma, focusing on the interaction between kinetic effects driven by a proton temperature anisotropy and magnetic reconnection processes.
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13 June 2013
SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference
17–22 June 2012
Big Island, Hawaii
Research Article|
June 13 2013
Proton temperature anisotropy and current sheet stability: 2-D hybrid simulations
Lorenzo Matteini;
Lorenzo Matteini
Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Italy and now at Imperial College London, London, SW7 2AZ,
United Kingdom
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Simone Landi;
Simone Landi
Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze,
Italy
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Marco Velli;
Marco Velli
Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Italy and Jet Propulsion Laboratory, Pasadena, California,
USA
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William H. Matthaeus
William H. Matthaeus
Bartol Research Institute, Department of Physics and Astronomy, University of Delaware,
USA
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AIP Conf. Proc. 1539, 247–250 (2013)
Citation
Lorenzo Matteini, Simone Landi, Marco Velli, William H. Matthaeus; Proton temperature anisotropy and current sheet stability: 2-D hybrid simulations. AIP Conf. Proc. 13 June 2013; 1539 (1): 247–250. https://doi.org/10.1063/1.4811034
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