MHD turbulence in the Earth's plasma sheet: Dynamics, dissipation, and driving

By J. Borovsky, H. Funsten. 2003

192 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/00424fb9864768a0ef490b9dd30ed7d04b9677fa

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. M. Denton
2. J. Borovsky
3. Fran Bagenal
4. P. Delamere

In Molecular Biology

1. J. Borovsky
2. M. Denton
3. Fran Bagenal
4. P. Delamere

Citations in the corpus

• Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?: FLUX TUBE TEXTURE OF SOLAR WIND (2008, background): “…is fundamentally different from the turbulence of the solar wind because the plasma sheet turbulence is a ‘‘turbulence-in-a-box’’ [Borovsky et al., 1997, Borovsky and Funsten, 2003]; however, owing to the flux tube texture of the solar wind, the two types of turbulence may not be so dissimilar.”
• A statistical look at plasmaspheric drainage plumes (2008, background): “…can be compared with hodograms of two other A09221 BOROVSKY AND DENTON: PLASMASPHERIC DRAINAGE PLUMES 17 of 23 A09221 plasmas well known to be turbulent: the solar wind [Tu and Marsch, 1995; Goldstein et al., 1995] and the Earth’s plasma sheet [Borovsky and Funsten, 2003; Weygand et al., 2005].”
• Solar wind interaction with Jupiter's magnetosphere (2009, background): “Alternatively, spatial structures frozen into the flow resulting from reconnection flows, nonlinear development of Kelvin‐Helmholtz vortices, interchange instability, mode conversion, or other instabilities [ Borovsky and Funsten, 2003 ] can lead to eddy diffusion across the boundary layer [Borovsky”