Magnetic helicity signature produced by cross-field 2D turbulence

Journal Article · Thu Jun 13 00:00:00 EDT 2013 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.4811032· OSTI ID:22118613

Markovskii, S. A.; Vasquez, Bernard J. ^[1]

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1. Space Science Center, Institute for the Study of Earth, Oceans, and Space, and Department of Physics, University of New Hampshire, Durham, NH 03824 (United States)

Hybrid numerical simulations of freely decaying 2D turbulence are presented. The background magnetic field is perpendicular to the simulation plane, which eliminates linear kinetic Alfven waves from the system. The normalized magnetic helicity of the initial large-scale fluctuations is zero, while the normalized cross-helicity is not. As the turbulence evolves, it develops nonzero magnetic helicity at smaller scales, in the proton kinetic range. In the quasi-steady state of evolution, the magnetic helicity spectrum has a peak consistent with the solar wind observations.

• OSTI ID: 22118613
• Journal Information: AIP Conference Proceedings, Vol. 1539, Issue 1; Conference: SOLAR WIND 13: 13. international solar wind conference, Big Island, HI (United States), 17-22 Jun 2012; Other Information: (c) 2013 AIP Publishing LLC; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ALFVEN WAVES
ASTROPHYSICS
COMPUTERIZED SIMULATION
FLUCTUATIONS
HELICITY
INTERPLANETARY MAGNETIC FIELDS
MAGNETISM
NUMERICAL ANALYSIS
PLASMA
PLASMA SIMULATION
SOLAR PROTONS
SOLAR WIND
STEADY-STATE CONDITIONS
TURBULENCE