Magnetohydrodynamics turbulence: An astronomical perspective |
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Authors: | S SRIDHAR |
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Institution: | (1) Astronomy Department, University of Florence, Florence, Italy;(2) SIDC, Royal Observatory of Belgium, Bruxelles, Belgium;(3) JPL, Pasadena, CA, USA;(4) Imperial College, London, UK;(5) Present address: IAS, Orsay, France |
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Abstract: | Early work on magnetohydrodynamic (MHD) turbulence in the 1960s due, independently, to Iroshnikov and Kraichnan (IK) considered
isotropic inertial-range spectra. Whereas laboratory experiments were not in a position to measure the spectral index, they
showed that the turbulence was strongly anisotropic. Theoretical horizons correspondingly expanded in the 1980s, to accommodate
both the isotropy of the IK theory and the anisotropy suggested by the experiments. Since the discovery of pulsars in 1967,
many years of work on interstellar scintillation suggested that small-scale interstellar turbulence must have a hydromagnetic
origin; but the IK spectrum was too flat and the ideas on anisotropic spectra too qualitative to explain the observations.
In response, new theories of balanced MHD turbulence were proposed in the 1990s, which argued that the IK theory was incorrect,
and made quantitative predictions of anisotropic inertial-range spectra; these theories have since found applications in many
areas of astrophysics. Spacecraft measurements of solar-wind turbulence show that there is more power in Alfvén waves that
travel away from the Sun than towards it. Theories of imbalanced MHD turbulence have now been proposed to address interplanetary
turbulence. This very active area of research continues to be driven by astronomy. |
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