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Paper: Turbulence Transport Modeling of the Temporal Outer Heliosphere
Volume: 484, Outstanding Problems in Heliophysics: From Coronal Heating to the Edge of the Heliosphere
Page: 1
Authors: Adhikari, L.; Zank, G. P.; Hu, Q.; Dosch, A.
Abstract: The evolution of the low-frequency MHD turbulence in the solar wind is thought to be responsible for the large-scale heating of the solar wind, scattering of the solar energetic particles (SEPs), and so forth. Zank et al. (1996) developed a turbulence transport model that describes the transport of the magnetic energy density and the correlation length throughout the heliosphere. Here, we assume that the solar cycle changes the solar wind properties in the heliosphere. It introduces a variable solar wind convection speed, time-dependent source terms and inner boundary conditions. A time-dependent form of the turbulence transport model of Zank et al. (1996) is solved by using an explicit finite difference scheme, and the fluctuations of magnetic energy density and correlation length are calculated along the trajectory of Voyager 2 assuming solar cycle variability for three different cases: Undriven Models, Stream Interaction Models, and Pickup Ion Driven Models. The theoretical model with all appropriate sources of turbulence is compared with the observed fluctuation of magnetic energy density of Voyager 2 data.
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