Turbulence transport within the Heliosphere

13th Annual International Astrophysics Conference: Voyager, IBEX, and the Interstellar Medium

物理学;天文学

Adhikari, L.^1,2 ; Zank, G.P.^1,2 ; Bruno, R.^3 ; Telloni, D.^3 ; Hunana, P.^2 ; Dosch, A.^2

Department of Space Science, University of Alabama in Huntsville, Huntsville

AL

35899, United States^1

Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville

AL

35899, United States^2

AA(INAF-IAPS Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere 100, Roma

00133, Italy^3

关键词: Correlation lengths;    Coupled transport equations;    Heliosheath;    Heliospheres;    Propagating mode;    Residual energy;    Turbulence transports;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/577/1/012001/pdf
DOI  :  10.1088/1742-6596/577/1/012001

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

This work continues the investigation of turbulence transport throughout the supersonic solar wind initiated in Zank et al 1996 [27] and Zank et al 2012 [20]. [20] developed a system of six coupled transport equations that describe the transport of energy corresponding to forward propagating (g) and backward propagating modes (f), the residual energy (ED), and the correlation lengths corresponding to forward propagating modes (λ-), backward propagating modes (λ+), and the correlation length (λD) for residual energy. These models can be applied to both sub-Alfvénic (such as the lower corona) and super-Alfvénic (e.g., supersonic solar wind and inner heliosheath) flows. The correlation lengths calculated from our model are in good agreement with those observed. The evolution of related parameters is also calculated from 0.29 AU to 5 AU.