The transport of low-frequency turbulence in the super-Alfvénic solar wind

14th Annual International Astrophysics Conference: Linear and Nonlinear Particle Energization throughout the Heliosphere and Beyond

物理学;天文学

Adhikari, L.^1,2 ; Zank, G.P.^1,2 ; Bruno, R.^3 ; Telloni, D.^4 ; Hunana, P.^2 ; Dosch, A.^2 ; Marino, R.^5 ; Hu, Q.^1,2

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

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

I-00133, Italy^3

INAF-Astrophysical Observatory of Torino, Via Osservatorio 20, Pino Torinese

I-10025, Italy^4

National Center for Atmospheric Research, P.O. Box 3000, Boulder

CO

80307, United States^5

关键词: Azimuthal angle;    Inhomogeneous flow;    Interplanetary magnetic fields;    Solar wind flow;    Transport equation;    Transverse components;    Turbulence transports;    Wind temperature;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/642/1/012001/pdf
DOI  :  10.1088/1742-6596/642/1/012001

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

Understanding the transport of low-frequency turbulence in an expanding magnetized flow is very important in analyzing numerous problems in space physics and astrophysics. Zank et al 2012 developed six general coupled turbulence transport equations, including the Alfvén velocity to describe the transport of low-frequency turbulence for any inhomogeneous flows, including sub-Alfvénic coronal flows, and super-Alfvénic solar wind flows. Here, we solve the 1D steady state six coupled turbulence transport equations of Zank et al 2012, and the transport equation corresponding to the solar wind temperature in the super-Alfvénic solar wind flows from 0.29 to 100 AU without the Alfvén velocity. We calculate turbulent quantities corresponding to Voyager 2 data sets for three cases; i) a positive and negative sign of Br; ii) the azimuthal angle φ = tan-1(Bt/Br), and iii) a positive and negative sign of Bt, where Brand Btare the radial and transverse components of the interplanetary magnetic field, respectively. We compare our theoretical results to the observational results, and find good agreement between them.