SH11B-2388
Modeling Magnetic Flux-Ropes Structures

Monday, 14 December 2015
Poster Hall (Moscone South)
Teresa Nieves-Chinchilla, Catholic University of America, Washington, DC, United States, Mark Linton, US Naval Research Laboratory, Washington, DC, United States, Miguel A. UAH Hidalgo, Alcala University, Madrid, Spain, Angelos Vourlidas, Applied Physics Laboratory Johns Hopkins, Space Department, Laurel, MD, United States, Neel Savani, University of Maryland Baltimore County, Baltimore, MD, United States, Adam Szabo, NASA Goddard Space Flight Center, Greenbelt, MD, United States, Charles J Farrugia, New hampshire university, Durham, NH, United States and Wenyuan Yu, University of New Hampshire Main Campus, Durham, NH, United States
Abstract:
Flux-ropes are usually associated with magnetic structures embedded in the interplanetary Coronal Mass Ejections (ICMEs) with a depressed proton temperature (called Magnetic Clouds, MCs). However, small-scale flux-ropes in the solar wind are also identified with different formation, evolution, and dynamic involved.

We present an analytical model to describe magnetic flux–rope topologies. The model is generalized to different grades of complexity. It extends the circular-cylindrical concept of Hidalgo et al. (2002) by introducing a general form for the radial dependence of the current density. This generalization provides information on the force distribution inside the flux rope in addition to the usual parameters of flux-rope geometrical information and orientation. The generalized model provides flexibility for implementation in 3-D MHD simulations.

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