ScholarLens Back to search
1994•Geophysical Research LettersRequires access

3‐D Simulation of high‐latitude interaction regions: Comparison with Ulysses results

V. J. Pizzo, J. T. Gosling

Open publisher page 94 citations

Abstract

A three‐dimensional (3‐D) magnetohydrodynamic (MHD) numerical model is used to simulate the global evolution of a steady, tilted‐dipole solar wind flow configuration similar to that prevalent in interplanetary space in 1993. Systematic latitudinal changes in the structure of a corotating interaction region (CIR) near 5 AU is shown to agree well with recent Ulysses observations. The abrupt disappearance of forward shocks and continued persistence of reverse shocks poleward of the latitude where Ulysses crossed the southern edge of the coronal streamer belt is explained as a natural consequence of the 3‐D flow geometry.

About this research paper

What this paper is about

A three‐dimensional (3‐D) magnetohydrodynamic (MHD) numerical model is used to simulate the global evolution of a steady, tilted‐dipole solar wind flow configuration similar to that prevalent in interplanetary space in 1993. Systematic latitudinal changes in the structure of a corotating interaction region (CIR) near 5 AU is shown to agree well with recent Ulysses observations. The abrupt disappearance of forward shocks and continued persistence of reverse shocks poleward of the latitude where Ulysses crossed the southern edge of the coronal streamer belt is explained as a natural consequence of the 3‐D flow geometry.

Why it matters

OpenAlex reports 94 citations for this work. Citation counts describe recorded attention and do not establish research quality.

Key contribution

A contribution statement is not available in the OpenAlex record.

Method / approach

Method details are not available in the OpenAlex metadata.

Main findings

Findings are not separately available in the OpenAlex metadata.

Limitations

Limitations are not available in the OpenAlex metadata.

Applications

Application details are not available in the OpenAlex metadata.

Available abstract

A three‐dimensional (3‐D) magnetohydrodynamic (MHD) numerical model is used to simulate the global evolution of a steady, tilted‐dipole solar wind flow configuration similar to that prevalent in interplanetary space in 1993. Systematic latitudinal changes in the structure of a corotating interaction region (CIR) near 5 AU is shown to agree well with recent Ulysses observations. The abrupt disappearance of forward shocks and continued persistence of reverse shocks poleward of the latitude where Ulysses crossed the southern edge of the coronal streamer belt is explained as a natural consequence of the 3‐D flow geometry.

Key concepts: Physics, Magnetohydrodynamic drive, Solar wind, Magnetohydrodynamics, Latitude, Heliosphere, Interplanetary spaceflight, Geophysics

Related papers

Related paper 1Related paper 2Related paper 3
Back to paper searchBrowse research topicsOriginal source
3‐D Simulation of high‐latitude interaction regions: Comparison with Ulysses results — Research Paper | ScholarLens