An exact analytical solution for the interstellar magnetic field in the vicinity of the heliosphere
arXiv:1412.7199 · doi:10.1088/0004-637X/805/2/173
Abstract
An analytical representation of the interstellar magnetic field in the vicinity of the heliosphere is derived. The three-dimensional field structure close to the heliopause is calculated as a solution of the induction equation under the assumption that it is frozen into a prescribed plasma flow resembling the characteristic interaction of the solar wind with the local interstellar medium. The usefulness of this analytical solution as an approximation to self-consistent magnetic field configurations obtained numerically from the full MHD equations is illustrated by quantitative comparisons.
13 pages, 4 figures, accepted for publication at ApJ. The MPEG animation referenced in Figure 3 may be accessed via [http://www.tp4.rub.de/heliophysics/movies/pflow_drape+btime_annot.mp4]
References in corpus (5)
- Anisotropy and Corotation of Galactic Cosmic Rays
- The effects of a kappa-distribution in the heliosheath on the global heliosphere and ENA flux at 1 AU
- Comparing various multi-component global heliosphere models
- Cosmic Ray Transport in Heliospheric Magnetic Structures: I. Modeling Background Solar Wind Using the CRONOS MHD Code
- The Local Bubble and Interstellar Material Near the Sun