MHD flows at astropauses and in astrotails
arXiv:1501.05122 · doi:10.5194/ap-1-51-2014
Abstract
The geometrical shapes and the physical properties of stellar wind -- interstellar medium interaction regions form an important stage for studying stellar winds and their embedded magnetic fields as well as cosmic ray modulation. Our goal is to provide a proper representation and classification of counter-flow configurations and counter-flow interfaces in the frame of fluid theory. In addition we calculate flows and large-scale electromagnetic fields based on which the large-scale dynamics and its role as possible background for particle acceleration, e.g. in the form of anomalous cosmic rays, can be studied. We find that for the definition of the boundaries, which are determining the astropause shape, the number and location of magnetic null points and stagnation points is essential. Multiple separatrices can exist, forming a highly complex environment for the interstellar and stellar plasma. Furthermore, the formation of extended tail structures occur naturally, and their stretched field and streamlines provide surroundings and mechanisms for the acceleration of particles by field-aligned electric fields.
arXiv comment10 pages, 4 Figures
References in corpus (13)
- A model of acceleration of Anomalous Cosmic Rays by Reconnection in the Heliosheath
- Magnetic reconnection as the cause of cosmic ray excess from the heliospheric tail
- The Interstellar Magnetic Field Close to the Sun II
- The Astrosphere of the Asymptotic Giant Branch Star Irc+10216
- A Porous, Layered Heliopause
- The return of the bow shock
- Cometary Astropause of Mira Revealed in the Far-Infrared
- Stationary field-aligned MHD flows at astropauses and in astrotails. Principles of a counterflow configuration between a stellar wind and its interstellar medium wind
- Thin current sheets caused by plasma flow gradients in space and astrophysical plasma
- Reconnection at the Heliopause
- Fragmentation of electric currents in the solar corona by plasma flows
- Relation between current sheets and vortex sheets in stationary incompressible MHD
- 2D stationary resistive MHD flows: borderline to magnetic reconnection solutions