Magnetohydrostatic modelling of stellar coronae
arXiv:1511.06133 · doi:10.1093/mnras/stv2714
Abstract
We introduce to the stellar physics community a method of modelling stellar coronae that can be considered to be an extension of the potential field. In this approach, the magnetic field is coupled to the background atmosphere. The model is magnetohydrostatic (MHS) and is a balance between the Lorentz force, the pressure gradient and gravity. Analytical solutions are possible and we consider a particular class of equilibria in this paper. The model contains two free parameters and the effects of these on both the geometry and topology of the coronal magnetic field are investigated. A demonstration of the approach is given using a magnetogram derived from Zeeman-Doppler imaging of the 0.75 M M-dwarf star GJ 182.
arXiv commentAccepted for publication in MNRAS
References in corpus (14)
- Large-scale magnetic topologies of early M dwarfs
- Can we predict the global magnetic topology of a pre-main sequence star from its position in the Hertzsprung-Russell diagram?
- The global magnetic topology of AB Doradus
- Powerful Winds from Low-Mass Stars: V374 Peg
- Global 3D Simulations of Disc Accretion onto the classical T Tauri Star V2129 Oph
- The coronal structure of AB Dor determined from contemporaneous Doppler imaging and X-ray spectroscopy
- Magnetic Field Extrapolations in the Corona: Success and Future Improvements
- 3D MHD Flux Emergence Experiments: Idealized models and coronal interactions
- Influence of surface stressing on stellar coronae and winds
- The Coronal Structure of AB Doradus
- Analytic and numerical models of the 3D multipolar magnetospheres of pre-main sequence stars
- Coronal structure of the cTTS V2129 Oph
- Coronal Structure of Low-Mass Stars
- Non-symmetric magnetohydrostatic equilibria: a multigrid approach
Cited by in corpus (5)
- Magnetohydrostatic modeling of AR11768 based on a SUNRISE/IMaX vector magnetogram
- Interpreting magnetic helicity flux in solar flux emergence
- Analytical Three-dimensional Magnetohydrostatic Equilibrium Solutions for Magnetic Field Extrapolation Allowing a Transition from Non-force-free to Force-free Magnetic Fields
- Three-Dimensional Solutions of the Magnetohydrostatic Equations For Rigidly Rotating Magnetospheres in Cylindrical Coordinates
- Effects of shell thickness on cross-helicity generation in convection-driven spherical dynamos