Open and closed magnetic configurations of twisted flux tubes
arXiv:1904.03149 · doi:10.3847/1538-4357/ab141a
Abstract
We construct two classes of magnetohydrostatic (MHS) equilibria for an axisymmetric vertical flux tube spanning from the photosphere to the lower part of the transition region within a realistic stratified solar atmosphere subject to solar gravity. We assume a general quadratic expression of the magnetic flux function for the gas pressure and poloidal current and solve the Grad-Shafranov equation analytically. The solution is a combination of a homogeneous and a particular part where the former is separable by a Coulomb function in and exponential in , while the particular part is an open configuration that has no dependence. We also present another open field solution by using a self-similar formulation with two different profile functions and incorporating stratified solar gravity to maintain the magnetohydrostatic equilibria, which is a modification of earlier self-similar models with a twist. We study the admitted parameter space that is consistent with the conditions in the solar atmosphere and derive magnetic and the thermodynamic structures inside the flux tube that are reasonably consistent with the photospheric magnetic bright points (MBPs) for both open and closed field Coulomb function and self-similar models as estimated from observations and simulations. The obtained open and closed field flux tube solutions can be used as the background conditions for the numerical simulations for the study of the wave propagation through the flux tubes. The solutions can also be used to construct realistic magnetic canopies.
arXiv comment34 pages; 21 figures with 29 sub-figures; 6 tables, Accepted in the Astrophysical Journal
References in corpus (16)
- Emergence of Small-Scale Magnetic Loops in the Quiet Sun Internetwork
- Fully resolved quiet-Sun magnetic flux tube observed with the Sunrise IMaX instrument
- The size distribution of magnetic bright points derived from Hinode/SOT observations
- Wave propagation and energy transport in the magnetic network of the Sun
- Magnetic field strength distribution of magnetic bright points inferred from filtergrams and spectro-polarimetric data
- Magnetohydrostatic equilibrium. I: Three-dimensional open magnetic flux tube in the stratified solar atmosphere
- Torsional Alfven Waves in Solar Magnetic Flux Tubes of Axial Symmetry
- A photospheric bright point model
- Separable solutions of force-free spheres and applications to solar active regions
- On the relationship between G-band bright point dynamics and their magnetic field strengths
- Plasma properties and Stokes profiles during the lifetime of a photospheric magnetic bright point
- The dark side of solar photospheric G-band bright points
- Comparison of force-free coronal magnetic field modeling using vector fields from Hinode and Solar Dynamics Observatory
- Magnetohydrostatic equilibrium. II. Three-dimensional multiple open magnetic flux tubes in the stratified solar atmosphere
- A global galactic dynamo with a corona constrained by relative helicity
- Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere