Researchers used MAGEC code for simulating the solar atmosphere from the convection zone to the corona.
MAGEC is a radiative magnetohydrodynamic (MHD) simulation tool. By using this, conservation of mass, momentum, magnetic flux, and energy in a plasma are calculated. It models how plasma (ionized gas) behaves under magnetic fields, radiation, and thermal conduction.
The solar atmosphere has shocks (sudden jumps in temperature and density)in the chromosphere. MAGEC uses a shock-capturing method.
The Sun’s chromosphere and corona lose energy by emitting radiation. MAGEC computes radiative losses based on local temperature and density.
Thermal conduction is very strong along magnetic field lines in the corona but weak across them. MAGEC includes both: Parallel conduction (along B-fields): dominant in the corona. Perpendicular conduction (across B-fields): usually small but found to have cumulative effects. To handle conduction numerically, they used a hyperbolic (flux-limited) approach meaning heat flux reacts like a wave that propagates at a finite speed.
Magnetic field geometry controls coronal heating. The researchers found that how magnetic field lines are arranged strongly affects the Sun’s temperature structure. Open magnetic fields → hotter and more extended corona.
Magnetic field geometry and cross-field thermal conduction play key roles in shaping coronal temperatures.
The vertical magnetic field keeps the corona hotter at medium heights than a loop-shaped (arcade) field does.
0 comments:
Post a Comment