Carrington Rotation 2196

Simulation of Solar Wind quantities for Carrington Rotation 2196 by making use of my APOLLO model computer code; which is a remastered version completely rewritten in Julia. Initial conditions were generated from:

https://ccmc.gsfc.nasa.gov/

Solar Wind Radial Speed

Solar Wind Density

Solar Wind Videos

To watch my latest videos (concerning computational electromagnetics, computational magnetohydrodynamics, computational fluid dynamics, smoothed particle hydrodynamics, kinetic plasma simulations and gravitational n-body solvers) check my youtube channel:

https://www.youtube.com/@michaelpieters1844

Create Your Own Website With JouwWeb

Not only does the Sun radiate light of different frequencies, it also blows out huge bubbles of supersonic plasma, engulfing all planets and a host of other bodies, shaping their environments. Solar wind related phenomena include geomagnetic storms on Earth, aurora and comet plasma tails.

Interplanetary space is separated by a source surface into two regions: the corona and the heliosphere. Within the source surface, the solar magnetic field controls the plasma. Outside, the magnetic field only plays a minor role in the dynamics.

The corona is modeled by a potential field source surface model (PFSS) that takes magnetograms as initial condition. The magnetic field is reconstructed with associated Legendre Polynomials through a least-squared approach.

The heliospheric solar wind is determined by applying a conservative discretization scheme to the Euler equations with a gravity source in a rotating frame.

Due to solar rotation the wind twists into an Archimedean spiral. The variability of the solar wind causes regions of compression and rarefaction. The magnetic fieldlines are dragged out by the solar wind.