![]() ![]() Where $Z_$ is the number density of species $s$. The plasma is quasi-neutral so the total electron number density will satisfy: In general, the corona and solar wind are comprised of ~95% protons, ~4% alpha-particles, and the remaining ~1% contains all the heavier ions. I would also glance at the references therein to see some examples of other coronal number density models. The paper by Gopalswamy and Yashiro discusses some simplified number density models that vary with radial distance, for instance. ![]() Spectroscopic measurements indicate strong ionization in the corona and a plasma temperature in excess of 1000000 kelvins, much hotter than the surface of the Sun, known as the photosphere. It is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The solar wind, which sweeps radially outward through the whole solar system, is. As a result of the Sun's magnetic field, the corona's size and form change all the time. It has a temperature of around two million kelvins and a very low density. The Sun's corona lies above the chromosphere and extends millions of kilometres into outer space. The corona is the outermost portion of the Sun's atmosphere, made mostly of plasma (hot ionised gas). At what altitude do you intend to model the corona? The number density varies with altitude. A corona is the outermost layer of a star's atmosphere. It has a temperature of approximately two million kelvins and an extremely low density. If I intend to model the corona as an homogenous shell (which definitely is a strong assumption), what are the ranges of the number densities of the abundant particles? corona, outermost region of the Sun’s atmosphere, consisting of plasma (hot ionized gas). I have provided some references in the following answer. Iron is present as well, but in much lower amounts. Beyond alpha-particles, the number densities drop exponentially with CNO constituents plus sulphur and silicon picking up the tail. The main particle species (order of particle number density from largest to smallest) are electrons, protons, and alpha-particles. What are the main constituents of the coronal plasma? ![]() The location of the associated termination shocks would be determined largely by a balance of hydrodynamic and magnetic forces (much more heavily weighted toward the former than latter in many cases). The size and shape of the Sun's region of influence in the interstellar medium (ISM) depends upon the strength/speed of the solar wind and the properties of the ISM. This is tricky because the corona actually stops at the termination shock of the heliosphere. Is there any rule of thumb for the average dimensions of the corona, possibly depending on the mass of or other parameters of the star? Is it possible to estimate to at least an order of magnitude how thick a shell around a star would be which would be most likely be filled with plasma? So my best guess is that the corona is also remarkably "average." Technically the most abundant stars are red dwarfs and the Sun is a yellow dwarf, but dwarf stars are the most abundant and the sun is part of the main sequence line of stars. The Sun is remarkably "average" (e.g., see ). ![]()
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