Where Do Electrons Go in the Plasma State of Stars?

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SUMMARY

The discussion focuses on the behavior of free electrons in the plasma state of stars, specifically in the context of the Sun. When hydrogen atoms transition to plasma, free electrons are released and become part of the plasma, bouncing around without a specific destination. In the case of the Sun, these electrons contribute to the solar wind, which can extend to distances beyond the orbit of Pluto. Additionally, phenomena such as Coronal Mass Ejections can release large quantities of electrons that impact Earth, potentially disrupting radio and power systems.

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  • Understanding of plasma physics
  • Knowledge of solar phenomena, particularly solar wind
  • Familiarity with Coronal Mass Ejections and their effects
  • Basic concepts of electromagnetic fields in astrophysics
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  • Study the mechanisms behind Coronal Mass Ejections
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Astronomers, astrophysicists, and students interested in plasma physics and solar phenomena will benefit from this discussion.

shivakumar06
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dear sir,
when hydrogen atom is converted to plasma state, the free electron must be released. i am curious to know where does this electron go in case of plasma in stars.
thank you.
 
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It doesn't really go anywhere, it just becomes a free electron bouncing around in the plasma like all the free nucleons. The average charge of the plasma is still 0.
 
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Our own Sun is a star. In this case, electrons accelerate away from the Sun in the solar wind out to great distances - twice the orbit of Pluto - to the edge of the heliosphere! In powerful discharges known as Coronal Mass Ejections, huge quantities of electrons may impact Earth and cause harmful events such as disruption of radio and power grids.


http://en.wikipedia.org/wiki/Solar_wind
http://en.wikipedia.org/wiki/Coronal_mass_ejection
The solar wind is a stream of plasma released from the upper atmosphere of the Sun. It consists of mostly electrons and protons with energies usually between 1.5 and 10 keV. The stream of particles varies in density, temperature, and speed over time and over solar longitude. These particles can escape the Sun's gravity because of their high energy, from the high temperature of the corona and magnetic, electrical and electromagnetic phenomena in it.

The solar wind flows outward supersonically to great distances, filling a region known as the heliosphere, an enormous bubble-like volume surrounded by the interstellar medium. Other related phenomena include the aurora (Northern and Southern lights), the plasma tails of comets that always point away from the Sun, and geomagnetic storms that can change the direction of magnetic field lines and create strong currents in power grids on Earth.
 
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