Abstract
AbstractIn this chapter we discuss the concepts that govern the motion of charged particles in the geomagnetic field and the principles how they stay trapped in the radiation belts. The basic particle orbit theory can be found in most plasma physics textbooks. We partly follow the presentation in Koskinen (Physics of space storms, from solar surface to the earth. Springer-Praxis, Heidelberg, 2011). A more detailed discussion can be found in Roederer and Zhang (Dynamics of magnetically trapped particles. Springer, Heidelberg, 2014). A classic treatment of adiabatic motion of charged particles is Northrop (The adiabatic motion of charged particles. Interscience Publishers, Wiley, New York, 1963).
Highlights
Integration of the equation of motion in realistic magnetic field configurations must be done numerically
The equation of motion of a charged particle m dv = q(v × B) (2.2) dt describes a helical orbit with constant speed along the magnetic field and circular motion around the magnetic field line with the angular frequency ωc = |q|B . (2.3) m
Looking along the magnetic field, the particle rotating clockwise has a negative charge. In plasma physics this is the convention of right-handedness. This way we have decomposed the motion into two elements: constant speed v along the magnetic field and circular velocity v⊥ perpendicular to the field
Summary
In this chapter we discuss the concepts that govern the motion of charged particles in the geomagnetic field and the principles how they stay trapped in the radiation belts. The basic particle orbit theory can be found in most plasma physics textbooks. We partly follow the presentation in Koskinen (2011). A more detailed discussion can be found in Roederer and Zhang (2014). A classic treatment of adiabatic motion of charged particles is Northrop (1963).
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