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The energetic particles are in general believed to be accelerated by the Fermi acceleration mechanism.
Surprisingly, the resulting energy spectrum anticipated from this physical setup is very similar to the one found for first order Fermi acceleration.
Fermi acceleration is one plausible particle acceleration process in radio-loud active galaxies.
This random process is now called second-order Fermi acceleration, because the mean energy gain per bounce depends on the mirror velocity squared, .
Rieger, Bosch-Ramon and Duffy: Fermi acceleration in astrophysical jets.
This model was introduced in 1968 in, and studied in, by L. D. Pustyl'nikov in connection with justification of the Fermi acceleration mechanism.
FUM is a variant of Enrico Fermi's primary work on acceleration of cosmic rays, namely Fermi acceleration.
Two main mechanisms of acceleration are possible: diffusive shock acceleration (DSA, sometimes referred as first-order Fermi acceleration) or shock-drift mechanism.
The Fermi-Pustyl'nikov model, named after Enrico Fermi and Lev Pustyl'nikov, is a model of the Fermi acceleration mechanism.
This is because Fermi acceleration only applies to particles with energies exceeding the thermal energies, and frequent collisions with surrounding particles will cause severe energy loss and as a result no acceleration will occur.
Fermi acceleration, sometimes referred to as diffusive shock acceleration (a subclass of Fermi acceleration), is the acceleration that charged particles undergo when being repeatedly reflected, usually by a magnetic mirror.
There are two types of Fermi acceleration: First order Fermi acceleration (in shocks) and Second Order Fermi acceleration (in the environment of moving magnetized gas clouds).
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