Abstract
To date, it is well established that the heliosphere is filled with charged particles of various origins (solar wind and solar cosmic rays, GCR, anomalous component of cosmic rays, etc.). In general, they occupy a huge range of energies (about 20 orders of magnitude). In particular, solar cosmic rays (SCR) occupy the range of kinetic energies from Еk ≥ 1 MeV to Еk ≥ 10, possibly up to ~100 GeV (for protons). Below we will present the basic information on the transfer of particles, mainly using the example of SCR. The same transport laws are valid for GCRs, for their anomalous components, for particles of a different origin in interplanetary space, but taking into account other temporal and spatial scales. If particles move in coronal, interplanetary and geomagnetic fields without interacting with each other, then their transfer can be considered within the framework of a simple trajectory approach. Such an approach is possible in the case when the particle energy density is significantly lower than the magnetic energy density, i.e., when the condition
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mрnpv2/2 << B2/8π (6.1)
where mр, np and v are the mass, concentration and velocity of the proton, respectively, and B is the magnetic field strength. In the opposite case, it is necessary to take into account the collective interaction of the ensemble of particles with the surrounding magnetic field (self-consistent approach). As for the SCR itself, the kinetic energy Еk ~ 1 MeV/nucleon for most flares can be conventionally taken as the lower limit of their spectrum. However, we will not limit our consideration to the dominant SCR component (i.e., protons with energy Ep ≥ 1 MeV): the initial stage of particle acceleration from thermal velocities (see Chap. 5) is of fundamental interest, and the most acute problems of the formation of the SCR spectrum are just in the energy range Еk ≤ 1 MeV/nucleon. The transfer of energetic particles in the heliosphere implies various types of their motions and interactions: movement in large-scale magnetic structures, scattering by inhomogeneities of the interplanetary magnetic field, various kinds of drifts, wave-particle interactions, generation of disturbances in interplanetary plasma, etc. In addition, a particle may experience acceleration or deceleration, i.e. change your energy. In fact, we are talking about changes in the distribution function of particles f(r, p, t) in the process of transfer, while both the spatial coordinates (vector r) and the components of the particle velocity (its momentum p) can change.
Among the continuum of wacky theories,
there are sure to be some
whose predictions coincide with experiment.
Niels Bor
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Miroshnichenko, L. (2023). Transport of Particles in the Heliosphere. In: Solar-Terrestrial Relations. Springer, Cham. https://doi.org/10.1007/978-3-031-22548-2_6
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