3.3.5.3 Energetic particles in interplanetary space

2005 ◽  
pp. 251-256
Author(s):  
M. Scholer
Keyword(s):  
Interplanetary Space ◽  
Energetic Particles

SOLAR ENERGETIC PARTICLES

2005 ◽  
Vol 20 (29) ◽  
pp. 6634-6641
Author(s):  
PÉTER KIRÁLY
Keyword(s):  
Solar Cycle ◽  
Interplanetary Space ◽  
Energetic Particles ◽  
Vital Role ◽  
Solar Energetic Particles ◽  
Interstellar Space ◽  
Interplanetary Shocks ◽  
Quiet Time ◽  
Solar Origin ◽  
Suprathermal Particles

Energetic particles recorded in the Earth environment and in interplanetary space have a multitude of origins, i.e. acceleration and propagation histories. At early days practically all sufficiently energetic particles were considered to have come either from solar flares or from interstellar space. Later on, co-rotating interplanetary shocks, the termination shock of the supersonic solar wind, planetary bow shocks and magnetospheres, and also coronal mass ejections (CME) were recognized as energetic particle sources. It was also recognized that less energetic (suprathermal) particles of solar origin and pick-up ions have also a vital role in giving rise to energetic particles in interplanetary disturbances. The meaning of the term "solar energetic particles" (SEP) is now somewhat vague, but essentially it refers to particles produced in disturbances fairly directly related to solar processes. Variation of intensity fluctuations with energy and with the phase of the solar cycle will be discussed. Particular attention will be given to extremes of time variation, i.e. to very quiet periods and to large events. While quiet-time fluxes are expected to shed light on some basic coronal processes, large events dominate the fluctuation characteristics of cumulated fluence, and the change of that fluctuation with energy and with the phase of the solar cycle may also provide important clues. Mainly ISEE-3 and long-term IMP-8 data will be invoked. Energetic and suprathermal particles that may never escape into interplanetary space may play an important part in heating the corona of the sun.

Radio Tracking of Solar Energetic Particles through Interplanetary Space

Science ◽  
1972 ◽  
Vol 178 (4062) ◽  
pp. 743-745 ◽  
Author(s):  
J. Fainberg ◽  
L. G. Evans ◽  
R. G. Stone
Keyword(s):  
Interplanetary Space ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Radio Tracking

scholarly journals Superdiffusive transport in laboratory and astrophysical plasmas

2015 ◽  
Vol 81 (6) ◽  
Author(s):  
G. Zimbardo ◽  
E. Amato ◽  
A. Bovet ◽  
F. Effenberger ◽  
A. Fasoli ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Interplanetary Space ◽  
Mean Square Displacement ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Space Physics ◽  
Anomalous Transport ◽  
Shock Acceleration ◽  
Astrophysical Plasmas ◽  
Superdiffusive Transport

In the last few years it has been demonstrated, both by data analysis and by numerical simulations, that the transport of energetic particles in the presence of magnetic turbulence can be superdiffusive rather than normal diffusive (Gaussian). The term ‘superdiffusive’ refers to the mean square displacement of particle positions growing superlinearly with time, as compared to the normal linear growth. The so-called anomalous transport, which in general comprises both subdiffusion and superdiffusion, has gained growing attention during the last two decades in many fields including laboratory plasma physics, and recently in astrophysics and space physics. Here we show a number of examples, both from laboratory and from astrophysical plasmas, where superdiffusive transport has been identified, with a focus on what could be the main influence of superdiffusion on fundamental processes like diffusive shock acceleration and heliospheric energetic particle propagation. For laboratory plasmas, superdiffusion appears to be due to the presence of electrostatic turbulence which creates long-range correlations and convoluted structures in perpendicular transport: this corresponds to a similar phenomenon in the propagation of solar energetic particles (SEPs) which leads to SEP dropouts. For the propagation of energetic particles accelerated at interplanetary shocks in the solar wind, parallel superdiffusion seems to be prevailing; this is based on a pitch-angle scattering process different from that envisaged by quasi-linear theory, and this emphasizes the importance of nonlinear interactions and trapping effects. In the case of supernova remnant shocks, parallel superdiffusion is possible at quasi-parallel shocks, as occurring in the interplanetary space, and perpendicular superdiffusion is possible at quasi-perpendicular shocks, as corresponding to Richardson diffusion: therefore, cosmic ray acceleration at supernova remnant shocks should be formulated in terms of superdiffusion. The possible relations among anomalous transport in laboratory, heliospheric, and astrophysical plasmas will be indicated.

scholarly journals Energetic particle investigation using the ERNE instrument

1996 ◽  
Vol 14 (5) ◽  
pp. 497-502 ◽  
Author(s):  
J. Torsti ◽  
E. Valtonen ◽  
L. Kocharov ◽  
M. Lumme ◽  
T. Eronen ◽  
...  
Keyword(s):  
Solar Flares ◽  
Particle Transport ◽  
Energetic Particle ◽  
Interplanetary Space ◽  
Solar Wind Plasma ◽  
Energetic Particles ◽  
Particle Energy ◽  
Particle Properties ◽  
Energetic Particle Transport ◽  
Accelerated Particles

Abstract. During solar flares and coronal mass ejections, nuclei and electrons accelerated to high energies are injected into interplanetary space. These accelerated particles can be detected at the SOHO satellite by the ERNE instrument. From the data produced by the instrument, it is possible to identify the particles and to calculate their energy and direction of propagation. Depending on variable coronal/interplanetary conditions, different kinds of effects on the energetic particle transport can be predicted. The problems of interest include, for example, the effects of particle properties (mass, charge, energy, and propagation direction) on the particle transport, the particle energy changes in the transport process, and the effects the energetic particles have on the solar-wind plasma. The evolution of the distribution function of the energetic particles can be measured with ERNE to a better accuracy than ever before. This gives us the opportunity to contribute significantly to the modeling of interplanetary transport and acceleration. Once the acceleration/transport bias has been removed, the acceleration-site abundance of elements and their isotopes can be studied in detail and compared with spectroscopic observations.

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