http://polaris.nipr.ac.jp/~ryuho/coem/Parker1965PSS.pdf

The passage of energetic charged particles through interplanetary space

Matter which is exposed to cosmic radiation undergoes characteristic changes in its chemical and isotopic composition. Such irradiated material can be found in many places on earth and belongs to either of two categories:

Cosmic ray produced radioactivity on the earth.

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A theory for the self-consistent configuration of upstream hydromagnetic waves, upstream energetic storm particle (ESP) events, and downstream postshock ion enhancements at interplanetary traveling shocks is presented. The observations of upstream ultralow frequency waves and those ESP events and postshock enhancements which exhibit approximately isotropic ion distributions in the solar wind or shock frame are briefly reviewed. The theory of Lee (1982) for application to interplanetary traveling shocks is modified and analytical solutions for the wave spectrum as a function of wavenumber and z are presented along with the ion omnidirectional distribution functions as functions of energy and z for all ion species. The theory quantitatively explaines the observed features of the shock-associted energetic ions and predicts the configuration of upstream hydromagnetic waves.

Coupled hydromagnetic wave excitation and ion acceleration at interplanetary traveling shocks

Data from the Goddard particle experiments on IMPs 4, 5, 7, and 8, and ISEE 3 are used to model particle intensity profiles including prompt solar particles and the effects of shocks. It is shown that the intensity profiles of solar protons depend on the heliolongitude, and it is suggested that the major controlling agent is the existence of an interplanetary (IP) shock. Shocks are strongest when observed along the radial from the source region, with the highest shock-associated intensities generally observed from central meridian flares. Using a recently derived model for the large-scale structure of IP shocks, the change in shape as a function of heliolongitude is explained.

The role of interplanetary shocks in the longitude distribution of solar energetic particles

A full description of the cosmic ray experiment on Explorer 12 is given and cosmic ray measurements made during the solar event of September 28, 1961, are reported and discussed. Galactic cosmic ray measurements are also reported. A few hours before the class 3 flare of September 28, two short counting rate increases were observed and are interpreted as electron bursts. The anisotropy of the medium- and low-energy solar protons early in the event and their intensity throughout the event are described. It is found that the history of the intensity of the solar protons is consistent, once isotropy is established, with their having diffused through interplanetary space with an effective mean free path of 0.04 AU. This result is discussed and is shown to be not obviously in disagreement with the generally accepted views regarding the configuration of the interplanetary magnetic field. An estimate of the distance from the sun at which diffusion becomes unimportant and particles escape gives 2 to 3 AU. It is pointed out that simple diffusion (where the particles are scattered from discrete scattering centers and the influence of a general magnetic field is negligible) does not account for the behavior of the anisotropy before isotropy is reached. Two days after the flare, and beginning just before the sudden commencement of a magnetic storm, there was a large increase in the intensity of protons between 2 and 15 Mev, the lower energy limit being determined by the sensitivity of the detectors. As most of these particles, which we have called ‘energetic storm particles,’ arrived after the sudden commencement occurred, we suggest that they were solar protons trapped within the plasma cloud which caused the magnetic storm. The outline of a possible trapping mechanism is given. Explorer 12 measurements of the Forbush decrease of September 30, 1961, are compared with neutron monitor measurements at Deep River. The decrease is larger at Explorer 12 by a factor of 1.7±0.3.

Explorer 12 Observations of Solar Cosmic Rays and Energetic Storm Particles after the Solar Flare of September 28, 1961

Four solar proton events observed by Explorers XII and XIV indicate that propagation of particles is velocity dependent process

/pdf/studies-of-solar-protons-with-explorers-xii-and-xiv-5cuzab8w5w.pdf

Studies of solar protons with explorers xii and xiv

Continual Acceleration of Solar Protons in the MeV Range

Explorer XII measurements of the intensity of interplanetary protons of energy greater than 3 Mev are discussed as possible evidence for long-lived solar streams in interplanetary space. The intensity variations of the protons are related to several solar and geophysical disturbances. (C.E.S.)

/pdf/new-evidence-for-long-lived-solar-streams-in-interplanetary-uad9f98wjr.pdf

New Evidence for Long-Lived Solar Streams in Interplanetary Space

Explorer 12 observations of solar cosmic rays and energetic storm particles following solar flare activity

U. D. Desai

Papers

Explorer 12 Observations of Solar Cosmic Rays and Energetic Storm Particles after the Solar Flare of September 28, 1961

Studies of solar protons with explorers xii and xiv

Continual Acceleration of Solar Protons in the MeV Range

New Evidence for Long-Lived Solar Streams in Interplanetary Space

Explorer 12 observations of solar cosmic rays and energetic storm particles following the solar flare of 28 September 1961