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Predicting and Modeling Solar Flare Generated Proton Fluxes in the Inner Heliosphere

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Solar energetic particles are assumed to be accelerated above the solar active regions from the available coronal material. The composition of large solar particle events is consistent with an ion selection process based on the first ionization potential of the elements in the solar corona. The transport of solar protons in interplanetary space is controlled by the topology and characteristics of the interplanetary magnetic field. The topology of the magnetic field lines in interplanetary space is controlled by the flow speed of the ionized plasma and the rotation rate of the sun, resulting in the so called Archimedean spiral configuration. The particle flux longitudinal gradients observed in the inner heliosphere are variable, and local interplanetary conditions and structures greatly influence the time-intensity profiles observed. The most extensive solar particle measurements are those observed by earth-orbiting spacecraft, and forecast and prediction procedures are best for the position of the earth. These earth-based models can be extended to other heliolongitudes or to more distant locations in the inner heliosphere. Solar protons, Solar proton prediction, Interplanetary medium, Solar flare, Heliosphere.

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Journal article

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Availability: Pub. in Biological Effects and Physics of Solar and Galactic Cosmic Radiation, Part B p101-117, 1993. Available only to DTIC users. No copies furnished by NTIS.



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Approved for public release; distribution is unlimited. Document partially illegible.

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