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The "FIP Effect" and the Origins of Solar Energetic Particles and of the Solar Wind View all abstracts by submitter

Donald V Reames   Submitted: 2018-01-19 11:43

We find that the element abundances in solar energetic particles (SEPs) and in the slow solar wind (SSW), relative to those in the photosphere, show different patterns as a function of the first ionization potential (FIP) of the elements. Generally, the SEP and SSW abundances reflect abundance samples of the solar corona, where low-FIP elements, ionized in the photosphere, are more efficiently conveyed upward to the corona than high-FIP elements that are initially neutral atoms. Abundances of the elements, especially C, P, and S show a crossover from low to high FIP at ~10 eV in the SEPs but ~14 eV for the solar wind, suggesting that cooler photospheric plasma, perhaps from cool sunspots beneath active regions, supply the coronal source material that eventually will be shock-accelerated as SEPs, while the source of the SSW may lie at the base of diverging open-field lines surrounding but outside active regions. Meanwhile, energetic particles accelerated from the solar wind itself by shock waves at corotating interaction regions (CIRs), generally beyond 1 AU, confirm the FIP pattern of the solar wind.

Authors: Donald V. Reames
Projects: None

Publication Status: submitted to Solar Phys.
Last Modified: 2018-01-23 11:53
Go to main E-Print page  Observations of Electron-driven Evaporation during a Flare Precursor  Sun-to-Earth MHD Simulation of the 14 July 2000   Edit Entry  Download Preprint  Delete Entry 

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