Other
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21d..07g&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SH21D-07
Other
2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
Velocity distributions, f(v), of the suprathermal electrons that carry the solar wind electron heat flux usually consist of a dominant field-aligned component directed outward from the Sun, known as the strahl, and a much weaker and more isotropic halo component. However, other types of distributions, such as counterstreaming strahls, depletions and enhancements of f(v) centered on a pitch angle of 90 deg., and sunward streaming conics, are not uncommon. Moreover, the strahl angular width and intensity are highly variable, often on a time scale of minutes, and the halo intensity also varies widely. Temporal variations in suprathermal electrons typically are most dramatic in the vicinity of the heliospheric current sheet, where the strahl often is bursty and where the strahl and/or halo frequently virtually disappear for hours at a time, but substantial variability can occur anywhere in the wind. During the energetic solar electron events that produce type III radio bursts the strahl is often considerably enhanced and broadened at energies above ~200 eV. This paper provides an overview of (1) suprathermal electron variability in the solar wind at energies less than 1.4 keV as well as (2) some of the physical processes and phenomena that produce this variability.
No associations
LandOfFree
Suprathermal Electron Variability in the Solar Wind at Energies Below 1.4 keV does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Suprathermal Electron Variability in the Solar Wind at Energies Below 1.4 keV, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Suprathermal Electron Variability in the Solar Wind at Energies Below 1.4 keV will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1723236