Physics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh42a..04h&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH42A-04
Physics
7514 Energetic Particles (2114), 7519 Flares, 7534 Radio Emissions, 2114 Energetic Particles (7514)
Scientific paper
We derive the speed along the interplanetary field of the leading edge and peak flux density of interplanetary type-III fast-drift radio bursts associated with 171 near-relativistic beam-like electron events observed at 1 AU from 1997 to 2004. The speeds of the leading edge and peak of the type III bursts are established by a best fit to time-frequency points obtained from multiple frequency cuts of the WIND/WAVES spectrograms (courtesy of M. J. Kaiser). These are the points when the flux density first rises above the pre-event level or reaches the maximum flux density, respectively. The peak flux speeds are usually <0.1c with a median of 0.065c (electron excitation energy of 6 keV). While the speeds assigned to the leading edge can sometimes exceed 0.3c, their median speed is 0.15c (electron excitation energy of 6 keV). Consistently, the near-relativistic electrons are injected after the start of the decameter type III burst, with a median delay ~10 minutes. Consequently, the near-relativistic electrons measured at 1AU by ACE/EPAM cannot be the high-energy tail of the electron population generating the type III bursts. Because the near-relativistic electrons exhibit beam-like anisotropies (implying nearly scatter-free propagation from the Sun to 1 AU), they must be injected differently than are the type III electrons, i.e., they are a separate electron population. Furthermore, we compare the speeds of the leading edge of the type-III bursts with the injection delays of the near-relativistic electrons. We find no statistically significant correlation and interpret this as further evidence for a lack of meaningful association between the low-energy electrons in the type-III leading edge en route to 1 AU and the population of near-relativistic beam-like electrons observed at Earth.
Haggerty Dennis K.
Roelof Edmond C.
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