Differences between transmitter precipitation peaks and storm injection peaks in low-altitude energetic electron spectra

2006 ◽  
Vol 111 (A12) ◽  
Author(s):  
Dayton Datlowe
Keyword(s):  
Energetic Electron ◽  
Electron Spectra ◽  
Low Altitude

scholarly journals Strong localized variations of the low-altitude energetic electron fluxes in the evening sector near the plasmapause

1998 ◽  
Vol 16 (1) ◽  
pp. 25-33 ◽  
Author(s):  
E. E. Titova ◽  
T. A. Yahnina ◽  
A. G. Yahnin ◽  
B. B. Gvozdevsky ◽  
A. A. Lyubchich ◽  
...  
Keyword(s):  
Sharp Increase ◽  
Electron Flux ◽  
Particle Interaction ◽  
Energetic Electron ◽  
Recovery Phase ◽  
Electron Precipitation ◽  
Statistical Characteristics ◽  
Evening Sector ◽  
Proton Precipitation ◽  
Low Altitude

Abstract. Specific type of energetic electron precipitation accompanied by a sharp increase in trapped energetic electron flux are found in the data obtained from low-altitude NOAA satellites. These strongly localized variations of the trapped and precipitated energetic electron flux have been observed in the evening sector near the plasmapause during recovery phase of magnetic storms. Statistical characteristics of these structures as well as the results of comparison with proton precipitation are described. We demonstrate the spatial coincidence of localized electron precipitation with cold plasma gradient and whistler wave intensification measured on board the DE-1 and Aureol-3 satellites. A simultaneous localized sharp increase in both trapped and precipitating electron flux could be a result of significant pitch-angle isotropization of drifting electrons due to their interaction via cyclotron instability with the region of sharp increase in background plasma density.Key words. Ionosphere (particle precipitation; wave-particle interaction) Magnetospheric Physics (plasmasphere)

Geant4 Modeling of the EPI-Hi Instrument on Parker Solar Probe to Calculate Solar Energetic Electron Spectra

2021 ◽  
Author(s):  
Allan Labrador ◽  
Grant Mitchell ◽  
Eric Christian ◽  
Christina Cohen ◽  
Alan C. Cummings ◽  
...  
Keyword(s):  
Energetic Electron ◽  
Electron Spectra

Energetic electron spectra in the radiation belts

1966 ◽  
Vol 71 (9) ◽  
pp. 2217-2226 ◽  
Author(s):  
J. D. Mihalov ◽  
R. Stephen White
Keyword(s):  
Energetic Electron ◽  
Radiation Belts ◽  
Electron Spectra

scholarly journals Low altitude energetic electron lifetimes after enhanced magnetic activity as deduced from SAC-C and DEMETER data

2010 ◽  
Vol 28 (3) ◽  
pp. 849-859 ◽  
Author(s):  
S. Benck ◽  
L. Mazzino ◽  
M. Cyamukungu ◽  
J. Cabrera ◽  
V. Pierrard
Keyword(s):  
Pitch Angle ◽  
Energetic Electron ◽  
Magnetic Activity ◽  
Decay Rates ◽  
Data Sets ◽  
Quiet Time ◽  
Loss Cone ◽  
Energetic Electrons ◽  
Low Altitude ◽  
The Difference

Abstract. When flux enhancements of energetic electrons are produced as a consequence of geomagnetic storm occurrence, they tend to vanish gradually when the magnetic activity calms down and the fluxes decay to quiet-time levels. We use SAC-C and DEMETER low altitude observations to estimate the energetic electron lifetimes (E=0.16–1.4 MeV, L=1.6–5, B=0.22–0.46 G) and compare the decay rates to those observed at high altitude. While crossing the radiation belts at high latitude, the SAC-C and DEMETER instruments sample particles with small equatorial pitch angles (αeq<18° for L>2.5) whereas the comparison is done with other satellite data measured mainly in the equatorial plane (for αeq>75°). While in the inner belt and in the slot region no significant lifetime differences are observed from the data sets with different αeq, in the outer belt, for the least energetic electrons (<500 keV), the lifetimes are up to ~3 times larger for the electrons with the equatorial pitch-angle close to the loss cone than for those mirroring near the equator. The difference decreases with increasing energy and vanishes for energies of about 1 MeV.

Energetic electron spectra in Saturn's plasma sheet

2011 ◽  
Vol 116 (A7) ◽  
pp. n/a-n/a ◽  
Author(s):  
J. F. Carbary ◽  
C. Paranicas ◽  
D. G. Mitchell ◽  
S. M. Krimigis ◽  
N. Krupp
Keyword(s):  
Plasma Sheet ◽  
Energetic Electron ◽  
Electron Spectra

scholarly journals Statistical Results for Solar Energetic Electron Spectra Observed over 12 yr with STEREO/SEPT

2020 ◽  
Vol 889 (2) ◽  
pp. 143 ◽  
Author(s):  
Nina Dresing ◽  
Frederic Effenberger ◽  
Raúl Gómez-Herrero ◽  
Bernd Heber ◽  
Andreas Klassen ◽  
...  
Keyword(s):  
Energetic Electron ◽  
Electron Spectra ◽  
Statistical Results

The Detection and Consequences of Coherent Electromagnetic Plasma Waves: Prediction of Rapid L = 2-3 Electron Slot Formation

2020 ◽  
Author(s):  
Bruce Tsurutani ◽  
Sang A Park ◽  
Jolene Pickett ◽  
Gurbax Lakhina ◽  
Abhijit Sen
Keyword(s):  
Energetic Electron ◽  
Low Frequency ◽  
Plasma Waves ◽  
Entry Points ◽  
Ram Pressure ◽  
Low Altitude ◽  
Dominant Characteristic ◽  
Gradient Drift ◽  
The Waves ◽  
Elliptically Polarized

&lt;p&gt;Low frequency (LF) ~22 Hz to 200 Hz plasmaspheric hiss was studied using a year of Polar&lt;br&gt;plasma wave data occurring during solar cycle minimum. The waves are found to be most intense in the noon and early dusk sectors. When only the most intense LF (ILF) hiss was examined, they are found to be substorm dependent and most prominent in the noon sector. The noon sector ILF waves were also determined to be independent of solar wind ram pressure. The ILF hiss intensity is independent of magnetic latitude. ILF hiss is found to be highly coherent in nature. ILF hiss propagates at all angles relative to&lt;br&gt;the ambient magnetic field. Circular, elliptical, and linear/highly elliptically polarized hiss have been detected, with elliptical polarization the dominant characteristic. A case of linear polarized ILF hiss that occurred deep in the plasmasphere during geomagnetic quiet was noted. The waveforms and polarizations of ILF hiss are similar to those of intense high frequency hiss. We propose the hypothesis that ~10&amp;#8211;100 keV substorm injected electrons gradient drift to dayside minimum B pockets close to the magnetopause to generate LF chorus. The closeness of this chorus to low altitude entry points into the plasmasphere will minimize wave damping and allow intense noon&amp;#8208;sector ILF hiss. The coherency of ILF hiss leads the authors to predict energetic electron precipitation into the midlatitude ionosphere and the electron slot formation during substorms. Several means of testing the above hypotheses are discussed.&lt;br&gt;&amp;#160;&lt;br&gt;References&lt;br&gt;[1] Tsurutani, B.T., S.A. Park, B.J. Falkowski, J. Bortnik, G.S. Lakhina, A. Sen, J.S. Pickett, R. Hajra, M. Parrot, and P. Henri (2020), Low frequency (f &lt; 200 Hz) Polar plasmasheric hiss: Coherent and intense, J. Geophys. Res. Spa. Phys., in press.&amp;#160;&lt;/p&gt;

Solar Flare Energetic Neutral Emission Measurements in the Project Coronas-I

1994 ◽  
Vol 144 ◽  
pp. 635-639
Author(s):  
J. Baláž ◽  
A. V. Dmitriev ◽  
M. A. Kovalevskaya ◽  
K. Kudela ◽  
S. N. Kuznetsov ◽  
...  
Keyword(s):  
Solar Flare ◽  
Energy Range ◽  
Gamma Rays ◽  
Pulse Shape ◽  
Gamma Ray ◽  
Pulse Shape Discrimination ◽  
Shape Discrimination ◽  
Solar Neutron ◽  
Low Altitude

AbstractThe experiment SONG (SOlar Neutron and Gamma rays) for the low altitude satellite CORONAS-I is described. The instrument is capable to provide gamma-ray line and continuum detection in the energy range 0.1 – 100 MeV as well as detection of neutrons with energies above 30 MeV. As a by-product, the electrons in the range 11 – 108 MeV will be measured too. The pulse shape discrimination technique (PSD) is used.

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