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Title: NUMERICAL SIMULATION OF ENERGETIC ELECTRONS IN THE INNER MAGNETOSPHERE DURING THE OCTOBER 2001 STORM

Authors:
 [1];  [2]
  1. Los Alamos National Laboratory
  2. NON LANL
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE
OSTI Identifier:
1321611
Report Number(s):
LA-UR-07-2465
DOE Contract Number:
AC52-06NA25396
Resource Type:
Conference
Resource Relation:
Conference: INTERNATIONAL CONFERENCE HELD IN RIKKYO UNIVERSITY ; 200611 ; JAPAN
Country of Publication:
United States
Language:
English

Citation Formats

JORDANOVA, VANIA K., and MIYOSHI, YOSHIZUMI. NUMERICAL SIMULATION OF ENERGETIC ELECTRONS IN THE INNER MAGNETOSPHERE DURING THE OCTOBER 2001 STORM. United States: N. p., 2007. Web.
JORDANOVA, VANIA K., & MIYOSHI, YOSHIZUMI. NUMERICAL SIMULATION OF ENERGETIC ELECTRONS IN THE INNER MAGNETOSPHERE DURING THE OCTOBER 2001 STORM. United States.
JORDANOVA, VANIA K., and MIYOSHI, YOSHIZUMI. Fri . "NUMERICAL SIMULATION OF ENERGETIC ELECTRONS IN THE INNER MAGNETOSPHERE DURING THE OCTOBER 2001 STORM". United States. doi:. https://www.osti.gov/servlets/purl/1321611.
@article{osti_1321611,
title = {NUMERICAL SIMULATION OF ENERGETIC ELECTRONS IN THE INNER MAGNETOSPHERE DURING THE OCTOBER 2001 STORM},
author = {JORDANOVA, VANIA K. and MIYOSHI, YOSHIZUMI},
abstractNote = {},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = {Fri Apr 13 00:00:00 EDT 2007},
month = {Fri Apr 13 00:00:00 EDT 2007}
}

Conference:
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  • The Van Allen Probe satellites were near apogee in the late evening local time sector during the 1 June 2013 magnetic storm's main phase. About an hour after crossing the ring current's “nose structure” into the plasma sheet, the satellites encountered a quasiperiodic sequence of 0.08–3 keV O + ions. Pitch angle distributions of this population consistently peaked nearly antiparallel to the local magnetic field. We then interpret this population as O + conics originating in the northern ionosphere. The sequences began as fairly steady state conic fluxes with energies in the ~ 80 to 100 eV range. Over aboutmore » a half hour buildup phase, O + energies peaked near 1 keV. During subsequent release phases lasting ~ 20 min, O + energies returned to low-energy starting points. We argue these observations reflect repeated formations and dissolutions of downward, magnetically aligned electric fields (ε||) layers trapping O + conics between mirror points within heating layers below and electrostatic barriers above. Nearly identical variations were observed at the locations of both satellites during 9 of these 13 conic cycles. Phase differences between cycles were observed at both spacecraft during the remaining events. Most “buildup” to “release” phase transitions coincided with AL index minima. But, in situ magnetometer measurements indicate only weak dipolarizations of tail-like magnetic fields. The lack of field-aligned reflected O + and tail-like magnetic fields suggest that both ionospheres may be active. However, Southern Hemisphere origin conics cannot be observed since they would be isotropized and accelerated during neutral sheet crossings.« less
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  • Cyclotron resonance between trapped energetic electrons and VLF waves produces pitch angle scattering which leads to electron precipitation in the inner magnetosphere. Previous experiments have shown that in the drift loss cone at L values from 1.5 to 1.8 energy spectrum of the electrons above 50 keV is often dominated by a single narrow peak. The center energy of this peak varies with L in a manner characteristic of cyclotron resonance between the electrons and monochromatic VLF waves in the vicinity of the geomagnetic equator. The source of the waves is probably VLF communication or navigation transmitters. The authors reportmore » the results of a study of 680 occurrences of these peaks detected by the low altitude polar orbiting satellite S81-1. The present data, from altitudes between 170 and 270 km, show the resonance peaks only in two restricted longitude zones centered at 100E and 300E; this result contrasts with the previous measurements at higher altitudes, which detected peaks over a wide range of longitudes. The majority of nighttime events were near transmitter locations where the cyclotron resonance condition was met by electrons with pitch angles near the edge of the loss cone. Detailed study of the events occurring near 100E reveals a 27-day periodicity in the frequency of occurrence; peaks are most often observed during minima in solar/geomagnetic activity. The peaks observed at nighttime in both longitude zones have a possible seasonal variation, being most frequent when it is wintertime at the site of the VLF transmitters responsible for the precipitation.« less