Measurements of the ambient photoelectron spectrum from atmosphere explorer: II. AE-E measurements from 300 to 1000 km during solar minimum conditions

Lee, J.S.; Doering, J. P.; Potemra, T. A.; Brace, L. H.

doi:10.1016/0032-0633(80)90059-8

Cited by 52 publications

(31 citation statements)

References 15 publications

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“…It has been well recognized that particle observations in this energy range are essential for the understanding of the ionospheric and magnetospheric physics, and extensive measurements have been made (e.g., MENG, 1978;Voss and SMITH, 1980;LEE et al, 1980aLEE et al, , 1980b. Most of the data obtained by the EXOS-C satellite are generally consistent with those obtained hitherto by others, but some peculiar phenomena have also been found out.…”

supporting

confidence: 77%

“…For example, a peak can be seen at the energy of 27eV in the first LEE et al (1980b) also have found that both the flux and spectral structure of photoelectrons in the energy range of 20 to 30eV are extremely variable at altitudes higher than 300km and have a good correlation with the density of the ambient plasma. Unfortunately we have not obtained the electron density data in this particular orbit.…”

Section: (C)mentioning

confidence: 96%

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Initial observation of low-energy charged particles by satellite OHZORA (EXOS-C)

Mukai

Kaya

Kubo

et al. 1985

J. geomagn. geoelec

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The low-energy particle experiment (ESP) on the EXOS-C satellite was designed to measure the energy spectrum and the pitch-angle distribution of electrons over the energy range of 6 eV to 16 keV and positive ions from 200 eV to 16 keV. The experiment has been successful and it has revealed global characteristics of ionospheric photoelectrons and magnetospheric energetic particles over a wide range of latitude, longitude, altitude (350-850km) and local time. The precipitation of auroral particles is observed at latitudes higher than the trapping boundary of higher-energy particles. The electron precipitation pattern is diffuse in the dayside auroral region, whereas it is quite discrete on the nightside. The energy spectrum of ions precipitating into the auroral region is found to be generally harder than the corresponding electrons. Energetic electrons with energies of 10-100keV have also been detected at dusk hours near the equator. The nature of these electrons is not yet known. The energy spectrum of photoelectrons is found to have a peak in an energy range from 20 to 30eV and a sharp cutoff near 60eV. However, the spectral shape in the energy range of 20 to 30eV is found to vary significantly depending on latitude, longitude and local time. A large peak at 20-30eV is observed occasionally over the region of the South-Atlantic geomagnetic anomaly.

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supporting

confidence: 77%

Section: (C)mentioning

confidence: 96%

Initial observation of low-energy charged particles by satellite OHZORA (EXOS-C)

Mukai

Kaya

Kubo

et al. 1985

J. geomagn. geoelec

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“…In this calculation, initial distributions for the kinetic part of the model are applied at the lower boundary, and are associated with the upper half of the Maxwellian distribution. The ions are initially distributed with the Maxwellian energy spread ( Ã ) being 0.3 eV for H and 0.6 eV for O , while the photoelectrons are of 21.6 eV energy spread, with energy ranging from 2 to 62 eV (based on the photoelectron spectra measured by Lee et al (1980)). Note that we use``energy spread'' instead of the more popular term``temperature'' to describe the initial distribution functions, because as will be discussed below, such``temperatures'' will be dierent from their corresponding values in the ®nal result.…”

Section: Theory Data Closurementioning

confidence: 99%

Further development in theory/data closure of the photoelectron-driven polar wind and day-night transition of the outflow

1998

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Abstract. Recent in situ observations have revealed novel features in the polar wind. Measurements between 5000 and 9000 km altitude by the Akebono satellite indicate that both H and O ions can have remarkably higher out¯ow velocities in the sunlit region than on the nightside. Electrons also display an asymmetric behavior: the dayside dierence in energy spread, greater for upward-moving than downward-moving electrons, is absent on the nightside. Here, we discuss the further development of a theory by Tam et al. that can explain most of these observed peculiar properties by properly taking into account the global, kinetic, collisional eects of the sunlit photoelectrons, on the background polar wind and the electric ®eld. Quantitative comparisons of the calculated results with actual data will be described. In addition, transition from the daytime photoelectrondriven polar wind to the night-time polar wind will be discussed.

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“…Photoelectrons give a measure of the coupling between the northern and southern hemispheres. Lee et al (1980) have postulated that such decreases might be due to enhancements in the thermal electrons within the local flux tube. This shielding phenomena has been noted in many of the SAR -arc cases (both visual and subvisual) we have investigated.…”

Section: B Discussionmentioning

confidence: 99%

Magnetospheric Plasma Studies Using Data from the Dynamics High and Low Altitude Plasma Instruments.

Barfield¹

1983

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Measurements of the ambient photoelectron spectrum from atmosphere explorer: II. AE-E measurements from 300 to 1000 km during solar minimum conditions

Cited by 52 publications

References 15 publications

Initial observation of low-energy charged particles by satellite OHZORA (EXOS-C)

Initial observation of low-energy charged particles by satellite OHZORA (EXOS-C)

Further development in theory/data closure of the photoelectron-driven polar wind and day-night transition of the outflow

Magnetospheric Plasma Studies Using Data from the Dynamics High and Low Altitude Plasma Instruments.

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