In-situ probes for ionospheric investigations

Sayers, Jentery

doi:10.1016/0021-9169(70)90214-x

Cited by 20 publications

(5 citation statements)

References 57 publications

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“…The first attempts at direct in situ measurements of the ionospheric electron temperature (for a review of in situ techniques, see Sayers [1970] sure the physical parameters (e.g., electron density and electron and ion temperature) was demonstrated in the late 1950's [Bowles, 1958], and reliable results started to become available a few years later [Evans, 1962]. The electron temperatures measured by this radar method provided independent support for the Langmuir probe and retarding potential analyzer measurements of high electron temperatures, thus prompting intensive theoretical studies to explain the observations (for a history of this early work, see Walker and Spencer [1968]).…”

Section: Early Electron Temperature Measurementsmentioning

confidence: 99%

Electron temperatures in the F region of the ionosphere: Theory and observations

Schunk¹,

Nagy²

1978

Reviews of Geophysics

443

339

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The theory and observations relating to electron temperatures in the F region of the ionosphere are reviewed. The review is divided into three basic parts. In the first part the theory concerning electron heating, cooling, and energy transport processes is reviewed, and all the relevant expressions are updated. In the second part the behavior of F region electron temperatures, as measured by satellites, rockets, and incoherent scatter radars, is discussed. This portion covers electron temperature variations with altitude, latitude, local time, season, geomagnetic activity, and solar cycle. The third part is primarily devoted to a discussion of the various attempts to compare measured and calculated F region electron temperatures.

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Section: Early Electron Temperature Measurementsmentioning

confidence: 99%

Electron temperatures in the F region of the ionosphere: Theory and observations

Schunk¹,

Nagy²

1978

Reviews of Geophysics

443

339

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“…The electron temperature variations in the Earth's ionosphere have been studied extensively through ground-based and in situ observations [Farley et al, 1967;Evans, 1973;Hanson et al, 1973;Oyama and Hirao, 1975;Titheridge, 1976;Brace and Theis, 1978;Oyama et al, 1985Oyama et al, , 1988Suet al, 1995;Watanabe et al, 1995] and through theoretical calculations [Dalgarno et al, 1963;Geisler and Bowhill, 1965;Banks and Nagy, 1970;Mayr et al, 1972;Bailey et al, 1975]. Excellent reviews of the observations and theory have been presented by Sayers [1970], Bauer and Nagy [1975], and Schunk and Nagy [1978].…”

Section: Introductionmentioning

confidence: 99%

Plasmasphere electron temperature studies using satellite observations and a theoretical model

Balan¹,

Oyama²,

Bailey³

et al. 1996

J. Geophys. Res.

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Electron temperature variations in the Earth's plasmasphere are studied using the Exos D satellite observations and the Sheffield University plasmasphere‐ionosphere model. The observations made during the years 1989–1994 are analyzed to investigate the local time and altitude (1000–8000 km) variations of the electron temperature at magnetic latitudes 0°–45°N. The observed electron temperature Te is almost constant during both day and night and is found to have large day‐to‐night differences that vary with altitude and latitude; the largest day‐to‐night ratio in Te (≈6500 K/2600 K) occurs at the highest altitude at equatorial latitudes and the smallest ratio (≈3300 K/2300 K) at the lowest altitude at midlatitudes. During daytime, Te increases rapidly with altitude in the lower plasmasphere (altitude <2500 km) and slowly in the upper plasmasphere with mean gradients of 1.33 and 0.22 K km−1, respectively. At night, on the other hand, the lower plasmasphere is in thermal equilibrium, and in the upper plasmasphere Te increases slowly with a mean gradient equal to the daytime value. The electron temperature shows maximum latitude variation at medium plasmaspheric altitudes (around 4000 km) and smaller variations at lower and higher altitudes, particularly during daytime. At the altitude of maximum latitude variation, Te increases by about 1200 K between the equator and 40°N during both day and night. The model reproduces the observations reasonably well and is used to explain the occurrence of a prominent morning peak in Te. The morning peak becomes prominent in the lower plasmasphere at low latitudes because of the vertical E × B drift in the equatorial F region, which increases Te during morning hours and decreases Te during daytime hours. The observations and model results also show the occurrence of an afternoon peak in Te, which becomes prominent with increasing altitude and latitude; the peak could be caused by the daytime poleward neutral wind.

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“…Reviews on this topic have been published by Florida (1969), Sayers (1970), the Special Issue ofRadio Science for April 1973, Bauer andNagy (1975) Meyer-Vernet andPerche (1989), and (pertaining to the Dynamics Explorer satellite) by Hoffman (1981). In practice, these experiments utilize electrical probes mounted on rocket or satellite payloads.…”

Section: Ionospheric In Situ Measurementsmentioning

confidence: 99%