Electron density and electron flux in a glow aurora

Bryant, D. A.; Courtier, G. M.; Skovli, G.; Lindalen, H.R.; Aarsnes, K.; Mase̊ide, K.

doi:10.1016/0021-9169(70)90175-3

Cited by 20 publications

(3 citation statements)

References 16 publications

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“…In this paper the measurements of the N 2 emissions at 427.8 nm are used. This emission has been found to be a good indicator for the energy¯ux of the precipitating electrons (Bryant et al, 1970;Omholt, 1971). As this is a prompt emission, the N 2 measurements are very suitable for comparison with the X-ray¯uxes that are also produced immediately.…”

Section: The Rocket Experiments and Launch Conditionsmentioning

confidence: 87%

Simultaneous measurements of X-rays and electrons during a pulsating aurora

et al. 1998

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Abstract. The PULSAUR II rocket was launched from Andùya Rocket Range at 23.43 UT on 9 February 1994 into a pulsating aurora. In this paper we focus on the observations of precipitating electrons and auroral X-rays. By using models it is possible to deduce the electron energy spectrum from X-ray measurements. Comparisons are made between the deduced electron uxes and the directly measured electron¯uxes on the rocket. We found the shape of the observed and the deduced electron spectra to ®t very well, with almost identical e-folding energies in the energy range from 10 ke V to $ 60±80 ke V. For the integrated¯uxes from 10.8 to 250 ke V, we found a discrepancy of 30% . By combining two models, we have found a good method of deducing the electron precipitation from X-ray measurements. The discrepancies between calculations and measurements are in the range of the uncertainties in the measurements.

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Section: The Rocket Experiments and Launch Conditionsmentioning

confidence: 87%

Simultaneous measurements of X-rays and electrons during a pulsating aurora

et al. 1998

View full text Add to dashboard Cite

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“…In this paper the measurements of the N 2 emissions at 427.8 nm are used. This emission has been found to be a good indicator for the energy ¯ux of the precipitating electrons (Bryant et al, 1970;Omholt, 1971). As this is a prompt emission, the N 2 measurements are very suitable for comparison with the X-ray ¯uxes that are also produced immediately.…”

Section: The Rocket Experiments and Launch Conditionsmentioning

confidence: 96%

Simultaneous measurements of X-rays and electrons during a pulsating aurora

et al. 1998

View full text Add to dashboard Cite

Abstract. The PULSAUR II rocket was launched from Andøya Rocket Range at 23.43 UT on 9 February 1994 into a pulsating aurora. In this paper we focus on the observations of precipitating electrons and auroral X-rays. By using models it is possible to deduce the electron energy spectrum from X-ray measurements. Comparisons are made between the deduced electron fluxes and the directly measured electron fluxes on the rocket. We found the shape of the observed and the deduced electron spectra to fit very well, with almost identical e-folding energies in the energy range from 10 ke V to ~60–80 ke V. For the integrated fluxes from 10.8 to 250 ke V, we found a discrepancy of 30% . By combining two models, we have found a good method of deducing the electron precipitation from X-ray measurements. The discrepancies between calculations and measurements are in the range of the uncertainties in the measurements.Key words. Ionospheric particle precipitation · Magnetospheric physics · Annual phenomena · Energetic particle

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“…To produce a beam spot that is optically detectable from the ground in the presence of active aurora, a beam power of 5 kW or more needs to be deposited in the atmosphere. Each 1 kW of beam power results in about 1.1 W of 4278 Å emission [Bryant et al, 1970) and about 3 W of 3914 Å emission. The spectral lines emitted by the beam spot will be the same spectral lines as emitted by the electron aurora.…”

Section: Detecting the Beam Spotmentioning

confidence: 99%

A Mission Concept to Determine the Magnetospheric Causes of Aurora

Borovsky

Delzanno

Henderson

2020

Front. Astron. Space Sci.

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Insufficiently accurate magnetic-field-line mapping between the aurora and the equatorial magnetosphere prevents us from determining the cause of many types of aurora. An important example is the longstanding question of how the magnetosphere drives low-latitude (growth-phase) auroral arcs: a large number of diverse generator mechanisms have been hypothesized but equatorial magnetospheric measurements cannot be unambiguously connected to arcs in the ionosphere, preventing the community from identifying the correct generator mechanisms. Here a mission concept is described to solve the magnetic-connection problem. From an equatorial instrumented spacecraft, a powerful energetic-electron beam is fired into the atmospheric loss cone resulting in an optical beam spot in the upper atmosphere that can be optically imaged from the ground, putting the magnetic connection of the equatorial spacecraft’s measurements into the context of the aurora. Multiple technical challenges that must be overcome for this mission concept are discussed: these include spacecraft charging, beam dynamics, beam stability, detection of the beam spot in the presence of aurora, and the safety of nearby spacecraft.

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Electron density and electron flux in a glow aurora

Cited by 20 publications

References 16 publications

Simultaneous measurements of X-rays and electrons during a pulsating aurora

Simultaneous measurements of X-rays and electrons during a pulsating aurora

Simultaneous measurements of X-rays and electrons during a pulsating aurora

A Mission Concept to Determine the Magnetospheric Causes of Aurora

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