Doppler-Shifted Auroral Hydrogen Emission.

Meinel, A. B.

doi:10.1086/145375

Cited by 137 publications

(33 citation statements)

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“…Gartlein (1951) confirmed the observation and interpretation with detection of the H α , H β , and H γ lines. With greater resolution Meinel (1951) obtained spectra that clearly showed that precipitating protons of very high velocity are responsible for an extended short wavelength tail in the line profile. Eather and Jacka (1966) made measurements in the magnetic zenith and the magnetic horizon directions, noting that the H β line was broadened in both directions and that the zenith profile was shifted, in addition, toward shorter wavelengths.…”

Section: Ground-based Observations Of Auroral Hydrogen Linesmentioning

confidence: 99%

High resolution measurements and modeling of auroral hydrogen emission line profiles

et al. 2003

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Abstract. Measurements in the visible wavelength range at high spectral resolution (1.3Å) have been made at Longyearbyen, Svalbard (15.8 E,78.2 N) during an interval of intense proton precipitation. The shape and Doppler shift of hydrogen Balmer beta line profiles have been compared with model line profiles, using as input ion energy spectra from almost coincident passes of the FAST and DMSP spacecraft. The comparison shows that the simulation contains the important physical processes that produce the profiles, and confirms that measured changes in the shape and peak wavelength of the hydrogen profiles are the result of changing energy input. This combination of high resolution measurements with modeling provides a method of estimating the incoming energy and changes in flux of precipitating protons over Svalbard, for given energy and pitch-angle distributions. Whereas for electron precipitation, information on the incident particles is derived from brightness and brightness ratios which require at least two spectral windows, for proton precipitation the Doppler profile of resulting hydrogen emission is directly related to the energy and energy flux of the incident energetic protons and can be used to gather information about the source region. As well as the expected Doppler shift to shorter wavelengths, the measured profiles have a significant red-shifted component, the result of upward flowing emitting hydrogen atoms.

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Section: Ground-based Observations Of Auroral Hydrogen Linesmentioning

confidence: 99%

High resolution measurements and modeling of auroral hydrogen emission line profiles

et al. 2003

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“…It also provided the first evidence that aurorae were caused by particle precipitation. The presence of proton precipitation was later confirmed with higher spectral resolution of H emission measurements by Meinel (1951). Review papers on proton aurora include those by Eather (1967), McNeal andBirely (1973), Eather (1988), and Rees (1989).…”

Section: Introductionmentioning

confidence: 88%

Proton aurora observed from the ground

Galand

Chakrabarti

2006

Journal of Atmospheric and Solar-Terrestrial Physics

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“…A final concern about the existence of significant particle beams in solar flares comes from the absence of the effect described by Orrall and Zirker (1976). As originally proposed, this theory noted that a downward proton beam would produce an enhanced red wing on the Lyα line via charge exchange, analogous to the presence of Doppler-shifted Hα in the proton aurora (Meinel, 1951). This theory has never been tested well, but we have recently used EUV observations of the He II 304 Å line to look for the analogous effect resulting from primary α-particles , known from γ -ray observations to be present (Kozlovsky and Ramaty, 1974;Share and Murphy, 1997) in solar flares.…”

Section: To Beam or Not To Beam?mentioning

confidence: 99%

Chasing White-Light Flares

Hudson

2016

Sol Phys

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In this memoir I describe my life in research, mostly in the area of solar physics. The recurring theme is "white-light flares," and several sections of this paper deal with this and related phenomena; I wind up describing how I see the state of the art in this stillinteresting and crucially important (as it has been since 1859) area of flare research. I also describe my participation in two long-lived satellite programs dedicated to solar observations (Yohkoh and RHESSI) and elaborate on their discoveries. These have both helped with white-light flares both directly and also with closely related X-ray and γ -ray emissions), with the result that this article leans heavily in that direction.

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Doppler-Shifted Auroral Hydrogen Emission.

Cited by 137 publications

References 0 publications

High resolution measurements and modeling of auroral hydrogen emission line profiles

High resolution measurements and modeling of auroral hydrogen emission line profiles

Proton aurora observed from the ground

Chasing White-Light Flares

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