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The Solar EruptioN Integral Field Spectrograph. [PDF]
Herde VL +19 more
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Solar flare high-energy electron spectra
Solar Physics, 1992It is shown that the solar flare electron spectra in a large energy range fit well with a power law in energy. This is used as a basis to discuss the possible division of solar flares into various groups, and also to compare the spectra of electrons in interplanetary space and at the flare site.
T Amari
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2022
Таврический астрофизический журнал, Выпуск 3 (2) 2022, Pages 17 ...
Kupryakov, Yu.A. +2 more
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Таврический астрофизический журнал, Выпуск 3 (2) 2022, Pages 17 ...
Kupryakov, Yu.A. +2 more
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Cyclotron lines in the spectra of solar flares and solar active regions
Solar Physics, 1989AbstractIt was shown by Zheleznyakov and Zlotnik (1980a, b) that in complex configurations of solar magnetic fields (in hot loops above the active centres, in neutral current sheets in the preflare phase, in hot X-ray kernels in the initial flare phase) a system of cyclotron lines in the spectrum of microwave radiation is likely to be formed.
V. V. Zheleznyakov, E. Ya. Zlotnik
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Spectra of solar flares from 8.5 � to 16 �
Solar Physics, 1973X-ray spectra of solar flares in the spectral range from 8.5 A to ∼ 16 A have been obtained from a Naval Research Laboratory crystal spectrometer flown on the sixth Orbiting Solar Observatory (OSO-6). A list of emission features is presented and tentative identifications of some of the features are suggested.
G. A. Doschek +2 more
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Annual Review of Astronomy and Astrophysics, 1972
Solar flares emit electromagnetic radiation within a very broad range of wavelengths, from 0.02 A (2 X 10-10 cm) up to more than 600 m (6X 104 cm). This may be continuous emission in some parts of the spectrum, line emission in others, or a combination of both.
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Solar flares emit electromagnetic radiation within a very broad range of wavelengths, from 0.02 A (2 X 10-10 cm) up to more than 600 m (6X 104 cm). This may be continuous emission in some parts of the spectrum, line emission in others, or a combination of both.
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Determining the Spatial Variation of Accelerated Electron Spectra in Solar Flares
AIP Conference Proceedings, 2008The RHESSI spacecraft images hard X‐ray emission from solar flares with an angular resolution down to ∼2″ and an energy resolution of 1 keV. For such a Rotating Modulation Collimator (RMC) instrument, imaging information is gathered not as a set of spatial images, but rather as a set of (energy‐dependent) spatial Fourier components (termed visibilities)
A. Gordon Emslie +12 more
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Interpretation of X-ray spectra from solar flares
Advances in Space Research, 1991Abstract A technique developed for analysing the SMM X-ray spectra has been adapted to the interpretation of high resolution cooled germanium flare spectra. It is shown that these can be fitted equally well by simple all thermal or non-thermal distributions, and that the data set is insufficient to determine the non-thermal nature of the flare.
A.H. Gabriel, F. Bely-Dubau, F. Millier
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Connecting solar flare hard X-ray spectra to in situ electron spectra
Aims. We aim to constrain the acceleration, injection, and transport processes of flare-accelerated energetic electrons by comparing their characteristics at the Sun with those injected into interplanetary space. Methods.
Dresing, N. +6 more
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