Results 1 to 10 of about 2,507 (154)
Validation of computed extreme ultraviolet emission spectra during solar flares [PDF]
Earth, Planets and Space, 2021 X-rays and extreme ultraviolet (EUV) emissions from solar flares rapidly change the physical composition of the Earth’s thermosphere and ionosphere, thereby causing space weather phenomena such as communication failures.
Shohei Nishimoto +4 more
doaj +2 more sources
Determination of Differential Emission Measure from Solar Extreme Ultraviolet Images [PDF]
Astrophysical Journal Letters, 2018 Abstract The Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) has been providing high-cadence, high-resolution, full-disk UV-visible/extreme ultraviolet (EUV) images since 2010, with the best time coverage among all the solar missions.
Brian Dennis +2 more
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Asymmetries of solar coronal extreme ultraviolet emission lines [PDF]
Astronomy and Astrophysics, 2010 Astronomy & Astrophysics (accepted), 17 pages, 13 ...
Hardi Peter
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The solar corona above active regions: A comparison of extreme ultraviolet line emission with radio emission [PDF]
Solar Physics, 1967 The observations of extreme ultraviolet (EUV) emission lines of Feix through Fe XVI made by OSO-I have been applied to a study of the solar corona above active regions. Ultraviolet and radio emission are determined for several levels of activity classified according to the type of sunspot group associated with the active region. Both radio emission and
exaly +3 more sources
Extreme-ultraviolet and X-Ray Emission of Turbulent Solar Flare Loops [PDF]
Astrophysical Journal Letters, 2019 Abstract Turbulence has been observed in flare loops and is believed to be crucial for the acceleration of particles and in the emission of X-ray photons in flares, but how the turbulence is produced is still an open question. A scenario proposed by Fang et al.
Chun Xia, Rony Keppens
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Extreme-Ultraviolet Emission from Solar Prominences
Astrophysical Journal, 1972 Spectra and spectroheliograms of prominences have been obtained at wavelengths of 300 to 1400 A from instruments aboard the OSO 4 and OSO 6 spacecraft. Quiescent prominences appear in emission above the limb for all strong lines formed at temperatures below 300,000 K, but not at higher temperatures.
M C E Huber, W H Parkinson, E M Reeves
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Emission lines of H2 in the extreme-ultraviolet solar spectrum
Astrophysical Journal, 1978 A sunspot EUV spectrum covering the wavelength range from 1175 to 1714 A with high spatial and spectral resolution is examined which contains about 200 lines not previously reported in solar spectra. Many of the lines are identified as transitions in the Lyman bands of H2.
G E Brueckner, Jordan C, Brueckner G E
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Extreme ultraviolet emission lines of Ni XII in laboratory and solar spectra [PDF]
Monthly Notices of the Royal Astronomical Society, 2000 Wavelengths for emission lines arising from 3s23p5-3s3p6 and 3s23p5-3s23p43d transitions in Ni XII have been measured in extreme ultraviolet spectra of the Joint European Torus(JET) tokamak. The 3s23p5 2P1/2-3s23p4(3P)3d 2D3/2 line is found to lie at 152.90 ± 0.02 A, a significant improvement over the previous experimental determination of 152.95 ± 0.5
Gert Botha, Keenan F P
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Measurements of extreme-ultraviolet emission-line profiles near the solar limb
Astrophysical Journal, 1978 Line profiles of optically thin extreme-ultraviolet emission lines observed in a quiet sun region at positions within and above the white-light limb with the NRL slit spectrograph (S082-B) on Skylab are discussed. Absolute line intensities and full widths at half-maximum are presented for lines formed over the temperature range from about 10,000 to 22 ...
J T Mariska, Doschek G A, Feldman U
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Modeling solar extreme ultraviolet irradiance variability using emission measure distributions
Geophysical Research Letters, 1996 We introduce a new model of solar irradiance variability at extreme ultraviolet (EUV) wavelengths. The model combines a spectral emission line database, solar emission measure distributions, and estimates from ground‐based solar images of the fraction of the Sun covered by the various types of activity to synthesize the irradiance.
H. P. Warren +4 more
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