Results 131 to 140 of about 2,393 (171)
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Optically thick line widths in pyrotechnic flares
Journal of Quantitative Spectroscopy and Radiative Transfer, 1975Experimentally determined sodium line widths for pyrotechnic flares are compared with simple analytical, optically-thick-line-shape calculations. Three ambient pressure levels are considered (760, 150 and 30 torr) for three different flare compositions. The measured line widths range from 1.3 to 481 A.
B.E. Douda, R.J. Exton
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Flare modeling and calculation on EUV optics
SPIE Proceedings, 2010Flare is a critical impact on extreme ultraviolet (EUV) lithography. Flare can be calculated by integrating flare point spread function (PSF) within the bright field. Flare PSF is defined as (1-TIS)δ(r)+PSF sc (r); where TIS, total integrated scatter, is traditonally defined as integration of PSF SC to infinity, and r is distance on wafer.
M. Shiraishi +3 more
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1965
We have to distinguish between the optical flare and what we now tend to call the radio or X-ray flare. Initially flares have been described and defined after their optical appearance. We now realize that in doing this, we may have excluded the most important part. In this chapter we restrict ourselves to the optical flares.
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We have to distinguish between the optical flare and what we now tend to call the radio or X-ray flare. Initially flares have been described and defined after their optical appearance. We now realize that in doing this, we may have excluded the most important part. In this chapter we restrict ourselves to the optical flares.
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Optical observations of solar flares
Space Science Reviews, 1966This paper gives a review of the results of optical observations of solar flares. Observations carried out in the Hα line, flare spectra, and the methods of analysing the flare spectra are briefly discussed. Great attention is paid to the continuous emission of flares in the optical spectral region. In the last section, optical aspects of proton flares
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Optical-to-Radio Continua in Solar Flares
Solar Physics, 2011Spectral continua observed during solar flares may contain information about both thermal and non-thermal heating mechanisms. Using two semi-empirical flare models F2 and FLA, we synthesize the thermal continua from optical to mm–radio domains and compare their intensities with quiet-Sun values computed from a recent model C7.
P. Heinzel, E. H. Avrett
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Future optical observations of solar flares
Advances in Space Research, 1988Abstract The fundamental importance of observing the chromospheric and photospheric components of solar flares is stressed. Careful interpretation of several optical flare spectral features enable us to disentangle the various proposed energy transfer mechanisms during the different phases of the flare development.
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Optical behaviour of markarian 421 during high-energy flares
Astronomical & Astrophysical Transactions, 1997Abstract In this paper we present the optical behaviour of Mrk 421 from 1992 to April, 1995. The observations were obtained at the Perugia University Observatory with the automatic imaging telescope in the BVR c I c broad-bands. Visual estimates done by “The Astronomer” group and the British Astronomical Association (BAA) are inclosed in the light ...
M. Fiorucci, TOSTI, Gino, G. M. Hurst
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Flare-Associated Optical Phenomena
1976Besides the optical flare proper a large number of various optical phenomena are observed in the solar chromosphere and corona that obviously are related in some way or the other to the flare event. We may divide them into four different types: (a) Activation of filaments (or prominences when seen on the limb) preceding the optical flare.
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Coronal Loops and Optical Radiation from Flaring Stars
Geomagnetism and Aeronomy, 2020The possibility that large-scale coronal loops of solar-type stars and M dwarfs make a significant contribution to the white-light continuum emission is considered. It is shown that that the existence of high-density (>1012 cm–3) coronal loops contradicts the standard model of solar and stellar flares.
Yu. T. Tsap +4 more
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Optical Emission from Stellar Flares
1996Optical observations of stellar flares on late-type stars are common, particularly in the U and B bands of the Johnson system. The reason for this preference is the large proportionate increase in the flux in the ultraviolet during flares on late-type stars, as compared to the quiescent stellar continuum which peaks in the near infra-red.
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