Results 231 to 240 of about 2,620 (256)

An example of radio and optical homologous flares

Solar Physics, 1970
Fokker (1967) has raised the question of whether the optical and radio homologies of flares are correlated. Two 2b flares occurring nearly 54 h apart (July 9 and 12, 1968) were observed at 29 wavelengths from Hα+4.00 A to Hα−4.26 A and at 10-cm radio. Adjacent pictures were spaced 0.295 A and 2 sec apart.
K. P. White, T. J. Janssens
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On the ionisation of hydrogen in optical flares

Solar Physics, 1973
Non-steady state and non-LTE effects on the ionisation equilibrium of hydrogen in optical flares are considered in terms of a two-level hydrogen atom. It is shown that, just as in the quiet low chromosphere, the ionisation equation is controlled by spontaneous recombination to the second level and by photoionisation from this level by photospheric ...
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Flare modeling and calculation on EUV optics

SPIE Proceedings, 2010
Flare 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, T. Oshino, K. Murakami, H. Chiba   +3 more
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On the origin of the flare optical continuum

Solar Physics, 1976
We show that the bluish-white emission knots, observed in white-light flares, can be due to the existence of a quite large amount of material at a temperature T e ≈2×104 K in the Lyman-α forming region.
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Optical Solar Flares

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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The optical continuum of solar and stellar flares

Solar Physics, 1981
A further development of the Kostyuk-Pikelner's model is presented. The response of the chromosphere heated by non-thermal electrons of the power-law energy spectrum has been studied on the basis of the numerical solution of the one-dimensional time-dependent equations of gravitational gas dynamics.
M. A. Livshits, O. G. Badalyan, A. G. Kosovichev, M. M. Katsova   +3 more
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Optical observations of flare stars in the galaxy

Astrophysics, 1995
Observations of flare stars in the galaxy are considered. UV Ceti type stars in the solar vicinity and flare stars is star clusters and associations have almost the same properties. The differences between them are connected with the age. Flare stars are one of the richest populations in the galaxy. The evolutionary path for all flare stars is the same.
L. V. Mirzoyan, V. V. Hambarian, A. T. Garibjanian, A. L. Mirzoyan   +3 more
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Flare-Associated Optical Phenomena

1976
Besides 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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A flare in the optical spectrum of 3C 273

Publications of the Astronomical Society of the Pacific, 1985
Flaring has been observed in 3C 273 in the BVRI spectrum during January 1983. The increase in luminosity is especially pronounced at longer wavelengths and amounts to as much as half a magnitude increase in brightness over quiescent values. These observations complement and are consistent with similar observations in the millimeter to IR made at about ...
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Energetic solar particles and their relation to optical flares

Solar Physics, 1973
It has been recently suggested by several investigators that the accelerated charged particles provide the energy of the optical flare by the ionization loss process. We have examined this mechanism assuming different forms of the spectrum of the accelerated protons at lower chromosphere.
S. Biswas, B. Radhakrishnan
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