Results 251 to 260 of about 34,279 (294)

Magnetic star-planet interaction in the young exoplanet system DS Tucanae Ab

Santos Ld, Owen J, Duvvuri G, Loyd ROP, Vidotto A, Presa A, Bourrier V, King G, Airapetian V, Ehrenreich D, France K, Lendl M, Lothringer J, Nielsen L.   +13 more
europepmc   +1 more source

A new optical flare in the OJ287 blazar

, 2016
Zoła, Stanisław, Dębski, Bartłomiej, Goyal, Arti, Valtonen, M., Ciprini, S., Ogłoza, W., Drożdż, M., Sadakane, K., Matsumoto, K., Kagitani, M., Okano, S., Sakanoi, T., Gazeas, K., Jermak, H., Steele, I. A., Dalessio, J., Provencal, J., Reichart, D. E., Moore, J. P., LaCluyze, A. P., Ivarsen, K. M., Erdem, A., Alicavus, F., Caton, D. B., Keel, W. C., Kidger, M., Naves, R., Montse, Campas, Siwak, Michał   +28 more
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Optical observations of solar flares

Space Science Reviews, 1966
This 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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Flare and Optical Transfer Function

Applied Optics, 1968
The optical image quality is influenced by aberrations, by diffraction, and by other factors, such as flare or stray light originating from the badly polished surfaces of lenses, from the edges of the mount, from striations and bubbles in the glass, and from unwanted double reflections.
K, Rosenhauer, K, Rosenbruch
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Optically thick line widths in pyrotechnic flares

Journal of Quantitative Spectroscopy and Radiative Transfer, 1975
Experimentally 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, 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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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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