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Nature, 1960
THE luminosity equation for the trail of a meteor is: where I is the luminous intensity at any point of the trail, is the rate of ablation of the meteoroid at that point, ν is the velocity of the meteoroid ...
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THE luminosity equation for the trail of a meteor is: where I is the luminous intensity at any point of the trail, is the rate of ablation of the meteoroid at that point, ν is the velocity of the meteoroid ...
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Reanalysis of the light curve of ES lib
Astronomische Nachrichten, 1981AbstractUsing Wood's (1972) model we have reanalyzed Bartolini et al.'s (1973) photoelectric light curve – as yet only crudely studied – of the single‐lined eclipsing binary ES Lib. Our photometric elements considerably differ from the previous ones.
GIURICIN G. +2 more
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The distortions in the light curves of MM herculis
Astrophysics and Space Science, 1987The RS CVn-type eclipsing binary MM Her was observed photoelectrically inB andV colours. The light curves obtained in 1984 and 1985 are presented. It was found that the depths of the primary minima are decreased from 1983 to 1985. However, the amplitude of the wave-like distortion outside the eclipses was detected to increase since 1976.
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1990
The supernova phenomenon was discovered because stellar explosions are prodigious sources of optical light. Although we know today that the energy budget for the core collapse of a massive star allocates 99% of the energy released to neutrinos and 1% to kinetic energy, the 10−4 part that becomes light makes super-novae the most luminous stars in the ...
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The supernova phenomenon was discovered because stellar explosions are prodigious sources of optical light. Although we know today that the energy budget for the core collapse of a massive star allocates 99% of the energy released to neutrinos and 1% to kinetic energy, the 10−4 part that becomes light makes super-novae the most luminous stars in the ...
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Light curve variations in ER vulpeculae
Astrophysics and Space Science, 1987Photoelectric observations of the peculiar eclipsing variable ER Vul were obtained in blue and yellow light, in the 1981 and 1982 observing seasons. The light curves suffer to change in short time-intervals. The wave-like distortion superimposed on the light curves is clearly seen, but sometimes there is no indication about its existence. The migration
Ibanoglu, C, Evren, S, Tunca, Z
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2014
In this chapter we use the multi-frequency single dish observations of CTA 102 to study the flaring behavior of the source. For our analysis we focused on the radio flare around April 2006 and used observations spanning from 4.8 to 340 GHz (see Fig. 3.1).
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In this chapter we use the multi-frequency single dish observations of CTA 102 to study the flaring behavior of the source. For our analysis we focused on the radio flare around April 2006 and used observations spanning from 4.8 to 340 GHz (see Fig. 3.1).
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The light curve analysis of MM Herculis
Astrophysics and Space Science, 1987The photoelectric light curves of MM Her obtained in 1983 and 1984 by Evren (1985, 1987) were analyzed by two different methods. Firsly, the effects of the wave-like distortions on the observations were removed from the observed magnitudes by obtaining its mathematical expression. The remaining light curves were analyzed by using Wood's approach. Later,
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The light saturation curve of photosynthesis
Biochimica et Biophysica Acta (BBA) - Bioenergetics, 1970H A, Herron, D M, Mauzerall
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Learning to Enhance Low-Light Image via Zero-Reference Deep Curve Estimation
IEEE Transactions on Pattern Analysis and Machine Intelligence, 2021Chen Change Loy, Chongyi Li
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A survey on machine learning based light curve analysis for variable astronomical sources
Wiley Interdisciplinary Reviews: Data Mining and Knowledge Discovery, 2021Shanjiang Tang, Yihan Tao, Chongke Bi
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