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The light curve variations in AR Lacertae
Astrophysics and Space Science, 1982The eclipsing binary AR Lac has been observed in two colours,B andV, in 1980 and 1981. The new times of minimal obtained during the observatons indicate that the period of the system is still continuing its decrease. The wave-like distortions outside eclipses have two maxima and are very similar in shape in successive two years.
Ertan A.Y. +5 more
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Light curve analysis of contact binaries: Characteristic quantities of the light curve
Astrophysics and Space Science, 1981Quantities characterizing light curves of contact binaries of W UMa-type are introduced. For 2700 cases, theoretical light curves of contact binaries are computed by the light curve synthesis method, and characteristic quantities for these light curves are tabulated. An example of application of the table to the light curve analysis of contact binaries
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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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Light curve variations in V471 Tauri
Astrophysics and Space Science, 1986The light curves of V471 Tau obtained in four successive years from 1981 to 1984 are presented. The light variations due to the tidally distorted red dwarf have been computed and subtracted out from the light curves obtained so far. A pure shape of the wave-like distortion has therefore been derived.
Evren, S +3 more
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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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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 of RT lacertae
Astrophysics and Space Science, 1980The eclipsing variable RT Lac, which is classified as an RS CVn-type binary by Hall, was observed in two colours,B andV, during the summer seasons of 1978 and 1979. The observations made during two successive seasons indicate that, outside eclipses, the system has brightened by about 0.12 and 0.15 magnitudes on average inB andV, respectively. Moreover,
Ibanoglu C. +5 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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The light saturation curve of photosynthesis
Biochimica et Biophysica Acta (BBA) - Bioenergetics, 1970H A, Herron, D M, Mauzerall
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