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Solar eclipse
About: Solar eclipse is a research topic. Over the lifetime, 2737 publications have been published within this topic receiving 22625 citations.
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TL;DR: In this article, the amplitude of time variations N was 2 × 109−4 × 1010 m−3, and the relative amplitude was 0.10−0.15, for the day of a partial solar eclipse and for a background day.
Abstract: Quasi-periodic variations in the power of incoherent scattered signals, caused by wave disturbances of the electron concentration in the ionosphere, are analyzed for the day of a partial solar eclipse and for a background day. The windowed and adaptive Fourier transforms and the wavelet transform are used for spectral analysis. The spectral parameters of the wave disturbances at altitudes of 100–500 km in the 10–120 min period range differed significantly on the day of the solar eclipse and on the background day. Variations in the spectrum began near the onset of the phase of maximum disk occultation and continued no less than 2 h. The amplitude of time variations N was 2 × 109–4 × 1010 m−3, and the relative amplitude was 0.10–0.15. Wave disturbances have been compared for five solar eclipses; the comparison shows a noticeable variation in the spectrum of the wave disturbances during these events.
18 citations
TL;DR: In this paper, the polarization distribution in the sky during a total solar eclipse is calculated with a simple secondary light-scattering model using the light intensity measurements near the horizon during the eclipse and the pretotality and posttotality skylight polarization observations as input.
Abstract: The polarization distribution in the sky during a total solar eclipse is calculated with a simple secondary light-scattering model. This model uses the light-intensity measurements near the horizon during the eclipse and the pretotality and posttotality skylight polarization observations as input. It is found that the model can explain various observations during totality, including the quantitative measurements of Shaw [ Appl. Opt.14, 388 ( 1975)] of the polarization distribution of the sky in the solar vertical during the 1973 total eclipse.
18 citations
TL;DR: The amplitudes and phases (relative to a local high precision frequency standard) of WWV HF transmissions on 5, 10 and 15 MHz from Ft. Collins, Colorado, were recorded continuously during the period of the total solar eclipse on 7 March 1970.
17 citations
TL;DR: In this paper, measurements of Faraday rotation and differential absorption on frequencies 2.2, 3.9 and 7.8 MHz have been used to determine the height distribution of collision frequency and electron concentration during the annular solar eclipse of May 20, 1966 and on a comparison day.
17 citations
TL;DR: In this paper, radio-frequency power received from the sun at a wavelength of 50 cm. was measured at three well-separated places during the solar eclipse of November 1, 1948.
Abstract: Radio-frequency power received from the sun at a wavelength of 50 cm. was measured at three well-separated places during the solar eclipse of November 1, 1948. Abrupt changes in slope on the records of received flux density were interpreted as being the result of the covering and uncovering on the sun of small areas of great radio brightness. These areas were found to be associated with some visible sunspots, with positions previously occupied by sunspots, and with one prominence. The average effective temperature of the bright areas was about 5 X 106 °K., and the are= contributed a total power of roughly one-fifth of that from the entire sun. After the effects of active areas had been taken into account, the remaining four- fifths of the power received from the sun was found to originate from a source larger than the visible disk. About 40 per cent. of the power from this source originated outside the edge of the visible disk. The results were consistent with a theoretical distribution of brightness on the source, which involved limb-brightening. The relative magnitudes of the two circularly-polarized components of the solar radiation showed small differences as the bright areas were eclipsed. No predominance of one component was seen when one hemisphere of the sun was eclipsed ; hence no effects of any general magnetic field on the sun were detected.
17 citations