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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 gamma ray flux was measured during the annular solar eclipse on January 15, 2010 at Rameswaram, India using NaI (Tl) scintillator detectors and the variation in charged particles and gamma rays was monitored using Geiger M u ¨ller (GM) counters.
20 citations
TL;DR: In this article, the authors present observations from 11 very low frequency (VLF)/low-frequency (LF) receivers across the continental United States during the 21 August 2017 “Great American Solar Eclipse.
Abstract: We present observations from 11 very low frequency (VLF)/low-frequency (LF) receivers across the continental United States during the 21 August 2017 “Great American Solar Eclipse.” All receivers detected transmissions from VLF/LF beacons below 50 kHz, while seven also recorded LF beacons above 50 kHz, yielding dozens of individual transmitter-receiver radio links. Our observations show two separable superimposed signatures: (1) a gradual rise and fall in signal levels visible on almost all paths as the eclipse advances and then declines, as VLF attenuation is reduced by the changing ionosphere under an eclipsed Sun, and (2) direct reflective scattering off the narrow 100-km-wide totality spot, observed more uniquely when the transmitter or receiver, if not both, are relatively close to the totality spot. Plain Language Summary A solar eclipse provides a unique opportunity to study a region of the upper atmosphere known as the ionosphere, which is essentially the transition zone between Earth’s atmosphere and the space environment. While the Sun is known to have a dominant impact on the electrical properties of this region, it is difficult to quantify it precisely since these altitudes, 60–90 km, are too high to reach with balloons yet too low for satellites. On the other hand, the lower ionosphere plays a key role in communications and navigation. Very low frequency/low-frequency radio waves at 3–300 kHz reflect from this region, thus allowing us to remotely diagnose the lower ionosphere. A solar eclipse is the only time when the Sun’s influence rapidly turns off over a very small region. In this paper, we have analyzed dozens of diagnostic observations, namely, transmitter-to-receiver communications links, that allow to quantify how the lower ionosphere responded to this unique geophysical event. As the Sun’s influence changes, so too does the characteristics of these very low frequency/low-frequency transmitters detected many hundreds to thousands of miles away.
19 citations
TL;DR: A survey of the infrared coronal spectrum between 1 μ and 3 μ was made from a high altitude aircraft during the 7 March, 1970, solar eclipse as discussed by the authors, and the observations were made with a Fourier transform spectrometer and were confined to the outer chromosphere and inner corona.
Abstract: A survey of the infrared coronal spectrum between 1 μ and 3 μ was made from a high altitude aircraft during the 7 March, 1970, solar eclipse. The observations were made with a Fourier transform spectrometer and were confined to the outer chromosphere and inner corona. In addition to well known chromospheric lines of Hi and Hei, nine additional lines were seen. Evidence is presented for the tentative assignment of these lines to forbidden transitions in highly ionized atoms of magnesium, aluminum, silicon, sulphur, and chromium.
19 citations
TL;DR: In this paper, the effect of total solar eclipse (TSE) on the D-region of the ionosphere was investigated using ELF/VLF radio signal. And the modeled electron density height profile of the lower ionosphere depicts linear variation in the electron density with respect to solar radiation as observed by tweek analysis.
19 citations
TL;DR: In this article, the authors used a hydrostatic regional weather prediction model to simulate the tropospheric response to the total solar eclipse on the 11 August 1999 is simulated over central Europe both with real-time data and for a water vapor and cloud free scenario.
Abstract: Using a hydrostatic regional weather prediction model, the tropospheric response to the total solar eclipse on the 11 August 1999 is simulated over central Europe both with real time data and for a water vapor and cloud free scenario. The solar constant in the model is reduced stepwise along the surface path of the moon's shadow, reaching a value of 0 W/m 2 for a typical time span of 2 minutes during totality. In the presence of a large scale upper tropospheric trough centered over western Europe, the predicted radiative cooling ranging from -2°C over the UK, France and Germany to -5°C along the almost cloudless coast line of Croatia is in good agreement with observations. Over southeastern Europe the maximum cooling reaches -6°C to -7°C and the maximum sea surface pressure rise is enhanced from +0.4 hPa to +1.2 hPa, when the simulation is done without water vapor and clouds. The normally observed wind reduction is simulated as well as the temperature dependent increase of relative humidity near the ground. For some minutes even a slight cyclonic circulation is shown by the model surface winds. The upper air response to the eclipse is clearly correlated with the distribution of water vapor and clouds. The temperature and geopotential signals at the 500 hPa level are in the order of -0.01°C and -1 gpm remaining well below the sensitivity of routine sensors.
19 citations