Solar eclipse

About: Solar eclipse is a research topic. Over the lifetime, 2737 publications have been published within this topic receiving 22625 citations.

The April 8, 2005, Eclipse White-Light Corona

Abstract: The hybrid solar eclipse of April 8, 2005, provided a good opportunity to observe the white-light solar corona, even though the eclipse lasted just 30 seconds and could be seen only from ships in the Pacific Ocean. During the eclipse, we detected a unique ‘cloud’ of particles in the white-light corona above the west limb ≈260°–270°. We compare this feature with EUV images from SOHO. The feature’s density and temperature seem comparable to a coronal condensation, and, like a coronal condensation, it is connected to the emergence of material from the solar surface without a flare. However, the morphology of the feature shows clear differences from a classical coronal condensation.

Specific features of variations in the characteristics of VLF signals when the lunar shadow propagated along the path during the solar eclipse of March 29, 2006

Abstract: The effects of the solar eclipse of March 29, 2006, in the signals of ULF radio stations, in the intensity of regular radio noise at frequencies of 0.3–10 kHz, and in the number of atmospherics received in Yakutsk mostly from the west have been considered. The observations were performed using a multichannel parallel analyzer-recorder (11 channels in the frequency band 0.47–8.7 kHz), one-point lightning direction and range finder (0.3–100 kHz), narrow-sector radio noise direction-finder (0.3–10 kHz), recorder of signals from VLF radio stations, and broadband radio noise recorder (0.3–100 kHz). A GPS clock was used to synchronize a recorder of signals from VLF radio stations. The effect was observed in radio signals, radio noise, and number of atmospherics from the direction 270° ± 20° counted off clockwise from the north during the last stage of the eclipse (∼ 1100–1200 UT), when the lunar shadow approached the line of the nighttime terminator and obscured part of the signal propagation path. The effect was observed as an enhancement of the received signals by a factor of ∼1.2, a factor of ∼1.4 increase in the number of atmospherics, and a change in the radio station phase values.

Rocket measurements of D‐region electron number densities at sunrise

Abstract: This note reports the results of rocket measurements of quiet D-region electron number-density profiles near sunrise. The measurements were made with ARCAS rockets in New Zealand at a latitude of 350S as part of a study of the May 30, 1965, solar eclipse. The electron number density was determined by a Faraday rotation technique using CW radio transmissions at frequencies of 2.4 and 3.3 Mc/s. To measure the Faraday rotation effect, a linearly polarized signal was transmitted from a ground-based antenna and received on a linearly polarized antenna in the rocket.

Abnormalities of the time comparisons of atomic clocks during the solar eclipses.

Abstract: We have investigated into the time comparison data of the atomic clocks of some stations and have found that the solar eclipse has influence on the time comparison of atomic clocks.