Topic
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 paper, atmospheric boundary layer perturbations were monitored during an annular solar eclipse event on December 26, 2019 to understand its impact on meteorological parameters (temperature, relative humidity, wind speed, and wind direction) and trace gas concentrations (O3, NO, NO2, NH3, CO, and HONO) at Calicut (11.24° N, 75.78° E), a tropical city along the coastal belt of Arabian Sea in the southwest coast of Indian Subcontinent).
6 citations
Journal Article•
TL;DR: Preliminary results on short-period oscillations in the corona and changes in the earth's atmospheric parameters, observed during a total solar eclipse of 29 March 2006 from Manavgat, Turkey are reported.
Abstract: We report preliminary results on short-period oscillations in the corona and changes in the earth's atmospheric parameters, observed during a total solar eclipse of 29 March 2006 from Manavgat, Turkey.
6 citations
Posted Content•
TL;DR: The role of the Polynesian sun god Tagaloa has been studied in this paper, and the role of Maui-tikitiki, Tane and Tiki were related to the sun as well.
Abstract: The role of the Polynesian sun god Tagaloa has been studied. The Polynesian characters Maui-tikitiki, Tane and Tiki were related to the sun as well. The solar data of Easter Island are essential indeed. The rongorongo text on the Santiago staff about the solar eclipse of December 20, 1805 A.D. has been decoded. The Mataveri calendar was probably incised on a rock in 1775 A.D. So, a central event during the bird-man festval was the day of vernal equinox. The priests-astronomers watched not only the sun and the moon, but also some stars of the zodiacal constellations and other bright stars.
6 citations
TL;DR: In this article, the authors analyzed temporal changes in the solar corona before, during, and after the total solar eclipse on 21 August 2017 from a set of ground-based and of space-borne observations.
Abstract: Total solar eclipse (TSE) coronal large- and small-scale events were reported in the historical literature but a definite synoptic coverage was missing for studying a relationship with the more general magnetic context of the solar-disk. We here analyze temporal changes in the solar corona before, during, and after the total solar eclipse on 21 August 2017 from a set of ground-based and of space-borne observations. High-quality ground-based white-light (W-L) observations and a deep image processing allow us to reveal these changes for the first time with a fraction of a minute temporal resolution. Displacements of a number of fine coronal features were measured for the first time at these small radial distances, using a diffraction-limited instrument at a single site. The comparison with space-based observations, including observations from the Solar Terrestrial Relations Observatory (STEREO) mission, showed that the features belong to a slow coronal mass ejection (CME) propagating through the corona with the nearly constant speed of 250 km s−1. Our TSE images provide the same typical velocity as measured at a distance of one solar radius from the surface. The event was initiated by coronal dynamics manifested by a prominence eruption that started just before the eclipse observations and an ascent of a U-shaped structure visible in the Atmospheric Imaging Assembly (AIA) 171 A channel, which we assume as the lower part of a coronal cavity. The prominence material was observed draining down towards the chromosphere along the prominence arch. While the prominence disappears in the STEREO-A field-of-view at the height of about 6′ above the limb, the corresponding flux rope seems to continue towards the outer corona and produces the slow CME with turbulent motion. The overall mass of the moving features is evaluated based on absolute photometrical data extracted from our best W-L eclipse image.
6 citations
01 Jan 1982
TL;DR: In this paper, the F Corona was observed from ground in the near infrared at 2,2μ and 3,5μ in an attempt to measure the thermal emission peaks predicted by Peterson and found experiement mentally by Peterson (1967) and Mc Queen (1963), these measurements made in solar eclipse time were necessarily short and of limited signal to noise ratio.
Abstract: During the summers of 1973 and 1979 the F Corona was observed from ground in the near infrared at 2,2μ and 3,5μ in an attempt to measure the thermal emission peaks predicted by Peterson (1963) and found experi mentally by Peterson (1967) and Mc Queen (1963). These measurements made in solar eclipse time were necessarily short and of limited signal to noise ratio. However they could find emission peaks at 3,4 Ro, 3,9 Ro , 8,7 Ro and 9,2 Ro with the dominant peak at 3.9 Ro. The equivalent width of the peak was of the order of 8 arc. minutes. Different authors have found difficulties to explain the form and the existence of these peaks directly related with the depletion of interplanetary dust falling towards the sun Saito et al (1977) Calbert and Beard (1972) Roser and Stau de (1978). Another authors Mc Queen and Poland (1977), Bohlin (1971) could find coronal brightness changes justifiable by electron streams with long persistence time.
6 citations