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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 authors analyzed air temperature measurements made near the ground by the Williams College expedition to observe the first total occultation of the Sun [TOS (commonly known as a total solar eclipse)] of the 21st century in Lusaka, Zambia, in the afternoon of June 21, 2001.
13 citations
Journal Article•
TL;DR: The Schaeberle camera as discussed by the authors was a hallmark of the Lick Observatory's direct solar eclipse photography program for the first couple decades of the 20th century, and it was used to obtain high resolution images of inner coronal structure and images in which coronal brightness could be studied.
Abstract: The primary goal of the Lick Observatory's direct solar eclipse photography program was to secure high- resolution images of inner coronal structure and images in which coronal brightness could be studied. Between 1889 and 1932 the Observatory sent out seventeen eclipse expeditions worldwide. During these expeditions, direct coronal photography was a significant part of the program for the first couple of decades. By the end of the expedition series, spectrographic observations became of primary importance, yet direct coronal imaging continued. Lick Observatory astronomer, John M. Schaeberle, conceived and constructed a large portable camera of 5-inch aperture with a focal length of 40-feet, and from 1893 the so-called 'Schaeberle Camera' became a hallmark of the Observatory's eclipse expeditions. In this paper we provide details of the Schaeberle Camera's design, setup and operation, and we briefly discuss some of the ways in which Lick Observatory staff and other astronomers used the plates obtained during the various eclipse expeditions in their investigations of the solar corona.
13 citations
01 Aug 1965
TL;DR: For the radio astronomer, the solar mapping process gave resolution to his solar mapping, revealing the temperature and angular diameters of enhanced regions of solar activity associated with sunspots, plages, and prominences as discussed by the authors.
Abstract: From earliest recorded time man has been fascinated by eclipses of the sun For the astronomer, the eclipse served to reveal features of the chromosphere and the corona More recently, development in perfecting and utilizing the coronograph has provided a continuous monitoring of coronal activity but the eclipse still serves in many optical solar studies For the radio astronomer, the eclipsing process gave resolution to his solar mapping, revealing the temperature and angular diameters of enhanced regions of solar activity associated with sunspots, plages, and prominences The eclipse gave the radio astronomer data on coronal temperatures and on the extent of the corona at many wavelengths The development of high-resolution radio interferometers has lessened the need for eclipse measurements, but many eclipse measurements continue to add to our understanding of solar physics
13 citations
TL;DR: The structure of the corona from the solar limb to a couple of solar radii was observed with a wide dynamic range and a high signal-to-noise ratio as discussed by the authors.
Abstract: White-light observations of the total solar eclipse on 13 November 2012 were made at two sites, where the totality occurred 35 min apart. The structure of the corona from the solar limb to a couple of solar radii was observed with a wide dynamic range and a high signal-to-noise ratio. An ongoing coronal mass ejection (CME) and a pre-CME loop structure just before the eruption were observed in the height range between 1 – 2 R⊙. The source region of CMEs was revealed to be in this height range, where the material and the magnetic field of CMEs were located before the eruption. This height range includes the gap between the extreme ultraviolet observations of the low corona and the spaceborne white-light observations of the high corona, but the eclipse observation shows that this height range is essential for the study of CME initiation. The eclipse observation is basically just a snapshot of CMEs, but it indicates the importance of a continuous coverage of CME observations in this height range in the future.
13 citations
TL;DR: In this article, ground measurements of the geomagnetic field, during the total solar eclipse of July 11, 1991, were carried out at three sites in Costa Rica located within the eclipse's path of totality.
Abstract: Ground measurements of the geomagnetic field, during the total solar eclipse of July 11, 1991, were carried out at three sites in Costa Rica located within the eclipse's path of totality. Near totality, there was a significant change in the total intensity,F. Its normal decrease in the afternoon hours was interrupted during a period of about 45 min, in whichF varied very little. This was due mainly to a small variation in horizontal intensity,H, during such a period. The departure ofF from normal lasted about 100 min; its maximum departure was near 10 nT and occurred about 38 min after totality, The declination,D, also experienced a small change (about 2.3 min) during the total period of the eclipse. The vertical intensity,Z, and the inclination,I, did not show significant changes.
13 citations