Showing papers on "Solar eclipse published in 1988"

The Height Distribution of the Kinetic Temperature and Turbulent Velocity of Solar Hα Spicules

Abstract: The height distribution of the kinetic temperature of solar Hα spicules is determined using the widths of optically thin hydrogen and metallic lines obtained at the total solar eclipse of 1966: the temperature was found to be 8600 K at the height of 2200 km measured from the radial optical depth of unity at 5000 A, and to decrease to a minimum of 5000 K ± 180 K at 3200 km, and to increase again to 8200 K at 6000 km.

A Multilayer X-Ray Mirror For Solar Photometric Imaging Flown On A Sounding Rocket

Abstract: The flight of a multilayer-coated mirror on a sounding rocket experiment on March 17, 1988 which was used to obtain photometric images of the sun just prior to solar eclipse is discussed. The rocket payload and the choice of passband are described. The design of the multilayer, the fabrication of the mirror, and the reflectance measurements are addressed.

Sharp Rays: Javanese Responses to a Solar Eclipse

Abstract: When a total solar eclipse occurred over Central Java late in the morning of June 11, 1983, the air became very still and Java's lush vegetation glowed in the eerie light characteristic of sunset in the tropics. As at sunset, too, the horizon turned red, but it did so not only in the west but in all directions, and in the half-light distant volcanoes usually obscured by the glare of the sun became visible. For the four minutes of total eclipse, the sun, almost directly overhead, looked like a black ball surrounded by a brilliant white light. Most eerily of all, in one of the most densely populated rural areas in the world, there was no traffic on the roads, no movement in towns or villages, and no one watching the eclipse.

Analysis of Pre-Telescopic and Telescopic Sunspot Observations

Abstract: Sunspot data from the RGO series covering the period from 1874 to 1954 are analysed to show the asymmetric distribution of sunspot areas north and south of the solar equator. A detailed catalogue of naked-eye sunspots from Far Eastern annals is compiled from both the pre-telescopic and telescopic periods. Analysis of these fragmentary records indicates a mean period of about 10 years.

Solar coronal and magnetic field observations near the time of the 1988 March 18 solar eclipse

Abstract: Observations made during the interval March 1-31, 1988, are presented which were designed to provide a synoptic context in which data from the March 18, 1988, total solar eclipse can be interpreted. Daily observations made with the Mark III K-coronameter and the H-alpha prominence monitor at the Mauna Loa Solar Observatory, along with photographic records of the Sun in H-alpha from the flare patrol at Mees Solar Observatory on Haleakala, Maui, are included. Observations of the longitudinal component of the photospheric magnetic field made at Mees Solar Observatory were also gathered around the period of the eclipse. Together with the white-light image of the corona at the eclipse, these coronal and magnetic field observations assembled into synoptic maps for this epoch, are presented. On the basis of these observations, an interpretation of the global density distribution of the corona at the time of the eclipse is constructed.

Solar variability from historical records.

Abstract: The application of historical observations of (i) the Sun’s diameter, (ii) the corona and (iii) sunspots to the question of longterm solar variability is considered. Although solar diameter measurements can be mapped in detail since about A.D. 1700, at present it is not possible to use these results to estimate changes in the solar output of energy with any degree of confidence. Coronal observations are too infrequent to prove of much value in the study of changes in solar activity. The telescope record of sunspots since A.D. 1700 is of paramount importance to this problem. However, it is not possible to use observations of sunspots made before this time to reliably delineate solar activity owing to the presence of spurious trends in the data.

Power supply system

Abstract: PURPOSE:To supply an artificial satellite with power at all times by supplying the artificial satellite with the power of first and second power generating satellites. CONSTITUTION:An artificial satellite 1 has receiving antennas 7, 8 for receiving microwave power radiated from first and second power generating satellites 2, 3. The first and second power generating satellites 2, 3 respectively have solar cells 4, 5 and transmission antennas 9, 10. When the first satellite 2 enters a solar eclipse, the second satellite 3 receiving solar rays supplies the artificial satellite 1 with microwave power. When the second satellite 3 enters the solar eclipse, the first satellite 2 receiving solar rays supplies the artificial satellite 1 with microwave power.

Active region coronal loops observed at the total solar eclipse of February 16, 1980

Abstract: Analyse des structures des boucles coronales au-dessus d'une region active pendant une eclipse solaire totale Calcul des densites et temperatures des boucles a partir d'images monochromatiques de raies du fer ionise et du continuum

Changes in the earth's rate of rotation between A.D. 1672 and 1806 as deduced from solar eclipse timings

Abstract: Solar eclipse timings measured between A.D. 1672 and 1806 are analyzed to study the variation of Delta T (= ET - UT) over this interval. These solar eclipse observations confirm the results of Brouwer (1952), Martin (1969), and Stephenson and Morrison (1969) which were obtained from the analysis of occultations in this period. It is believed that Goldstein's (1985) analysis inadequately represents the changes in Delta T.

A coronal condensation observed at the total solar eclipse of June 11, 1983 and a related transient prominence

Abstract: A coronal condensation was observed simultaneously with Fexiv λ5303, Fex λ6374, Fe xi λ7892, and Hα filtergraphs. The size and shape of the condensation in λ5303 are different from those in other filtergrams. Hα filtergrams taken around the eclipse time show that a small transient prominence exists in close proximity to the condensation core and behaves like a post-flare loop system, though the appearance is quite different and no flare-report exists. A small-scale energetic phenomenon seems to have occurred at the top of magnetic loops.

Demonstration device of the sun, the moon and the earth movement

Abstract: The utility model discloses a demonstration device of the sun, the moon and the earth movements, which belongs to a teaching apparatus for middle schools and primary schools. The earth rotation, the revolution of the earth which winds the sun, the change of the four seasons and the day and night, and the appearance and the schedule of the leap year can all be demonstrated by the utility model; the moon rotation, the revolution of the moon which winds the earth, the state of the solar eclipse and the lunar eclipse, and the appearance and the schedule of the intercalary month can also be demonstrated by the utility model. The utility model is characterized in that one suite of epicyclic gear train can realize the precision of the movements of the sun and the earth, and 2.24 days are advanced after the demonstrative running of ten thousand years; the other suite of epicyclic gear train can realize the precision of the movements of the moon and the earth, and 2.26 days are advanced after the demonstrative running of ten thousand months. The shaft bracket of the earth rotation is arranged on the flat face of the translational movements; the utility model can make the invariant of the direction and the included angle of the axis of the earth rotation and the flat face of the revolution of the earth which winds the sun.

Photometric Analysis of the Solar Corona on 1984 November 22/23

Abstract: The total solar eclipse of 1984 November 22/23 was observed from a French naval vessel off Noumea (New Caledonia) in the Coral Sea. The observations were made by a team from the S.A.F., led by Serge Koutchmy and Christian Nitschelm of the Institut d’Astrophysique de Paris. The duration of the eclipse was considerably longer off New Caledonia (1 m 39 s) than in Papua-New-Guinea (55 s). However, the observational site — on board a ship well out to sea — greatly restricted the use of long-focal-length instruments that are normally employed. The equipment used to photograph this eclipse therefore was chosen with motion (pitching, rolling, etc.) of the support in mind. Short focal lengths were preferred, although one refractor with a focal length of 1.5 m was used as a trial.

Radiation data during solar eclipse

Abstract: SYNOPSIS On 11 June 1983, a total eclipse of the sun occurred over Java, producing a partial eclipse over Northern Australia. Pyrheliometers located at three solar radiation stations in the Northern Territory recorded the direct radiation during the eclipse. The unobscured area of the solar disc during this event was computed from formulae given in the Supplement to the Astronomical Ephemeris [1]. Comparison of the reduced direct solar insolation with the uneclipsed solar area shows an approximately constant ratio between these two quantities during the event, based on measurements taken at Darwin.