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  • Books
  • Other Sources  (7)
  • SOLAR PHYSICS  (7)
  • 1980-1984  (7)
  • 1982  (7)
  • 1
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    About the onsets of closely-consecutive homologous flares (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The onsets of closely consecutive homologous flares (CCHF), which are separated by less than 6 hours and most often by about 1 hour, are compared with that of isolated flares (no flare in the region half a day before). Isolated flares appear to be formed of two components, a surging arch and a flaring arch, while a set of CCHF may be composed of consecutive elementary flares or of a series of complex ones. It is shown that the onset of eruptive flare phenomena is not the same for an isolated event and for a member of CCHF (excluding the first) as found in H-alpha and EUV observations, and probably in X-ray observations also. It is suggested that a CCHF set would become a single flare with episodic enhancement of brightness by taking account of the common H-alpha behavior of surging and flaring arches as well as the EUV emission.
    Keywords: SOLAR PHYSICS
    Type: (ISSN 0273-1177)
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Unusual coronal activity following the flare of 6 November 1980 (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The major two-ribbon flare that occurred on November 6, 1980 is discussed, using data from the hard X-ray imaging spectrometer aboard the SMM satellite. The post-flare X-ray arch and loops are analyzed, showing the flare characteristics, the coronal arch, the time variations of X-rays after the flare, and the time variation of the maximum intensity at the top of the coronal arch in the 3.5-5.5 keV range. A comparison is made with an earlier arch. The post-flare conronal brightness variations are discussed, including a correlation with a 169 MHz noise stomr, the absence of chromospheric excitation, the brightness and temperature of the X-ray arch, the locations of the brightenings, and the details of the first and fifth brightenings. Problems posed by the observations are discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 80; Sept
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    NASA TECHNICAL REPORTS
  • 3
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    Observations of a post-flare radio burst in X-rays (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: More than six hours after the two-ribbon flare of May 21, 1980, the hard X-ray spectrometer aboard the SMM imaged an extensive arch above the flare region which was found to be the lowest part of a stationary post-flare noise storm recorded at the same time at Culgoora. The bent crystal spectrometer aboard the SMM confirms that the arch emission was basically thermal. Variations in brightness and energy spectrum at one of the supposed footpoints of the arch are seen as correlation in time with radio brightness, suggesting that suprathermal particles from the radio noise regions dumped in variable quantities onto the low corona and transition layer.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 75; Jan. 198
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    NASA TECHNICAL REPORTS
  • 4
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    EUV arcades - Signatures of filament instability (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: The present investigation is based on the EUV observations from the HCO spectroheliometer aboard Skylab. These observations provide a great deal of information on coronal structures. The investigation is concerned with the EUV corona around active region filaments. One of its goals is to define the geometry and temperature distribution around those filaments which appear to be 'stable' (lifetimes equal to or greater than 2 days). The second goal is to study time changes in structures associated with other filaments which are 'unstable'. It is pointed out that the filaments and associated EUV loops reported in this investigation are not flare-related. The data of primary interest are those of Sept. 5, 1973, for which there exist simultaneous EUV and H-alpha filtergrams for the active region McMath 12510. It is found that active region filaments lie within channels of low emissivity in EUV lines formed above 1.5 x 10 to the 6th K.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 81; Nov. 198
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  • 5
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    Study of the post-flare loops on 29 July 1973. IV - Revision of T and n sub e values and comparison with the flare of 21 May 1980 (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Revised temperature and density estimates are provided in a synthesis of previous studies of the two-ribbon solar flare of July 29, 1973 and results are compared with observations of a similar event by the Solar Maximum Mission on May 21, 1980. Photographs taken through X ray filters permitted determination of the spatial distribution of temperature and density in the loop system and variations over time. The entire growth process of the flare is detailed, including the magnetic field configurations and the enlargement of the Halpha flare ribbon separation distance. The temperature is revised to 8.8 million K during maximum soft X ray emission and 6.8 million K at the appearance of the last Halpha loops. The 1973 flare is noted to have occurred in an old, decaying spotless region, producing higher loops at lower density than the 1980 flare, which displayed ribbons imbedded in a sunspot group.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 78; June 198
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    NASA TECHNICAL REPORTS
  • 6
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    Solar corona at high resolution (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: The earth's surface is shielded from solar X rays almost completely by the atmosphere. It is, therefore, necessary to place X-ray detectors on rockets or orbiting satellites. Solar rays were detected for the first time in the late 1940's, using V-2 rockets. In 1960, the first true X-ray images of the sun were obtained with the aid of a simple pinhole camera. The spatial resolution of the X-ray images could be considerably improved by making use of reflective optics, operating at grazing incidence. Aspects of X-ray mirror developments are discussed along with the results obtained in coronal studies utilizing the new devices for the observation of solar X-ray emission. It is pointed out that the major achievements of the Skylab missions were due primarily to the unique opportunity to obtain data over an extended period of time. Attention is given to normal incidence X-ray optics, achievements possible by making use of high spatial resolution optics, and details of improved mirror design.
    Keywords: SOLAR PHYSICS
    Type: High resolution soft X-ray optics; Nov 18, 1981 - Nov 20, 1981; Brookhaven, NY
    Format: text
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    NASA TECHNICAL REPORTS
  • 7
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    Structure and physics of solar faculae. II - The non-thermal velocity field above faculae (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Description: The OSO-8 satellite enabled the study of various characteristics of the profiles of Si II, Si IV, C IV, and O VI lines above active areas of the sun, as well as above quiet areas, and the derivation of some physical properties of the transition region between chromosphere and corona (CCT). The study of the lines shows a general tendency for the microvelocity fields on the average to be nearly constant for the heights corresponding to a temperature greater than 100,000 K; however they seem to slightly increase with height in quiet areas, and decrease in active areas. A multicomponent model of the CCT is necessary, and its geometry is far from being a set of plane-parallel columns. It is similar to an association of moving knots within the nonmoving principal component of the matter. The proportion of mass, in the knots relative to that in the nonmoving component, is several times larger in active regions than in quiet regions. In the knots, the nonthermal microvelocity fields are smaller in active regions and seem to decrease for temperature increasing above 100,000 K, contrary to what happens in the steady principal component.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 78; May 1982
    Format: text
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