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  • 1
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    Purely coronal flare-like variations (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Quasiperiodic X-ray, UV, microwave, and metric-wave variations after a solar flare on November 6, 1980 are reported and analyzed, based on observational data from SMM (HXRBS, UVSP, HXIS), GOES-2, the 100-m radiotelescope at Bonn, and the Nancay radioheliograph. The maxima of the 13 brightenings observed are listed and characterized; a comparison is made with a 'normal' flare at 17:26 UT on the same day. The HXIS and UVSP data are discussed in terms of the physical properties, X-ray flux, O V flux, and H-alpha flux. The variations are found to be mainly thermal and purely coronal, with no chromospheric (H-alpha) participation (in contrast to the 17:26 flare). Since strong X-ray emissions were observed which should have involved the chromosphere through magnetic-field-line heat conduction, it is proposed that the variations wre produced ina coronal plasmoid magnetically separate from the chromosphere. A mechanism for the evolution of such a plasmoid from the upper loops of a giant X-ray arch is discussed. An iterative HXIS-image-deconvolution process is presented in an appendix.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 85; June 198
    Format: text
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  • 2
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    The Queen's flare - Its structure and development; precursors, pre-flare brightenings, and aftermaths (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: A limb flare, which started at about 20:20 UT on April 30, 1980, was observed by several of the instruments on the Solar Maximum Mission (SMM) spacecraft. This flare has been the subject of a joint analysis of the SMM instruments. The present investigation represents a continuation of research reported in part by Woodgate et al. (1981) and Gabriel et al. (1981). Several questions are explored regarding the preflare activity, the evolution of the flare, and its decay. It is concluded that the X-ray brightenings observed before the flare were indicative only of the generally high level of activity from this region. They were not connected with the build-up of energy before the flare since similar brightenings were observed in the region after the flare. At least one brightening occurred at the site of the kernel before the flare. There is also some evidence of a tongue.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 84; April 19
    Format: text
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  • 3
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    Periodicities in the occurrence of aurora as indicators of solar variability (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: A compilation of records of the aurora observed in China from the Time of the Legends (2000 - 3000 B.C.) to the mid-18th century has been used to infer the frequencies and strengths of solar activity prior to modern times. A merging of this analysis with auroral and solar activity patterns during the last 200 years provides basically continuous information about solar activity during the last 2000 years. The results show periodicities in solar activity that contain average components with a long period (approx. 412 years), three middle periods (approx. 38 years, approx. 77 years, and approx. 130 years), and the well known short period (approx. 11 years).
    Keywords: SOLAR PHYSICS
    Type: JPL Solar Wind Five; p 349-352
    Format: application/pdf
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  • 4
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    Activated solar filaments and flares (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Skylab observations have shown that activations and disruptions of dark H-alpha filaments are one of the basic and most important mechanisms of solar activity. The Kopp-Pneuman theory of post-flare loops shows that the process which disrupts a filament opens the magnetic field and causes a greatly enhanced mass flow along the field lines. The open field lines subsequently reconnect, starting from the bottom of the corona and proceeding upwards. This process can last for many hours. Hot loops are first seen in X-rays, then in extreme UV lines, and, after an appropriate cooling time, in H-alpha as the loop prominence systems.
    Keywords: SOLAR PHYSICS
    Format: text
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  • 5
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    The thermal X-ray flare plasma (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Following a review of current observational and theoretical knowledge of the approximately 10 to the 7th K plasma emitting the thermal soft X-ray bursts accompanying every H alpha solar flare, the fundamental physical problem of the plasma, namely the formation and evolution of the observed X-ray arches, is examined. Extensive Skylab observations of the thermal X-ray plasmas in two large flares, a large subflare and several compact subflares are analyzed to determine plasma physical properties, deduce the dominant physical processes governing the plasma and compare large and small flare characteristics. Results indicate the density of the thermal X-ray plasma to be higher than previously thought (from 10 to the 10th to 10 to the 12th/cu cm for large to small flares), cooling to occur radiatively as much as conductively, heating to continue into the decay phase of large flares, and the mass of the thermal X-ray plasma to be supplied primarily through chromospheric evaporation. Implications of the results for the basic flare mechanism are indicated.
    Keywords: SOLAR PHYSICS
    Format: text
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  • 6
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    Transient brightenings of interconnecting loops. III Interpretation (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Two alternative interpretations of the sudden X-ray brightenings observed in loops that interconnect active regions are presented. A fast tearing mode may be excited in those newly formed interconnecting loops within which sufficient magnetic free energy is stored to drive the mode. Alternatively, anomalous Joule heating driven by an inductive electric field parallel to the magnetic field, varying on a time scale of order of a minute, may cause the brightenings. It is suggested that it is plausible that the fast tearing mode may be the cause of brightenings in the young newly formed interconnecting loops, whereas the anomalous Joule heating might occur in old loop connections when an exteral disturbance propagates through them.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 87; Sept
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  • 7
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    Particle acceleration in the process of eruptive opening and reconnection of magnetic fields (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Keywords: SOLAR PHYSICS
    Type: Symposium on Solar and interplanetary dynamics; Aug 27, 1979 - Aug 31, 1979; Cambridge, MA
    Format: text
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  • 8
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    Structure and physics of solar faculae. III - The densities in the chromosphere-corona transition zone (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 83; Feb. 198
    Format: text
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