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  • 1
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    Study of the post-flare loops on 29 July 1973. I - Dynamics of the X-ray loops (1979)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: We derive an empirical model of the X-ray emitting post-flare loops observed during the decay phase of the 29 July 1973 flare. We find that the loops are elliptical, with the brightest emitting region at the tops. We determine the height, velocity of growth, and ratio of height to width of the loops at times from 3 to 12 hr after the flare onset.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 62; May 1979
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  • 2
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    Study of the post-flare loops on 29 July 1973. II - Physical parameters in the X-ray loops (1979)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: We use the filter ratio method of analysis to determine spatially resolved values of plasma parameters in the X-ray emitting post-flare loop system which developed on 29 and 30 July 1973. We find that the loops were hotter and had higher plasma pressure at their tops than near their footpoints. The loop tops were at nearly the same temperature at different places 3 hr after the flare maximum and were also at nearly this same temperature 3 and 8 hr later. Variations in brightness transverse to the loops were due to variations in emission measure. We show by consideration of radiative losses alone that energy must have been added to the hottest part of the flare, at the tops of the loops, late in the decay phase of the flare.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 62; May 1979
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  • 3
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    High coronal structure of high velocity solar wind stream sources (1977)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: It is shown analytically that the transition from a high-speed stream source to the ambient coronal conditions is quite rapid in longitude in the high corona. This sharp eastern coronal boundary for the solar wind stream sources is strongly suggested by the solar wind 'dwells' which appear in plots of solar wind velocity against constant-radial-velocity-approximation source longitudes. The possibility of a systematic velocity-dependent effect in the constant-radial-velocity approximation, which would cause this boundary to appear sharper than it is, is investigated. A velocity-dependent interplanetary propagation effect or a velocity-dependent 'source altitude' are two possible sources of such a systematic effect. It is shown that, for at least some dwells, significant interplanetary effects are not likely. The variation of the Alfvenic critical radius in solar wind dwells is calculated, showing that the high-velocity stream originates from a significantly lower altitude than the ambient solar wind.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 51; Mar. 197
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  • 4
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    Solar wind stream structure during the early phase of solar cycles 20 and 21 (1978)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 60; Nov. 197
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  • 5
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    The relationship between solar activity and coronal hole evolution (1978)
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    Publication Date: 2019-06-27
    Description: The relationship between coronal hole evolution and solar active regions during the Skylab period is examined. A tendency is found for holes to grow or remain stable when the activity nearby, seen as calcium plages and bright regions in X-rays, is predominantly large, long-lived regions. It is also found that there is a significantly higher number of small, short-lived active regions, as indicated by X-ray bright points, in the vicinity of decaying holes than there is near other holes. This is interpreted to mean that holes disappear at least in part because they become filled with many small scale, magnetically closed, X-ray emitting features. This interpretation, together with the observation that the number of X-ray bright points was much larger near solar minimum than it was during the Skylab period, provides a possible explanation for the disappearance of the large, near-equatorial coronal holes at the time of solar minimum.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 60; Nov. 197
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  • 6
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    Coronal hole evolution by sudden large scale changes (1978)
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    Publication Date: 2019-06-27
    Description: Sudden shifts in coronal-hole boundaries observed by the S-054 X-ray telescope on Skylab between May and November, 1973, within 1 day of CMP of the holes, at latitudes not exceeding 40 deg, are compared with the long-term evolution of coronal-hole area. It is found that large-scale shifts in boundary locations can account for most if not all of the evolution of coronal holes. The temporal and spatial scales of these large-scale changes imply that they are the results of a physical process occurring in the corona. It is concluded that coronal holes evolve by magnetic-field lines' opening when the holes are growing, and by fields' closing as the holes shrink.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 56; Jan. 197
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  • 7
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    Solar wind, energetic particles, and coronal magnetic structure - The first year of solar cycle 20 (1977)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Coronal magnetic field structure is investigated by using solar and interplanetary magnetic polarity measurements and by using observations of solar wind plasma and energetic particles during the first 8 months of 1965. When it is compared by using all data available during this period, interplanetary polarity (mapped back to the high corona by using observed solar wind velocities) correlates best with mid-latitude solar polarity. However, when it is compared at only those times when energetic particles were present in the interplanetary medium and again at times of fast solar wind, the best correlation is with equatorial solar polarity. From these results we infer that energetic particles and fast solar wind escape preferentially from equatorial coronal magnetic structures which are open, while the more usual equatorial structures at this time are closed.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 82; June 1
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  • 8
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    Association of X-ray arches with chromospheric neutral lines (1976)
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    Publication Date: 2019-06-27
    Description: Daily maps of magnetic neutral lines derived from H-alpha observations have been superimposed on solar X-ray images for the period from June 15 to 30, 1973. Nearly all X-ray-emitting structures consist of systems of arches covering chromospheric neutral lines. Areas of low emissivity, coronal holes, appear as the areas between arcades of arches. The presence of a coronal hole, therefore, is determined by the spacing between neutral lines and the scale of the arches over those neutral lines. X-ray emissivity on the solar disk extends from neutral lines in proportion to the vertical and horizontal scale of the arches over those neutral lines. Increasing scale of arches corresponds with increasing age of magnetic fields associated with the neutral line. All X-ray filament cavities coincided with neutral lines, but filaments appeared under cavities for only part of their length and for only a fraction of the disk passage.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 49; July 197
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  • 9
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    A comparison of solar wind streams and coronal structure near solar minimum (1977)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Solar wind data from the MIT detectors on the IMP 7 and 8 satellites and the SOLRAD 11B satellite for the solar-minimum period September-December, 1976, were compared with X-ray images of the solar corona taken by rocket-borne telescopes on September 16 and November 17, 1976. There was no compelling evidence that a coronal hole was the source of any high speed stream. Thus it is possible that either coronal holes were not the sources of all recurrent high-speed solar wind streams during the declining phase of the solar cycle, as might be inferred from the Skylab period, or there was a change in the appearance of some magnetic field regions near the time of solar minimum.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 4; July 197
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  • 10
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    Relation of large-scale coronal X-ray structure and cosmic rays. II - Coronal control of interplanetary injection of 300 keV protons (1975)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: We report the striking coronal control of low-energy solar particles from the solar flare of September 7, 1973. The flare was at S18, W46 (Carrington longitude 188 deg) in McMath Plage Region 12307. We find strong intensity gradients in heliolongitude (about 10% per deg) that are nearly identical in protons, helium, and medium nuclei at energies about 0.5 MeV/nuc, as well as relativistic electrons and 3 MeV protons. This pervasive gradient occurs at longitudes over bright X-ray emission structures east of the flare site which interconnect large-scale chromospheric polarity regions identifiable in H-alpha filtergrams.
    Keywords: SOLAR PHYSICS
    Type: International Cosmic Ray Conference; Aug 15, 1975 - Aug 29, 1975; Munich
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