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  • 1
    Electronic Resource
    Electronic Resource
    Is Ball Lightning a Nuclear Phenomenon ? (1970)
    [s.l.] : Nature Publishing Group
    Nature 228 (1970), S. 545-547 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] In one incident a lightning ball fell into a rain barrel and boiled 18 1. of water for a few minutes5. The energy of the ball was estimated as 8 x 106 J with an energy density between 2 x 1C9 and 5 x 109 J m-3 (refs. 4, 6, 7). Another report8, brought to our attention by C. M. Botley, describes a ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/228545a0
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  • 2
    Electronic Resource
    Electronic Resource
    A search for forward scattering of sunlight from lunar libration clouds
    Amsterdam : Elsevier
    Planetary and Space Science 23 (1975), S. 1313-1319 
    Details
    ISSN: 0032-0633
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Geosciences , Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0032-0633(75)90155-5
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  • 3
    Electronic Resource
    Electronic Resource
    Do we understand coronal mass ejections yet?
    Amsterdam : Elsevier
    Advances in Space Research 6 (1986), S. 297-306 
    Details
    ISSN: 0273-1177
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Mechanical Engineering, Materials Science, Production Engineering, Mining and Metallurgy, Traffic Engineering, Precision Mechanics , Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0273-1177(86)90164-X
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  • 4
    Electronic Resource
    Electronic Resource
    The association of coronal mass ejection transients with other forms of solar activity (1979)
    Springer
    Solar physics 61 (1979), S. 201-215 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Coronal mass ejection transients observed with the white light coronagraph on Skylab are found to be associated with several other forms of solar activity. There is a strong correlation between such mass ejection transients and chromospheric Hα activity, with three-quarters of the transients apparently originating in or near active regions. We infer that 40% of transients are associated with flares, 50% are associated with eruptive prominences solely (without flares), and more than 70% are associated with eruptive prominences or filament disappearances (with or without flares). Nine of ten flares which displayed apparent mass ejections of Hα-emitting material from the flare site could be associated with coronal transients. Within each class of activity, the more energetic events are more likely to be associated with an observable mass ejection.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155456
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  • 5
    Electronic Resource
    Electronic Resource
    Prompt solar proton events and coronal mass ejections (1978)
    Springer
    Solar physics 57 (1978), S. 429-443 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We have used data from the HAO white light coronagraph and AS&E X-ray telescope on Skylab to investigate the coronal manifestations of 18 prompt solar proton events observed with the GSFC detectors on the IMP-7 spacecraft during the Skylab period. We find evidence that a mass ejection event is a necessary condition for the occurrence of a prompt proton event. Mass ejection events can be observed directly in the white light coronagraph when they occur near the limb and inferred from the presence of a long decay X-ray event when they occur on the disk. We suggest that: (1) the occurrence of mass ejection events facilitates the escape of protons - whether accelerated at low or high altitudes - to the interplanetary medium; and (2) there may exist a proton acceleration region above or around the outward moving ejecta far above the flare site.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00160116
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  • 6
    Electronic Resource
    Electronic Resource
    The High Altitude Observatory Coronagraph/Polarimeter on the Solar Maximum Mission (1980)
    Springer
    Solar physics 65 (1980), S. 91-107 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The High Altitude Observatory Coronagraph/Polarimeter, to be flown on the National Aeronautics and Space Administration's Solar Maximum Mission satellite, is designed to produce images of the solar corona in seven wavelength bands in the visible spectral range. The spectral bands have been chosen to specifically exclude or include ‘chromospheric’ spectral lines, so as to allow discrimination between ejecta at high (coronal) and low (chromospheric) temperatures, respectively. In addition, the instrument features spectral filters designed to permit an accurate color separation of the F and K coronal components, and a narrow band (5.5 Å) filter to observe the radiance and polarization of the Fe xiv 5303 Å line. The effective system resolution is better than 10 arc sec and the instrument images a selected quadrant (or smaller field) on an SEC vidicon detector. The total height range that may be recorded encompasses 1.6 to more than 6.0R ⊙ (from Sun center). The instrument is pointed independently of the SMM spacecraft, and its functions are controlled through the use of a program resident within the onboard spacecraft computer. Major experimental goals include: (a) Observation of the role of the corona in the flare process and of the ejecta from the flare site and the overlying corona; (b) the study of the direction of magnetic fields in stable coronal forms, and, perhaps, ejecta; and (c) examination of the evolution of the solar corona near the period of solar maximum activity.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151386
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  • 7
    Electronic Resource
    Electronic Resource
    Frequency of coronal transients and solar activity (1976)
    Springer
    Solar physics 48 (1976), S. 127-135 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The High Altitude Observatory's white light coronagraph aboard Skylab observed some 110 coronal transients - rapid changes in appearance of the corona - during its 227 days of operation. The longitudes of the origins of these transients were not distributed uniformly around the solar surface (51 of the 100 events observed in seven solar rotations arose from a single quadrant of longitude). Further, the frequency of transient production from each segment of the solar surface was well correlated with the sunspot number and Ca ii plage (area × brightness) index in the segment, rotation by rotation. This correlation implies that transients occur more often above strong photospheric and chromospheric magnetic fields, that is, in regions where the coronal magnetic field is stronger and, perhaps, more variable. This pattern of occurrence is consistent with our belief that the forces propelling transient material outward are, primarily, magnetic. A quantitative relation between transient production from an area and the Zürich sunspot number appropriate to that area is derived, and we speculate that the relation is independent of phase in the solar activity cycle. If true, the Sun may give rise to as many as 100 white light coronal transients per month at solar cycle maximum.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153339
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  • 8
    Electronic Resource
    Electronic Resource
    Coronal mass-ejections-kinematics of the 19 December 1973 event (1977)
    Springer
    Solar physics 55 (1977), S. 473-490 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract An eruptive prominence and coronal transient of 19 December, 1973 comprised one of the best-observed coronal mass ejection events during the skylab period (May, 1973–January, 1974). EUV observations show that the pre-eruptive quiescent prominence was (at 8000 K) not appreciably hotter than other quiescent prominences, but EUV radiation from it and its prominence-corona interface was unusually faint. The prominence material was distributed in helical threads which decreased in pitch angle during the early phases of eruption. No region of the prominence was markedly different from any other just prior to and during the eruption. For the first time, the temperature and density of rising prominence material were determined at great heights in the corona. At 3R ⊙, the prominence material was still confined in threads whose temperature and total hydrogen density were 2 × 104 K and ∼1.5 × 109 cm−3, respectively. Shortly after this observation (∼ 7hr after the start of the eruption), the prominence material expanded dramatically. A small portion (≲1%) of the prominence material was observed draining downward near the solar surface late in the event, and we infer that only a small fraction (∼10%) of the pre-eruptive prominence mass was expelled from the Sun. The remainder of the prominence apparently lay outside the instruments' fields of view. The bulk of the material expelled did not originate in the prominence. Both coronal and prominence material accelerated outward during the period of observations. A pre-existing streamer was disrupted by the outflowing material.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152588
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  • 9
    Electronic Resource
    Electronic Resource
    Forerunners: Outer rims of solar coronal transients (1978)
    Springer
    Solar physics 60 (1978), S. 155-170 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The large loop or blob-like transient events viewed in the white-light corona are rimmed by broad regions where the density is slightly enhanced above the pre-transient corona. Every one of the Skylab events studied for which sufficiently good Skylab coronagraph coverage is available shows this effect. The upper boundaries of these ‘forerunners’ blend gradually into the background corona 1 to ≥2R ⊙ above the transients' leading edges. In any single event, the coronal mass enhancement represented by the forerunner comprises up to 25% of the total excess mass present in the coronagraph's field of view and includes a much larger volume of the corona than previously attributed to the underlying transient. We have not yet seen a forerunner without an accompanying transient. Clearly, forerunners must be reckoned with in any proposed models of discrete outward coronal mass motions, because they indicate the presence of disturbed corona far ahead of the denser portions of the event.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152340
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  • 10
    Electronic Resource
    Electronic Resource
    The large coronal transient of 10 June 1973 (1975)
    Springer
    Solar physics 42 (1975), S. 163-177 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract During the 8.5 month flight of the High Altitude Observatory's white light coronagraph on board Skylab, over 100 coronal transients were observed. In this paper we present a description of one well observed loop transient, that of 10 June 1973. The transient apparently resulted from the eruption of a quiescent prominence on the limb; the emergence of a new, bipolar active region near the prominence may have caused the eruptior. The transient's leading edge rose from 3.6 to 5.0 solar radii (R ⊙) from Sun center at approximately 500 km s−1 during the 32 min of coronagraph observations. Material in a pre-existing streamer was swept away by the transient, causing the streamer to disappear. The mass ejected into the corona above a projected height of 2 R ⊙ was ≈ 5.4 × 1015 g, the potential energy associated with the ejected transient material was ⩾7.0 × 1030 erg, and the kinetic energy of the ejected material is estimated as 1.7 × 1030 erg. The 10 June 1973 transient was, in most respects, typical of other loop transients observed by Skylab.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153293
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