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  • 1
    Electronic Resource
    Electronic Resource
    Electron groups traced from the sun to 1 AU (1991)
    Springer
    Solar physics 136 (1991), S. 361-377 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We trace electrons from the Sun by a variety of proxy methods - solar flare positions, and metric and kilometric type III radio bursts from the Sun until they can be observed in situ as electrons at the ISEE-3 spacecraft. Our study extends over the period of operation of the electron experiment on ISEE-3 from August 1978 to November 1979. By carefully restricting timing within the data sets involved, we find a peak in the number of flares associated with in situ electrons near 60° west solar longitude. This peak shows that type III bursts can be fairly limited in spatial extent, and that the best connection with the solar surface to the flare is along the Archimedean magnetic field spiral. We use this spatial determination to define an ‘average’ beam shape for an event. We assume this average beam shape to be representative of the distribution in space of each electron group. The electron numbers at 2 and 29–45 keV energies combined with this average beam shape are used to approximate the total numbers of electrons and energy per burst for individual events. We find that the total number of electrons and total energy for events varies significantly with flare type; that on the average brighter flares are associated with more electrons.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00146542
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Solar and interplanetary observations of the mass ejection on 7 May, 1979 (1988)
    Springer
    Solar physics 115 (1988), S. 327-343 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present observations of a mass ejection that was observed by five different instruments along its way from the solar surface to more than 100 solar radii. The instruments involved are the ground-based Hα coronagraph at Wrocław, the white-light SOLWIND coronagraph on board the P78-1 satellite, zodiacal light photometers of the HELIOS B spacecraft, in situ plasma detectors and magnetometers on board the HELIOS B spacecraft, and interplanetary scintillation measurements on the ground. By using a CAT-scan analysis of the images obtained by the SOLWIND coronagraph near the Earth and HELIOS B photometers placed at 0.3 AU perpendicular to the Earth-Sun line, we have been able to get a three-dimensional density reconstruction of the mass ejection and fit the best velocity curve for its propagation. Although problems exist in smoothly joining the height-time curves (for instance, we had to reduce the brightness of the SOLWIND data by more than a factor of two to make the data sets agree photometrically), both this analysis and direct measurements by the other experiments clearly indicate higher speeds at greater distances from the Sun. The plasma acceleration in this case was obviously not limited only to distances within 3 R 0 , as is usually the case, but continued beyond the outer limit of the coronagraph view at ∼ 8 R 0 .
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00148732
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  • 3
    Electronic Resource
    Electronic Resource
    Giant solar arches and coronal mass ejections in November 1980 (1989)
    Springer
    Solar physics 122 (1989), S. 131-143 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Using data from the SOLWIND coronagraph and photometers aboard HELIOS-A we examine coronal mass ejections from an active region which produced a series of giant post-flare coronal arches. HXIS X-ray observations reveal that in several cases underlying flares did not disrupt these arch structures, but simply revived them, enhancing their temperature, density and brightness. Thus we are curious to know how these quasi-stationary X-ray structures could survive in the corona in spite of recurrent appearances of powerful dynamic flares below them. We have found reliable evidence that two dynamic flares which clearly revived the preexisting giant arch were not associated with any mass ejection. After two other flares, which were associated with mass ejections, the arch might have been newly formed when the ejection was over. In one of these cases, however, the arch had typical characteristics of a revived structure so that it is likely that it survived a powerful mass ejection nearby. In a magnetic configuration of the arch which results from potential-field modelling (Figure 1(b)) such a survival seems possible.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00162831
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  • 4
    Electronic Resource
    Electronic Resource
    A metric type III burst asymmetry relative to simple bipolar active regions (1986)
    Springer
    Solar physics 105 (1986), S. 123-132 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Metric type III solar radio burst positions are compared spatially and temporally to underlying active region geometry. The positions of these radio bursts have an asymmetric location distribution relative to simple bipolar regions. The type III bursts show a tendency to occur nearer the leading active region - an association shown before from type III burst and magnetic field polarity measurements. The type III bursts also generally occur to the left of the outward to inward directed magnetic field. The asymmetry relative to the outward directed magnetic field has a sense that is consistent with a mechanism of type III burst production that involves a pre-existing coronal current system situated between expanding closed and open magnetic field lines.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00156382
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  • 5
    Electronic Resource
    Electronic Resource
    Forerunners: Early coronal manifestations of solar mass ejection events (1981)
    Springer
    Solar physics 73 (1981), S. 133-144 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Coronal ejection transients viewed with the white light coronagraph on Skylab are studied from the times of their very earliest manifestations for clues to their origin. Excess coronal mass with a configuration like that of the eventual transient is seen in twelve events prior to the transient's associated near-surface Hα eruption or flare. In seven of the events, data are adequate to observe the rates of outward mass motion of coronal material prior to their surface manifestations. The observations place severe constraints on different solar mass ejection mechanisms because they spread the process responsible for the ejection over a larger region of the corona and over a longer period of time than normally considered. The observations suggest the corona is an active participant in the ejection that begins with the acceleration of the outer portion of a preexisting structure and ends with the obvious surface manifestation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153150
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  • 6
    Electronic Resource
    Electronic Resource
    A comparison of type III metric radio bursts and global solar potential field models (1981)
    Springer
    Solar physics 73 (1981), S. 183-190 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We compare evidence of coronal magnetic fields from polarized metric type III radio bursts with (a) global potential field models, (b) direct averages of the observed photospheric magnetic field, and (c) Hα synoptic charts. The comparison clearly indicates both that the principal aspects of type III burst radiation are understood and that global potential field models are a significantly more accurate representation of coronal magnetic field structure than either the large-scale photospheric field or Hα synoptic charts.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153153
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  • 7
    Electronic Resource
    Electronic Resource
    A CME mass distribution derived from SOLWIND coronagraph observations (1993)
    Springer
    Solar physics 148 (1993), S. 359-370 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Using estimates of the masses of nearly 1000 CMEs observed by SOLWIND from Howardet al. (1985), we re-plot the numbers of CMEs as a function of CME mass on a log-linear plot. The plot is significant in that it shows a linear trend over more than a decade of CME masses. The plot indicates a simple form for the distribution of the CME masses and allows an easy determination of the total mass ejected into the solar wind in the form of CMEs. We find that approximately 16% of the solar wind at solar maximum can be comprised of CME mass. There is no indication that the numbers of low-mass CMEs increase in number above the trend set by the more massive ones. Specifically, there is no increase in the numbers of small CMEs such that the whole of the solar wind can be comprised of them.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00645095
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  • 8
    Electronic Resource
    Electronic Resource
    Coronal mass ejection associated with the stationary post-flare arch of 21–22 May 1980 (1986)
    Springer
    Solar physics 103 (1986), S. 399-408 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract By using a combination of X-ray (HXIS), Hα (Haleakala), white-light corona (Solwind), and zodiacal light (Helios) images on 21–22 May, 1980 we demonstrate, and try to explain, the co-existence of a coronal mass ejection with a stationary post-flare coronal arch. The mass ejection was seen, both by Solwind and Helios, in prolongation of the path of a powerful spray, whereas the active region filament did not erupt. A tentative comparison is made with other occurrences of stationary, or quasi-stationary post-flare coronal arches.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00147838
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  • 9
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    Electron groups traced from the sun to 1 AU (1991)
    Springer
    Details
    Publication Date: 1991-12-01
    Print ISSN: 0038-0938
    Electronic ISSN: 1573-093X
    Topics: Physics
    Published by Springer
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  • 10
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    Giant solar arches and coronal mass ejections in November 1980 (1989)
    Springer
    Details
    Publication Date: 1989-03-01
    Print ISSN: 0038-0938
    Electronic ISSN: 1573-093X
    Topics: Physics
    Published by Springer
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