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  • 1
    Electronic Resource
    Electronic Resource
    Prediction of coronal structure of the solar eclipse of October 23, 1976 (1976)
    [s.l.] : Nature Publishing Group
    Nature 264 (1976), S. 730-731 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] This disagreement in the direction of the streamers in the outer corona with those observed arose from the early model's8,9 inability to calculate field directions beyond where the solar wind carried out the extended solar magnetic field, approximately one solar radius above the photosphere. A new ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/264730a0
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  • 2
    Electronic Resource
    Electronic Resource
    Prediction of the Coronal Structure for the Solar Eclipse of September 22, 1968 (1968)
    [s.l.] : Nature Publishing Group
    Nature 220 (1968), S. 1211-1213 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Fig. 1. a, Photograph of the corona of November 12,1966, by S. Smith, NASA-Ames "Research Center, b, Drawing of the magnetic structure ofthe corona according to the formalism outlined. The model consists of a "source surface" which, in first approximation, is a sphere concentric with the Sun. ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/2201211a0
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  • 3
    Electronic Resource
    Electronic Resource
    Preliminary Comparison of Predicted and Observed Structure of the Solar Corona at the Eclipse of March 7, 1970 (1970)
    [s.l.] : Nature Publishing Group
    Nature 226 (1970), S. 1130-1131 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] RECENTLY Schatten predicted1 the structure of the corona at the eclipse of March 7, 1970. The prediction was based on a projection onto the celestial plane of the coronal magnetic field resulting from a Green's function solution for the magnetic potential between the photosphere and a spherical ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/2261130a0
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  • 4
    Electronic Resource
    Electronic Resource
    Prediction of the Coronal Structure for the Solar Eclipse of March 7, 1970 (1970)
    [s.l.] : Nature Publishing Group
    Nature 226 (1970), S. 251-251 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] A "source surface" at one solar radius above the photosphere was used in the present prediction, rather than one at 0.6 solar radii as used in the earlier work, to allow for the more active Sun. Comparisons of calculations obtained with this newer value at the end of 1968 agree more closely with ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/226251a0
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  • 5
    Electronic Resource
    Electronic Resource
    Magnetic convection (1973)
    Springer
    Solar physics 33 (1973), S. 305-318 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this paper the process of magnetic convection is studied. It is shown that outside of a radius of about 2 × 105 km, magnetic fields in the Sun may be buoyant. Outside this limit strong field regions tend to rise at the expense of weak field regions which tend to sink. Magnetic convection may be important in magnetic stars and even in the solar interior. A recent calculation of the angular velocity of the Sun provides a period of rotation for the solar core of from 0.5 to 5 days. This calculation requires that the magnetic field extract angular momentum from the solar interior. Magnetic convection thus seems to be required, if this calculation is correct. Furthermore, magnetic convection may transfer heat and thereby possibly change the internal temperature structure of the Sun from what would be expected solely by radiation transfer.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152420
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  • 6
    Electronic Resource
    Electronic Resource
    Large-scale photospheric magnetic field: The diffusion of active region fields (1972)
    Springer
    Solar physics 26 (1972), S. 283-289 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The large-scale photospheric magnetic field has been computed by allowing observed active region fields to diffuse and to be sheared by differential rotation in accordance with the Leighton (1969) magnetokinematic model of the solar cycle. The differential rotation of the computed field patterns as determined by autocorrelation curves is similar to that of the observed photospheric field, and poleward of 20° latitude both are significantly different from the differential rotation of the long-lived sunspots (Newton and Nunn, 1951) used as an input into the computations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00165269
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  • 7
    Electronic Resource
    Electronic Resource
    Group Sunspot Numbers: A New Solar Activity Reconstruction (1998)
    Springer
    Solar physics 179 (1998), S. 189-219 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this paper, we construct a time series known as the Group Sunspot Number. The Group Sunspot Number is designed to be more internally self-consistent (i.e., less dependent upon seeing the tiniest spots) and less noisy than the Wolf Sunspot Number. It uses the number of sunspot groups observed, rather than groups and individual sunspots. Daily, monthly, and yearly means are derived from 1610 to the present. The Group Sunspot Numbers use 65941 observations from 117 observers active before 1874 that were not used by Wolf in constructing his time series. Hence, we have calculated daily values of solar activity on 111358 days for 1610–1995, compared to 66168 days for the Wolf Sunspot Numbers. The Group Sunspot Numbers also have estimates of their random and systematic errors tabulated. The generation and preliminary analysis of the Group Sunspot Numbers allow us to make several conclusions: (1) Solar activity before 1882 is lower than generally assumed and consequently solar activity in the last few decades is higher than it has been for several centuries. (2) There was a solar activity peak in 1801 and not 1805 so there is no long anomalous cycle of 17 years as reported in the Wolf Sunspot Numbers. The longest cycle now lasts no more than 15 years. (3) The Wolf Sunspot Numbers have many inhomogeneities in them arising from observer noise and this noise affects the daily, monthly, and yearly means. The Group Sunspot Numbers also have observer noise, but it is considerably less than the noise in the Wolf Sunspot Numbers. The Group Sunspot Number is designed to be similar to the Wolf Sunspot Number, but, even if both indices had perfect inputs, some differences are expected, primarily in the daily values.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005007527816
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  • 8
    Electronic Resource
    Electronic Resource
    Group Sunspot Numbers: A New Solar Activity Reconstruction (1998)
    Springer
    Solar physics 181 (1998), S. 491-491 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this paper, we construct a time series known as the Group Sunspot Number. The Group Sunspot Number is designed to be more internally self-consistent (i.e., less dependent upon seeing the tiniest spots) and less noisy than the Wolf Sunspot Number. It uses the number of sunspot groups observed, rather than groups and individual sunspots. Daily, monthly, and yearly means are derived from 1610 to the present. The Group Sunspot Numbers use 65941 observations from 117 observers active before 1874 that were not used by Wolf in constructing his time series. Hence, we have calculated daily values of solar activity on 111358 days for 1610–1995, compared to 66168 days for the Wolf Sunspot Numbers. The Group Sunspot Numbers also have estimates of their random and systematic errors tabulated. The generation and preliminary analysis of the Group Sunspot Numbers allow us to make several conclusions: (1) Solar activity before 1882 is lower than generally assumed and consequently solar activity in the last few decades is higher than it has been for several centuries. (2) There was a solar activity peak in 1801 and not 1805 so there is no long anomalous cycle of 17 years as reported in the Wolf Sunspot Numbers. The longest cycle now lasts no more than 15 years. (3) The Wolf Sunspot Numbers have many inhomogeneities in them arising from observer noise and this noise affects the daily, monthly, and yearly means. The Group Sunspot Numbers also have observer noise, but it is considerably less than the noise in the Wolf Sunspot Numbers. The Group Sunspot Number is designed to be similar to the Wolf Sunspot Number, but, even if both indices had perfect inputs, some differences are expected, primarily in the daily values.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1005056326158
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    Paper (German National Licenses)
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  • 9
    Electronic Resource
    Electronic Resource
    Influence of a solar active region on the interplanetary magnetic field (1968)
    Springer
    Solar physics 5 (1968), S. 240-256 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The interplanetary magnetic field has been mapped between 0.4 and 1.2 AU in the ecliptic plane, extrapolating from satellite measurements at 1 AU. The structure within sectors and the evolution of sectors are discussed. The development of a solar active region appears to produce magnetic loops in the interplanetary medium that result in the formation of a new sector.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00147968
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  • 10
    Electronic Resource
    Electronic Resource
    Natural selection in the corona (1993)
    [s.l.] : Nature Publishing Group
    Nature 361 (1993), S. 683-684 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] "HEAT always passes from the hotter to the cooler" according to the old song1 - so why is the Sun's corona hotter, by several million degrees, than the underlying Sun, where all the energy is gen-erated? Jack Scudder has a new suggestion2. Where others have sought to put extra energy into the ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/361683a0
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