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  • 1
    Electronic Resource
    Electronic Resource
    Structure of the extended solar magnetic field and the sunspot cycle variation in cosmic ray intensity (1976)
    [s.l.] : Nature Publishing Group
    Nature 262 (1976), S. 766-768 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] In the photosphere, near sunspot minimum, the sector magnetic fields cover a range in latitude of typically ± 40 (ref. 8), while at 1 AU the comparable range in latitude has been compressed to perhaps ± 15. How is this compression in latitude accomplished? A typical magnitude of the ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/262766a0
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  • 2
    Electronic Resource
    Electronic Resource
    Rigid and differential rotation of the solar corona (1974)
    Springer
    Solar physics 34 (1974), S. 3-10 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The rotation of the solar corona has been studied using recurrence properties of the green coronal line (5303 Å) for the interval 1947–1970. Short-lived coronal activity is found to show the same differential rotation as short-lived photospheric magnetic field features. Long-lived recurrences show rigid rotation in the latitude interval ±57°.5. It is proposed that at least part of the variability of rotational properties of the solar atmosphere may be understood as a consequence of coexistence of differential and rigid solar rotation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149592
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  • 3
    Electronic Resource
    Electronic Resource
    Green corona and solar sector structure (1974)
    Springer
    Solar physics 36 (1974), S. 115-120 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Analysis of the green line corona for the interval 1947–1970 suggests the existence of largescale organization of the emission. The green line emission at high northern latitudes (≈ 40°–60°) is correlated with the emission at high southern latitudes 6, 15 and 24 days later, while the low latitude green corona seems to be correlated on both sides of the equator with no time lag. These coronal features are recurrent with a 27-day period at all latitudes between ± 60 °, and we associate these large-scale structures with the solar magnetic sector structure. The high correlation between northern and southern high-latitude emission at 15 days time lag is explained as a signature of a two-sector structure, while four sectors are associated with the 6 and 24 day peaks.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151551
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  • 4
    Electronic Resource
    Electronic Resource
    The strength of the Sun's polar fields (1978)
    Springer
    Solar physics 58 (1978), S. 225-239 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The magnetic field strength within the polar caps of the Sun is an important parameter for both the solar activity cycle and for our understanding of the interplanetary magnetic field. Measurements of the line-of-sight component of the magnetic field generally yield 0.1 to 0.2 mT near times of sunspot minimum. In this paper we report measurements of the polar fields made at the Stanford Solar Observatory using the Fe i line λ 525.02 nm. We find that the average flux density poleward of 55° latitude is about 0.6 mT peaking to more than 1 mT at the pole and decreasing to 0.2 mT at the polar cap boundary. The total open flux through either polar cap thus becomes about 3 × 1014 Wb. We also show that observed magnetic field strengths vary as the line-of-sight component of nearly radial fields.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157268
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  • 5
    Electronic Resource
    Electronic Resource
    Long term evolution of solar sector structure (1975)
    Springer
    Solar physics 41 (1975), S. 461-475 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The large-scale structure of the solar magnetic field during the past five sunspot cycles (representing by implication a much longer interval of time) has been investigated using the polarity (toward or away from the Sun) of the interplanetary magnetic field as inferred from polar geomagnetic observations. The polarity of the interplanetary magnetic field has previously been shown to be closely related to the polarity (into or out of the Sun) of the large-scale solar magnetic field. It appears that a solar structure with four sectors per rotation persisted through the past five sunspot cycles with a synodic rotation period near 27.0 days, and a small relative westward drift during the first half of each sunspot cycle and a relative eastward drift during the second half of each cycle. Superposed on this four-sector structure there is another structure with inward field polarity, a width in solar longitude of about 100° and a synodic rotation period of about 28 to 29 days. This 28.5 day structure is usually most prominent during a few years near sunspot maximum. Some preliminary comparisons of these observed solar structures with theoretical considerations are given.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00154083
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  • 6
    Electronic Resource
    Electronic Resource
    The Hale solar sector boundary (1976)
    Springer
    Solar physics 49 (1976), S. 177-185 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A Hale solar sector boundary is defined as the half (northern hemisphere or southern hemisphere) of a sector boundary in which the change of sector magnetic field polarity is the same as the change of polarity from a preceding spot to a following spot. Above a Hale sector boundary the green corona has maximum brightness, while above a non-Hale boundary the green corona has a minimum brightness. The Hale portion of a photospheric sector boundary tends to have maximum magnetic field strength, while the non-Hale portion has minimum field strength.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00221492
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  • 7
    Electronic Resource
    Electronic Resource
    The mean magnetic field of the Sun: Observations at Stanford (1977)
    Springer
    Solar physics 54 (1977), S. 353-361 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A solar telescope has been built at Stanford University to study the organization and evolution of large-scale solar magnetic fields and velocities. The observations are made using a Babcock-type magnetograph which is connected to a 22.9 m vertical Littrow spectrograph. Sun-as-a-star integrated light measurements of the mean solar magnetic field have been made daily since May 1975. The typical mean field magnitude has been about 0.15 G with typical measurement error less than 0.05 G. The mean field polarity pattern is essentially identical to the interplanetary magnetic field sector structure (see near the Earth with a 4 day lag). The differences in the observed structures can be understood in terms of a ‘warped current sheet’ model.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00159925
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  • 8
    Electronic Resource
    Electronic Resource
    Comparison of Hα synoptic charts with the large-scale solar magnetic field as observed at Stanford (1977)
    Springer
    Solar physics 55 (1977), S. 63-68 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Two methods of observing the neutral line of the large-scale photospheric magnetic field are compared: (1) neutral line positions inferred from Hα photographs (McIntosh, 1972a, 1975; McIntosh and Nolte, 1975) and (2) observations of the photospheric magnetic field made with low spatial resolution (3′) and high sensitivity using the Stanford magnetograph. The comparison is found to be very favorable.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00150874
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  • 9
    Electronic Resource
    Electronic Resource
    On the supposed anticorrelation of solar polar and equatorial rotation rates (1978)
    Springer
    Solar physics 56 (1978), S. 463-466 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Howard and Harvey (1970) analyzed Mt. Wilson Doppler shifts to obtain a daily measure of the Sun's differential rotation. The data were fitted to give an angular velocity of the form ω = a + b sin2 B + c sin4 B (B = heliographic latitude). Changes in a, b, c were found to be correlated (Howard and Harvey, 1970). Yoshimura (1972) used the anticorrelation of the b and c parameters to infer the existence of large-scale convection. Wolff (1975) used the b-c anticorrelation and a weak correlation between a and b to infer that variations of the Sun's polar and equatorial rotation rates are anticorrelated. In this paper, the anticorrelation of b and c is shown to be due to numerical coupling.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152485
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  • 10
    Electronic Resource
    Electronic Resource
    Seasonal variation and magnitude of the solar sector structure–atmospheric vorticity effect (1975)
    [s.l.] : Nature Publishing Group
    Nature 255 (1975), S. 539-540 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] In the interval from about two days before a boundary is swept past the Earth by the solar wind to about four days after, the vorticity area index2 declined by about 10%, reaching a minimum about one day after the boundary. (The vorticity area index is a measure of the size and prominence of all ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/255539a0
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