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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
    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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  • 3
    Electronic Resource
    Electronic Resource
    Average photospheric poloidal and toroidal magnetic field components near solar minimum (1979)
    Springer
    Solar physics 61 (1979), S. 233-245 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Average (over longitude and time) photospheric magnetic field components are derived from 3′ Stanford magnetograms made near the solar minimum of cycle 21. The average magnetograph signal is found to behave as the projection of a vector for measurements made across the disk. The poloidal field exhibits the familiar dipolar structure near the poles, with a measured signal in the line Fe i λ 5250 Å of ≈ 1 G. At low latitudes the poloidal field has the polarity of the poles, but is of reduced magnitude (≈ 0.1 G). A net photospheric toroidal field with a broad latitudinal extent is found. The polarity of the toroidal field is opposite in the nothern and southern hemispheres and has the same sense as subsurface flux tubes giving rise to active regions of solar cycle 21. These observations are used to discusse large-scale electric currents crossing the photosphere and angular momentum loss to the solar wind.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00150408
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  • 4
    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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  • 5
    Electronic Resource
    Electronic Resource
    The sun's magnetic sector structure (1975)
    Springer
    Solar physics 45 (1975), S. 83-91 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The synoptic appearance of solar magnetic sectors is studied using 454 sector boundaries observed at Earth during 1959–1973. The sectors are clearly visible in the photospheric magnetic field. Sector boundaries can be clearly identified as north-south running demarcation lines between regions of persistent magnetic polarity imbalances. These regions extend up to about 35 ° of latitude on both sides of the equator. They generally do not extend into the polar caps. The polar cap boundary can be identified as an east-west demarcation line marking the poleward limit of the sectors. The typical flux imbalance for a magnetic sector is about 4 × 1021 Mx.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152219
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  • 6
    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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  • 7
    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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  • 8
    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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  • 9
    Electronic Resource
    Electronic Resource
    A model combining the polar and the sector structured solar magnetic fields (1974)
    Springer
    Solar physics 37 (1974), S. 157-172 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A phenomenological model of the interplay between the polar magnetic fields of the Sun and the solar sector structure is discussed. Current sheets separate regions of opposite polarity and mark the sector boundaries in the corona. The sheets are visible as helmet streamers. The solar sector boundary is tilted with respect to central meridian, and boundaries with opposite polarity change are oppositely tilted. The tilt of a given type of boundary [(+, −) or (−, +)] changes systematically during the sunspot cycle as the polarity of the polar fields reverses. Similar reversals of the position of the streamers at the limbs takes place. If we consider (a) a sunspot cycle where the northern polar field is inward (−) during the early part of the cycle and (b) a (+, −) sector boundary at central meridian then the model predicts the following pattern; a streamer at high northern latitudes should be observed over the west limb together with a corresponding southern streamer over the east limb. The current sheet runs now NW-SE. At sunspot maximum the boundary is more in the N-S direction; later when the polar fields have completed their reversal the boundary runs NE-SW and the northern streamer should be observed over the east limb and the southern streamer over the west limb. Observational evidence in support of the model is presented, especially the findings of Hansen, Sawyer and Hansen and Koomen and Howard that the K-corona is highly structured and related to the solar sector structure.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157852
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  • 10
    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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