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  • 1
    Electronic Resource
    Electronic Resource
    Magnetic field measurements based on the Zeeman splitting of forbidden transitions (1985)
    [S.l.] : American Institute of Physics (AIP)
    Review of Scientific Instruments 56 (1985), S. 855-856 
    Details
    ISSN: 1089-7623
    Source: AIP Digital Archive
    Topics: Physics , Electrical Engineering, Measurement and Control Technology
    Notes: The measurement of the poloidal magnetic field in a tokamak plasma from the Zeeman splitting and polarization of the magnetic dipole radiation from heavy ions is discussed. When viewed from a direction perpendicular to the toroidal field, the effect of the poloidal field on the circularly polarized radiation is detectable using a photoelectric polarimeter.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.1138071
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  • 2
    Electronic Resource
    Electronic Resource
    Solar gradual hard X-ray bursts: Observations and an interpretation
    Amsterdam : Elsevier
    Advances in Space Research 6 (1986), S. 249-252 
    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)90154-7
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  • 3
    Electronic Resource
    Electronic Resource
    A preliminary study of the Extreme Ultraviolet spectroheliograms from Skylab (1973)
    Springer
    Solar physics 33 (1973), S. 265-280 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Some of the first observations obtained with the Naval Research Laboratory's Extreme Ultraviolet Spectrograph (S082A) during the first Skylab mission are presented and compared with magnetograms and other ground-based data. The instrument is a slitless objective-type grating spectrograph covering 170–630 Å and described in Solar Phys. 27, 251 (1972). Chromospheric network, loop prominences, active regions, a flare, limb brightening, XUV bright points, and ‘coronal holes’ are among the phenomena shown and discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152418
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  • 4
    Electronic Resource
    Electronic Resource
    Observations of the horizontal velocity field surrounding sunspots (1972)
    Springer
    Solar physics 25 (1972), S. 98-103 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract During the summer and fall of 1971, Doppler spectroheliograms were obtained for several sunspots located near the solar limb. These observations confirm a previous result based on the study of only a few sunspots that in the plage-free photosphere surrounding sunspots the spatially-averaged, horizontal flow tends to be outward at 0.5–1.0 km s−1 for distances typically 10000–20000 km beyond the outer boundary of the penumbra. It is suggested that these material motions are the means by which small-scale fragments of magnetic flux are carried away from sunspots.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155747
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  • 5
    Electronic Resource
    Electronic Resource
    Measurements of the oscillatory and slowly-varying components of the solar velocity field (1971)
    Springer
    Solar physics 18 (1971), S. 379-384 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Spectroheliograms with high spatial resolution are presented to illustrate the decomposition of the solar velocity field into its oscillatory and slowly-varying components. An analysis of data obtained in the lines Fei λ 5434 and Feii λ 4924 yield essentially the same principal results: (1) Spectroheliograms of the oscillatory component have a mottled appearance of rising and falling elements ranging from 2000 km to 3000 km in size. These elements oscillate vertically with a period in the range 275–300 s and an amplitude of 0.5 km/s. Although most oscillations last two cycles some have been observed for as many as four cycles. (2) Spectroheliograms of the slowly-varying component show a velocity granulation pattern whose spatial properties correspond closely to those of the photospheric granulation visible on direct photographs of the Sun. The velocity granules are approximately 1000 km in diameter and rise relative to their intergranular spaces with speeds that are typically 0.6 km/s, but which may occasionally be as large as 0.9 km/s. Most velocity granules seem to live for at least 10 min with many lasting 10–30 min, and a few of the biggest and fastest moving lasting 30 min to 1 hr. It is concluded that Spectroheliograms of the slowly-varying component represent the velocity field of the photospheric granulation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149059
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  • 6
    Electronic Resource
    Electronic Resource
    Energy released by the interaction of coronal magnetic fields (1976)
    Springer
    Solar physics 47 (1976), S. 173-180 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Comparisons between coronal spectroheliograms and photospheric magnetograms are presented to support the idea that as coronal magnetic fields interact, a process of field line reconnection usually takes place as a natural way of preventing magnetic stresses from building up in the lower corona. This suggests that the energy which would have been stored in stressed fields is continuously released as kinetic energy of material being driven aside to make way for the reconnecting fields. However, this kinetic energy is negligible compared to the thermal energy of the coronal plasma. Therefore, it appears that these slow adjustments of coronal magnetic fields cannot account for even the normal heating of the corona, much less the energetic events associated with solar flares.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152254
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  • 7
    Electronic Resource
    Electronic Resource
    An improved measurement of a spectrogram of a ‘gap’ (1977)
    Springer
    Solar physics 51 (1977), S. 61-64 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A spectrogram of the 5250 Å region previously obtained during a period of excellent seeing has been remeasured and calibrated by reference to the preliminary KPNO photometric atlas. This analysis, using the logarithm of opacitance instead of an H-D plot, has reduced some of the effects of scattered light and shows greater facular line contrast.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00240445
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  • 8
    Electronic Resource
    Electronic Resource
    Extreme ultraviolet observations of coronal holes (1978)
    Springer
    Solar physics 56 (1978), S. 125-151 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Extreme-ultraviolet Skylab and ground-based solar magnetic field data have been combined to study the origin and evolution of coronal holes. It is shown that holes exist only within the large-scale unipolar magnetic cells into which the solar surface is divided at any given time. A well-defined boundary zone usually exists between the edge of a hole and the neutral line which marks the edge of its magnetic cell. This boundary zone is the region across which a cell is connected by magnetic arcades with adjacent cells of opposite polarity. Three pieces of observational evidence are offered to support the hypothesis that the magnetic lines of force from a hole are open. Kitt Peak magnetograms are used to show that, at least on a relative scale, the average field strengths within holes are quite variable, but indistinguishable from the field strengths in other quiet parts of the Sun's surface. Finally it is shown that the large, equatorial holes characteristic of the declining phase of the last solar cycle during Skylab (1973–74) were all formed as a result of the mergence of bipolar magnetic regions (BMR's), confirming an earlier hypothesis by Timothy et al. (1975). Systematic application of this model to the different aspects of the solar cycle correctly predicts the occurrence of both large, equatorial coronal holes (the ‘M-regions’ which cause recurrent geomagnetic storms) and the polar cap holes.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152639
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  • 9
    Electronic Resource
    Electronic Resource
    A survey of coronal holes and their solar wind associations throughout sunspot cycle 20 (1978)
    Springer
    Solar physics 56 (1978), S. 161-183 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract To gain insight into the relationships between solar activity, the occurrence and variability of coronal holes, and the association of such holes with solar wind features such as high-velocity streams, a study of the period 1963–1974 was made. This period corresponds approximately with sunspot cycle 20. The primary data used for this work consisted of X-ray and XUV solar images obtained from rockets. The investigation revealed that: (1) The polar coronal holes prominent at solar minimum, decreased in area as solar activity increased and were small or absent at maximum phase. This evolution exhibited the same phase difference between the two hemispheres that was observed in other indicators of activity. (2) During maximum, coronal holes occurred poleward of the sunspot belts and in the equatorial region between them. The observed equatorial holes were small and persisted for one or two solar rotations only; some high latitude holes had lifetimes exceeding two solar rotations. (3) During 1963–74 whenever XUV or X-ray images were available, nearly all recurrent solar wind streams of speed ⩾500 km s−1 were found associated with coronal holes at less than 40° latitude; however some coronal holes appeared to have no associated wind streams at the Earth.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152641
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  • 10
    Electronic Resource
    Electronic Resource
    Radio and visible-light observations of a coronal arcade transient (1984)
    Springer
    Solar physics 90 (1984), S. 161-176 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We discuss simultaneous visible-light and radio observations of a coronal transient that occurred on 9 April, 1980. Visible-light observations of the transient and the associated erupting prominence were available from the Coronagraph/Polarimeter carried aboard SMM, the P78-1 coronagraph, and from the Haleakala Observatory. Radio observations of the related type III-II-IV bursts were available from the Clark Lake and Culgoora Observatories. The transient was extremely complex; we suggest that an entire coronal arcade rather than just a single loop participated in the event. Type III burst sources observed at the beginning of the event were located along a nearby streamer, which was not disrupted, but was displaced by the outmoving loops. The type II burst showed large tangential motion, but unlike such sources usually do, it had no related herringbone structure. A moving type IV burst source can be associated with the most dense feature of the white-light transient.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153792
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