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  • SOLAR PHYSICS  (7)
  • 1
    Publication Date: 2014-08-21
    Description: Several methods for cloud cover estimation are described relevant to assessing the performance of a ground-based network of solar observatories. The methods rely on ground and satellite data sources and provide meteorological or climatological information. One means of acquiring long-term observations of solar oscillations is the establishment of a ground-based network of solar observatories. Criteria for station site selection are: gross cloudiness, accurate transparency information, and seeing. Alternative methods for computing this duty cycle are discussed. The cycle, or alternatively a time history of solar visibility from the network, can then be input to a model to determine the effect of duty cycle on derived solar seismology parameters. Cloudiness from space is studied to examine various means by which the duty cycle might be computed. Cloudiness, and to some extent transparency, can potentially be estimated from satellite data.
    Keywords: SOLAR PHYSICS
    Type: Solar Seismology from Space.; p 305-312
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  • 2
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    In:  Other Sources
    Publication Date: 2019-06-27
    Description: All active regions are born as Emerging Flux Regions (EFRs) which appear in H alpha as two small plages of opposite polarity connected by parallel dark arches. After a brief review of the properties of EFRs, new observations of the birth of an EFR and apparent subsequent field reconnection are reported. Fluxrope theories are reviewed, the appearance of EFRs is predicted, and this picture is then modified on the basis of high resolution observations. One arrives at a model of this phenomenon that encompasses relevant aspects such as the axial tilt of spot groups, the observed 'rotation' of EFRs as they emerge, and the fact that EFR fluxtubes are made up of many discrete strands.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 43; Aug. 197
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  • 3
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    In:  Other Sources
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 41; Mar. 197
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  • 4
    Publication Date: 2019-06-27
    Description: OSO-7 observations of the first five Lyman lines and the Lyman continuum of He II are given for the quiet sun, a coronal hole, prominences, filaments, and the flare of August 7, 1972. These data are calibrated and given in specific intensity units together with color and brightness temperatures for the He II continuum. It is found that He II is overionized in all features except the flare and that the continuum is formed at temperatures near 14,000 K. The He II-He III ionization equilibrium appears to be dominated by photoionizations and radiative recombinations. Schematic calculations for realistic chromosphere and transition-region models can account for the observed intensities of Ly-beta through Ly-epsilon, the Lyman continuum, and its color temperature. To account for the intensity of Ly-alpha, either an implausible 100-km plateau at temperatures near 80,000 K is needed or, more likely, the diffusion-enhanced collisional excitation should be incorporated into the models.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Jan. 15
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  • 5
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: PB-284726 , Astrophysical Journal; vol. 222
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  • 6
    Publication Date: 2019-08-28
    Description: The center-to-limb variation of the He II 304- and 256-A lines and He I 584- and 537-A lines is derived for different solar features, but averaged over the chromospheric supergranulation structure. The general trend is for limb brightening in quiet-sun regions, limb neutrality in unipolar magnetic regions (UMR), and limb darkening in polar coronal holes. The center-to-limb behavior in these optically thick emission lines indicates collisional excitation and decreasing transition-region temperature gradients with respect to optical depth in the sequence quiet sun to UMR to coronal hole.
    Keywords: SOLAR PHYSICS
    Type: PB80-118110 , Astrophysical Journal; vol. 220
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  • 7
    Publication Date: 2019-07-13
    Description: Digital image processing of eight solar flare events was performed using the Video Information Communication and Retrieval language in order to study moving emission fronts, flare halos, and Moreton waves. The techniques used include contrast enhancement, isointensity contouring, the differencing of images, spatial filtering, and geometrical registration. The spatial extent and temporal behavior of the faint phenomena is examined along with the relation of the three types of phenomena to one another. The image processing techniques make possible the detailed study of the history of the phenomena and provide clues to their physical nature.
    Keywords: SOLAR PHYSICS
    Type: Conference on Applications of Digital Image Processing to Astronomy; Aug 20, 1980 - Aug 22, 1980; Pasadena, CA
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