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  • 1
    Electronic Resource
    Electronic Resource
    Springer
    Cell & tissue research 204 (1979), S. 343-354 
    ISSN: 1432-0878
    Keywords: Hypothalamo-pituitary afferents ; Vasopressin ; Somatostatin ; 3-D Reconstruction
    Source: Springer Online Journal Archives 1860-2000
    Topics: Biology , Medicine
    Notes: Summary A three-dimensional reconstruction of the rat's hypothalamo-neurohypophysial system, depicting the neurons that project to the neurointermediate lobe of the pituitary, has been made by using retrograde transport of horseradish peroxidase injected into the neuro-intermediate lobe and by using immunocytochemistry with antisera to vasopressin and somatostatin. The overall picture illustrates the neurons situated in the walls of a pair of ill-defined cone-shaped tunnels, the apices pointing anteriorly. Among the neuronal aggregates in the tunnel wall two, the paraventricular and forniceal nuclei, appear similar in shape but clearly separated by a gap of at least 150 μm. Many of the vasopressin-positive neurons lie in the same nuclear aggregates with two notable exceptions: the suprachiasmatic nucleus contains many vasopressin-positive cells but does not project to the pituitary, and the forniceal aggregate, which does project to the pituitary, contains no vasopressin-positive cells. Somatostatin-positive cells are situated close to the third ventricle, and their size is intermediate between parvocellular and magnocellular. Cell counts show only half the cells in the system lying in the supraoptic and paraventricular nuclei, the rest being in “accessory nuclei”.
    Type of Medium: Electronic Resource
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  • 2
    Publication Date: 2011-08-19
    Description: In the present study of the microwave and hard X-ray characteristics of 13 solar flares emitting microwave fluxes greater than 500 solar flux units, simultaneous 3-35 GHz and hard X-ray observations were conducted in the 30-500 keV energy range. An analysis is conducted to determine whether the same distribution of energetic electrons can explain both emissions; tests for any correlations between them yield results suggesting that optically thick microwave emission, near the peak frequency, originates in the same electron population that produces the hard X-rays. A single temperature model and a multitemperature model were tested for consistency with the coincident X-ray and microwave spectra at microwave burst maximum; neither model, however, attempts to explain the high frequency component of the microwave spectrum.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 96; 339-356
    Format: text
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  • 3
    Publication Date: 2019-06-28
    Description: The microwave and hard X-ray charateristics of 13 solar flares that produced microwave fluxes greater than 500 Solar Flux Units were analyzed. These Great Microwave Bursts were observed in the frequency range from 3 to 35 GHz at Berne, and simultaneous hard X-ray observations were made in the energy range from 30 to 500 keV with the Hard X-Ray Burst Spectrometer on the Solar Maximum Mission spacecraft. The principal aim of this analysis is to determine whether or not the same distribution of energetic electrons can explain both emissions. Correlations were found between respective temporal characteristics and, for the first time, between microwave and hard X-ray spectral characteristics. A single-temperature and a multi-temperature model from the literature were tested for consistency with the coincident X-ray and microwave spectra at microwave burst maximum. Four events are inconsistent with both of the models tested, and neither of the models attempts to explain the high-frequency part of the microwave spectrum. A model in which the emissions above and below the peak frequency originate in two different parts of a diverging magnetic loop is proposed. With this model the entire microwave spectrum of all but one of the events is explained.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-85052 , NAS 1.15:85052
    Format: application/pdf
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  • 4
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Res. in the Space Sci., v. 2; 6 p
    Format: text
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  • 5
    Publication Date: 2019-06-27
    Description: Plastic and glass track detectors on rockets and Apollo spacecraft have been used to determine the composition of particles from He to Ni at energies from 0.1 to 50 MeV per nucleon in several solar flares of widely varying intensities. At low energies the composition of solar particles is enriched in heavy elements by an amount, relative to the asymptotic high-energy composition, that increases with atomic number from Z = 2 up to at least Z = 50, that decreases with energy, and that varies from flare to flare. At high energies (usually beyond an energy of 5 to 20 MeV per nucleon) the composition becomes independent of energy and, though somewhat variable from flare to flare, approximates the composition of the solar atmosphere. A table of abundances of the even-Z elements from He to Ni (plus N) in solar particles is constructed by averaging the asymptotic high-energy abundances in several flares.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 195; Jan. 1
    Format: text
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