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  • 1
    Electronic Resource
    Electronic Resource
    Large-Scale Dynamics of the Interstellar Medium (1974)
    Palo Alto, Calif. : Annual Reviews
    Annual Review of Astronomy and Astrophysics 12 (1974), S. 113-133 
    Details
    ISSN: 0066-4146
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1146/annurev.aa.12.090174.000553
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  • 2
    Electronic Resource
    Electronic Resource
    Structure and Dynamics of the Interstellar Medium (1968)
    Palo Alto, Calif. : Annual Reviews
    Annual Review of Astronomy and Astrophysics 6 (1968), S. 165-194 
    Details
    ISSN: 0066-4146
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1146/annurev.aa.06.090168.001121
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  • 3
    Electronic Resource
    Electronic Resource
    Models of cosmic maser sources (1976)
    Springer
    Astrophysics and space science 39 (1976), S. L19 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648350
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  • 4
    Electronic Resource
    Electronic Resource
    Formation of stellar associations (1970)
    Springer
    Astrophysics and space science 7 (1970), S. 489-493 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Rayleigh-Taylor instability forms massive complexes. When 1021 atoms cm−2 are gathered, X-rays which heat the gas and UV-rays which ionize carbon are absorbed. A layer should appear with temperatures as low as 6 K and density to 4×103 cm−3. Finally the layer is fragmented into stars whose masses may even be less than one solar mass. The temperature of the layer should increase with time because part of free carbon is gradually absorbed by dust. Therefore more massive stars should appear after less massive stars. The stars which are formed kept near the layer by its gravitation. When their total mass becomes comparable with the mass of the layer, they should fall to the galactic plane in agreement with observed proper motions of several studied stellar systems.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653284
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  • 5
    Electronic Resource
    Electronic Resource
    Nature of the fine structure of the middle chromosphere (1971)
    Springer
    Solar physics 20 (1971), S. 286-294 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Fine dark Hα filaments ‘fibrils’ form at the limb, apparently in most of the middle chromosphere corresponding to an altitude between 1500–2000 km and 4000 km. The space in between filaments is corona and the transition layer. The ‘cool’ gas in fibrils is protected by the magnetic field against the conductive flux out of the ‘hot’ corona. Therefore the fibrils stretch up to 4000 km where their temperature is about 18 000 K and the density about 5 × 109 cm−3. The gas in the fibrils is ionized by electronic collisions and by the external ultraviolet radiation. The second level of the hydrogen atoms in fibrils is populated by recombinations, electronic collisions and by Ly-α quanta. The calculated optical thickness of the fibrils in Hα is about 1, it explains the absorption features on the spectroheliograms. The gas pressure in fibrils is lower than the coronal pressure, and the pressure equilibrium is achieved by a magnetic field of about 1.5–2 G. In the active regions the photospheric fields are stronger, therefore the fibrils in active regions are wider and show more contrast. The emission of the fibrils at the limb is explained by the scattering of the solar radiation. The temperature in arches reaching as high as 5000–6000 km, is stabilized near the top by the HeII emission. Thus the middle chromosphere is essentially a collection of magnetic arches.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00159757
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  • 6
    Electronic Resource
    Electronic Resource
    Origin of quiescent prominences (1971)
    Springer
    Solar physics 17 (1971), S. 44-49 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract For stable equilibrium, prominences must be supported with magnetic lines of force leaning upon the photosphere and concave in their tops; however the general structure may be more complicated. If such a field appears in the corona, the heating of the gas near the upper pit should be low, because Alfvén and slow waves do not propagate across magnetic lines and fast mode waves attenuate because of refraction. The gas of the corona, distributed along the magnetic lines tube, cannot keep balance, it should flow down in the pit, condense there and fall down into the chromosphere in some places. The prominence, therefore, originates in the matter of the chromosphere which is situated at the other end of the magnetic lines and flows through the corona under the effect of a siphon-type mechanism. A similar mechanism for chromospheric structures was earlier suggested by Meyer and Schmidt. A stationary stream along the tube has been calculated with allowance for the heat conductivity and radiative cooling of the corona gas. The stream is subsonic and is about 1015 cm−2 sec−1 which corresponds to the prominence formation time of the order of a day.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152860
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  • 7
    Electronic Resource
    Electronic Resource
    Problems of solar flare theory (1977)
    Springer
    Radiophysics and quantum electronics 20 (1977), S. 904-909 
    Details
    ISSN: 1573-9120
    Source: Springer Online Journal Archives 1860-2000
    Topics: Electrical Engineering, Measurement and Control Technology , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF01356760
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