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  • 1
    Electronic Resource
    Electronic Resource
    Type III radio bursts in the outer corona (1969)
    Springer
    Solar physics 8 (1969), S. 388-397 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Type III solar radio bursts observed from 3.0 to 0.45 MHz with the ATS-II satellite over the period April–October 1967 have been analyzed to derive two alternative models of active region streamers in the outer solar corona. Assuming that the bursts correspond to radiation near the electron plasma frequency, ‘pressure equilibrium’ arguments lead to streamer Model I in which the streamer electron temperature derived from collision damping time falls off much more rapidly than in the ‘average’ corona and the electron density is as much as 25 times the average coronal density at heights of 10 to 50 solar radii (R ⊙). In Model II the streamer electron temperature is assumed to equal the average coronal temperature, giving a density enhancement which decreases from a factor of 10 close to the Sun to less than a factor of two at large distances (〉 1/4 AU). When the burst frequency drift is interpreted as resulting from the outward motion of a disturbance that stimulates the radio emission, Model I gives a constant velocity of about 0.35c for the exciting disturbance as it moves to large distances, while with Model II, there is a decrease in the velocity to less than 0.2c beyond 10 R ⊙.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155385
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Hectometric and kilometric solar radio emission observed from satellites in August 1972 (1976)
    Springer
    Space science reviews 19 (1976), S. 511-531 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Type II, III, and continuum solar radio events, as well as intense terrestrial magnetospheric radio emissions, were observed at low frequencies (10 MHz to 30 kHz) by the IMP-6 satellite during the period of high solar activity in August 1972. This review covers briefly the unique direction finding capability of the experiment, as well as a detailed chronology of the low frequency radio events, and, where possible, their association with both groundbased radio observations and solar flares. The attempted observation of solar bursts in the presence of intense magnetospheric noise may, as illustrated, lead to erroneous results in the absence of directional information. The problem of assigning an electron density scale and its influence on determining burst trajectories is reviewed. However, for the disturbed conditions existing during the period in question, we feel that such trajectories cannot be determined accurately by this method. In conclusion, the capabilities, limitations, and observing programs of present and future satellite experiments are briefly discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00210640
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    Paper (German National Licenses)
    Fulltext
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