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  • 1
    Electronic Resource
    Electronic Resource
    Type III solar radio burst storms observed at low frequencies (1970)
    Springer
    Solar physics 15 (1970), S. 222-233 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Storms of type III solar radio bursts observed from 5.4 to 0.2 MHz, indicate the quasicontinuous production of type III events observable for a half solar rotation but persisting in some cases for well over a complete rotation. The characteristics of these storms, including the dependance of occurrence and apparent drift rates on the disc position of the associated active region are discussed. The drift rate dependance is shown to be a consequence of the propagation time of emission from the source to the observer. The occurrence rate of a burst every 10 sec observed near CMP implies that if this level of activity persists, then about a quarter of a million exciter packets are released into the interplanetary plasma during a complete rotation. Storm bursts are less intense than most isolated type III's and occur over a more limited frequency range. There appears to be a very close relation between these storms and decametric continuum.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149487
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  • 2
    Electronic Resource
    Electronic Resource
    Type III solar radio burst storms observed at low frequencies (1970)
    Springer
    Solar physics 15 (1970), S. 433-445 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Storms of type III solar radio bursts observed from 5.4 ot 0.2 MHz consist of a quasi-continuous production of type III events observable for half a solar rotation but persisting in some cases for well over a complete rotation (Fainberg and Stone, 1970). The observed burst drift rates are a function of the heliographic longitude of the associated active region. This apparent drift rate dependence is a consequence of the radio emission propagation time from source to observer. Based on this dependence, a least squares analysis of 2500 drift rates between frequencies in the 2.8 to 0.7 MHz range yields an average exciter speed of 0.38 c for the height range from approximately 11 to 30 R ⊙. In conjunction with the available determinations of exciter speeds of 0.33 c close to the sun, i.e. less than 3 R ⊙, and with in situ measurements of 40 keV solar electrons by space probes, the present results suggest that the exciters are electron packets which propagate with little deceleration over distances of at least 1 AU.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151850
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  • 3
    Electronic Resource
    Electronic Resource
    A new method for reconstructing type III trajectories (1986)
    Springer
    Solar physics 106 (1986), S. 397-401 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A local density approximation (LDA) method is developed for reconstructing the trajectories of type III radio bursts through the interplanetary medium. The method uses the measured source directions and the measured frequency drift rates of the type III burst to determine the locations of the radio source in the interplanetary medium at consecutive frequency levels. The technique is used to reconstruct the trajectory of an actual type III burst and the results are compared to the trajectory obtained from the global density law method. The LDA method represents an improvement in that it utilizes more observed data on the type III burst and that it takes full account of the local density variations at the source locations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00158504
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  • 4
    Electronic Resource
    Electronic Resource
    Characteristics of type III exciters derived from low frequency radio observations (1973)
    Springer
    Solar physics 31 (1973), S. 501-511 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Low frequency radio observations (2.8 MHz-67 kHz) from the RAE-1 and IMP-6 satellites allow the tracking of type III solar burst exciters out to large distances from the Sun (of the order of 1 AU). A study of the interaction processes between the exciter and the interplanetary medium was made using the time-intensity profiles of the radio emission. We have investigated the change in exciter length with distance from the Sun, and the resulting exciter velocity dispersion which can be deduced from this change. From detailed measurements on 35 simple bursts we have found that the exciter length increases at a faster rate than a constant velocity dispersion would give. We have also investigated the damping of the radio emission and have concluded that some current theories of the damping mechanism give results which are not consistent with the low frequency observations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00152825
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  • 5
    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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  • 6
    Electronic Resource
    Electronic Resource
    Evidence for halo-like radio sources from kilometric type III burst observations (1990)
    Springer
    Solar physics 125 (1990), S. 371-388 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The radio azimuths for many kilometric type III bursts that originate near or behind the limb of the Sun are observed to drift far to the east or far to the west of the spacecraft-Sun line. It is shown that the behavior of the observed burst parameters for these events corresponds to the response of a spinning dipole antenna to halo-like sources of radiation around the Sun. Our results provide evidence for a previous suggestion that behind-the-limb type III events should appear as halo-like sources of radiation to an observer on the opposite side of the Sun, due to scattering of the radiation from the primary source back around the Sun.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00158413
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  • 7
    Electronic Resource
    Electronic Resource
    A comparison of type III solar radio burst theories using satellite radio observations and particle measurements (1971)
    Springer
    Solar physics 21 (1971), S. 198-203 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The required electron density to excite a type III solar burst can be predicted from different theories, using the low frequency radio observations of the RAE-1 satellite. Electron flux measurements by satellite in the vicinity of 1 AU then give an independent means of comparing these predicted exciter electron densities to the measured density. On this basis, one theory predicts the electron density in closest agreement with the measured values.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155790
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  • 8
    Electronic Resource
    Electronic Resource
    Radio evidence for an expanding magnetic arch beyond 20 solar radii (1975)
    Springer
    Solar physics 42 (1975), S. 179-181 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A magnetic loop located beyond 20 R ⊙ appears to be the later evolution of an expanding magnetic arch observed at 2 r ⊙. The expansion speed is of the order of 100 km s−1.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153294
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  • 9
    Electronic Resource
    Electronic Resource
    Satellite Observations of Radio Noise in the Magnetosphere (1968)
    [s.l.] : Nature Publishing Group
    Nature 218 (1968), S. 1145-1147 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Our recent observations on the ATS II satellite have provided new information on these noise bands to altitudes of about 8,000 km. The radio astronomy experiment on ATS II consisted of a Ryle-Vonberg radiometer operating at seven discrete frequencies between 450 kHz and 3 MHz. The antenna system ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/2181145a0
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  • 10
    Electronic Resource
    Electronic Resource
    Kilometric shock-associated events and microwave bursts (1990)
    Springer
    Astrophysics and space science 165 (1990), S. 101-110 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The peak times of impulsive microwave bursts are compared with those of shock-associated (SA) kilometric radio events. The first peaks in these two frequency regimes are usually well-correlated in time, but the last peaks of the SA events observed at 1 MHz occur an average of 20 min after the last impulsive microwave peaks. In some cases, the SA events overlap in time with the post-burst increases of microwave bursts; sometimes there is general correspondence in their intensity time profiles. These observations suggest that the earlier components of the SA events are usually caused by electrons accelerated in or near the microwave source region. We discuss the possibility that the later components of some SA events could be associated with nonthermal electrons responsible for microwave post-burst increases, although they have traditionally been attributed to electrons accelerated at type II burst producing shocks in the upper corona.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653661
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