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  • 1
    Electronic Resource
    Electronic Resource
    A Relation Between Solar Radio Emission and Polar Cap Absorption of Cosmic Noise (1960)
    [s.l.] : Nature Publishing Group
    Nature 186 (1960), S. 610-613 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] IONOSPHERIC absorption of cosmic noise in polar regions (called polar cap absorption) is believed to be caused by ionization of the upper atmosphere by fast protons (in the energy-range of 10-50 MeV.) emitted from the Sun after a big flare1 2. Direct balloon observations of protons have confirmed ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/186610a0
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  • 2
    Electronic Resource
    Electronic Resource
    Radio Observations of Ionized Hydrogen Nebulæ and Other Discrete Sources at a Wave-length of 9.4 cm. (1954)
    [s.l.] : Nature Publishing Group
    Nature 174 (1954), S. 176-177 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] We recently reported9 the further" extension, to a wave-length of 9-4 cm., of the spectra of six well-known sources and the detection of four bright galactic nebulae : the Orion, Omega, Trifid and Lagoon nebulae, bright individual HII regions. Diffuse nebulae had not been previously identified as ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/174176a0
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  • 3
    Electronic Resource
    Electronic Resource
    Evidence for electron excitation of type III radio burst emission (1972)
    Springer
    Solar physics 26 (1972), S. 468-473 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Type III radio bursts observed at kilometric wavelengths (≲ 0.35 MHz) by the OGO-5 spacecraft are compared with 〉 45 keV solar electron events observed near 1 AU by the IMP-5 and Explorer 35 spacecraft for the period March 1968–November 1969. Fifty-six distinct type III bursts extending to ≲ 0.35 MHz (≳ 50 R ⊙ equivalent height above the photosphere) were observed above the threshold of the OGO-5 detector; all but two were associated with solar flares. Twenty-six of the bursts were followed ≲ 40 min later by 〉 45 keV solar electron events observed at 1 AU. All of these 26 bursts were identified with flares located west of W 09 solar longitude. Of the bursts not associated with electron events only three were identified with flares west of W 09, 18 were located east of W 09 and 7 occurred during times when electron events would be obscured by high background particle fluxes. Thus almost all type III bursts from the western half of the solar disk observed by OGO-5 above a detection flux density threshold of the order of 10−13 Wm−2 Hz−1 at 0.35 MHz are followed by 〉 45 keV electrons at 1 AU with a maximum flux of ≳ 10 cm−2 s−1 ster−1. If particle propagation effects are taken into account it is possible to account for lack of electron events with the type III bursts from flares east of the central meridian. We conclude that streams of ≈ 10–100 keV electrons are the exciting agent for type III bursts and that these same electrons escape into the interplanetary medium where they are observed at 1 AU. The total number of 〉 45 keV electrons emitted in association with a strong kilometer wavelength type III burst is estimated to be ⩾ 5 × 1032.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00165288
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  • 4
    Electronic Resource
    Electronic Resource
    Radio observations of interplanetary magnetic field structures out of the ecliptic (1977)
    Springer
    Solar physics 52 (1977), S. 477-484 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract New observations of the out-of-the ecliptic trajectories of type III solar radio bursts have been obtained from simultaneous direction finding measurements on two independent satellite experiments, IMP-6 with spin plane in the ecliptic, and RAE-2 with spin plane normal to the ecliptic. Burst exciter trajectories were observed which originated at the active region and then crossed the ecliptic plane at about 0.8 AU. We find a considerable large scale north-south component of the interplanetary magnetic field followed by the exciters. The apparent north-south and east-west angular source sizes observed by the two spacecraft are approximately equal, and range from 25° at 600 kHz to 110° at 80 kHz.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00149662
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  • 5
    Electronic Resource
    Electronic Resource
    A New Class of Radio Source Spectra (1965)
    [s.l.] : Nature Publishing Group
    Nature 205 (1965), S. 487-488 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] In order to confirm the upward (positive) curvature in the spectra of these sources at centimetre wave-lengths, flux density measurements were also made at 16,500 Mc/s (l 1.82 cm). Table 1 lists the measured flux densities and their standard deviations of NGC 1275, 3C 279, and 3C 273 at 8,000 Mc/s ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/205487a0
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  • 6
    Electronic Resource
    Electronic Resource
    Solar wind density model from km-wave type III bursts (1973)
    Springer
    Solar physics 29 (1973), S. 197-209 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The analysis of type III bursts observed from the OGO-5 satellite between 3.5 MHz and 50 kHz (λ6 km) gives an empirical expression for the frequency drift rate as a function of frequency that is valid from 75 kHz to 550 MHz. Using this expression and some simplifying assumptions we obtain indirectly an empirical formula for the electron density distribution of the solar wind to 1 AU which is consistent with published values of electron density and with observed type III burst drift rates. Also J. Fainberg, L. G. Evans, and R. G. Stone have recently reported the detection of bursts at 30 kHz. (Science 178 (1972), 743.)
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153449
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  • 7
    Electronic Resource
    Electronic Resource
    The prevalence of second harmonic radiation in type III bursts observed at kilometric wavelengths (1973)
    Springer
    Solar physics 29 (1973), S. 183-196 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present the analysis of 64 type III solar bursts that drifted from 3.5 MHz down to the range 350-50 kHz between March 1968 and February 1970. Bursts arrival times were predicted by a simple model and then compared with observations. The results show that, as the bursts drift, the fundamental often disappears below a certain frequency range while the second harmonic remains. Below about 1 MHz the second harmonic occurrence predominates. Recognizing this fact we deduce a mean velocity of 0.32c±0.02c for the exciter particles, where the uncertainty is the standard error and c the velocity of light in vacuum; the electron density model used is comparable to a solar wind model.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153448
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  • 8
    Electronic Resource
    Electronic Resource
    Decay time of type III solar bursts observed at kilometric wavelengths (1973)
    Springer
    Solar physics 30 (1973), S. 175-182 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Type III bursts were observed between 3.5 MHz and 50 kHz by the University of Michigan radio astronomy experiment aboard the OGO-5 satellite. Decay times were measured and then combined with published data ranging up to about 200 MHz. The observed decay times increase with decreasing frequency but at a rate considerably slower than that expected from electron-proton Coulomb collisions. At 50 kHz values differ by about a factor of 100. Using Hartle and Sturrock's solar wind model, Coulomb collisional frequencies were computed and compared with the apparent collisional frequencies deduced from the observations. It was found that the ratio of observed to computed values varies with heliocentric distance according to an inverse 0.71 power. This is similar to an ad hoc function used by Wolff, Brandt, and Southwick to increase the electron-proton collisional energy exchange and make the solar wind theory agree with the measurements of electron and proton temperature near the Earth. These results may provide a clue about the nature of the non-collisional plasma wave damping process responsible for the short duration of type III bursts.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00156186
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  • 9
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    Decay time of type III solar bursts observed at kilometric wavelengths (1973)
    Springer
    Details
    Publication Date: 1973-05-01
    Print ISSN: 0038-0938
    Electronic ISSN: 1573-093X
    Topics: Physics
    Published by Springer
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  • 10
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    Proposal for the Detection of Dispersion in Radio-Wave Propagation Through Intergalactic Space (1965)
    American Physical Society
    Details
    Publication Date: 1965-06-21
    Print ISSN: 0031-9007
    Electronic ISSN: 1079-7114
    Topics: Physics
    Published by American Physical Society
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