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  • 1980-1984  (15)
  • 1
    Electronic Resource
    Electronic Resource
    The digital multi-channel radiospectrograph in Nançay (1982)
    Springer
    Solar physics 81 (1982), S. 383-394 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We describe the new Solar Radio Spectrograph which has been operated at the Nançay Radio Astronomy Station since December 1978 for the analog part (which uses photographic film data acquisition) and since July 1979 using digital magnetic recording. This instrument was designed and built by the Space Research Department of the Paris Observatory and covers the range 469–110 MHz. The multichannel receiver yields a high sensitivity, as compared to a sweep-frequency receiver and the frequency windows where external interference is present can be eliminated from the data acquisition. The digital recording leads to convenient intensity calibration procedures and allows a modern data-handling over a large dynamic range: 50 dB with a 11 bit resolution. Intermodulation effects due to non linearities have been kept to a minimum by building the multiplexer as a ‘tree’ and distributing the amplification along. The time resolution allows the data to be acquired at a rate of 100 samples per second per frequency channel. The frequency resolution can take two values: 120 channels 1 MHz-wide and 100 channels 200 kHz-wide can be positioned anywhere in the range 110–469 MHz. Some observations are shown including type V and type II-like bursts and harmonically related emission in hook structures. Some future plans are briefly mentioned aiming to perform circular polarization measurements in 120 frequency channels and real time data compression.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151311
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    Solar radio burst and in situ determination of interplanetary electron density (1984)
    Springer
    Solar physics 90 (1984), S. 401-412 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We review and discuss a few interplanetary electron density scales which have been derived from the analysis of interplanetary solar radio bursts, and we compare them to a model derived from 1974–1980 Helios 1 and 2 in situ density observations made in the 0.3–1.0 AU range. The Helios densities were normalized to 1976 with the aid of IMP and ISEE data at 1 AU, and were then sorted into 0.1 AU bins and logarithmically averaged within each bin. The best fit to these 1976-normalized, bin averages is N(R AU) = 6.1R -2.10 cm-3. This model is in rather good agreement with the solar burst determination if the radiation is assumed to be on the second harmonic of the plasma frequency. This analysis also suggests that the radio emissions tend to be produced in regions denser than the average where the density gradient decreases faster with distance than the observed R -2.10.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00173965
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    Paper (German National Licenses)
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  • 3
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    Solar radio burst and in situ determination of interplanetary electron density (1984)
    Springer
    Details
    Publication Date: 1984-02-01
    Print ISSN: 0038-0938
    Electronic ISSN: 1573-093X
    Topics: Physics
    Published by Springer
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    PAPER CURRENT
  • 4
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    The digital multi-channel radiospectrograph in Nan�ay (1982)
    Springer
    Details
    Publication Date: 1982-12-01
    Print ISSN: 0038-0938
    Electronic ISSN: 1573-093X
    Topics: Physics
    Published by Springer
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    PAPER CURRENT
  • 5
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    Determining the solar wind speed above active regions using remote radio-wave observations (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: A new technique has made it possible to measure the velocity of portions of the solar wind during its flow outward from the sun. This analysis utilizes spacecraft (ISEE-3) observations of radio emission generated in regions of the solar wind associated with solar active regions. By tracking the source of these radio waves over periods of days, it is possible to measure the motion of the emission regions. Evidence of solar wind acceleration during this outward flow, consistent with theoretical models, has also been obtained.
    Keywords: SOLAR PHYSICS
    Type: Science (ISSN 0036-8075); 222; 506-508
    Format: text
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  • 6
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    Energetic electrons associated with solar radio storms (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Keywords: SOLAR PHYSICS
    Type: Osservatorio Astronomico Solar Radio Storms. Proc. of the 4th CESRA Workshop on Solar Noise Storms; p 320-323
    Format: text
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  • 7
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    Solar radio storms in the hectometer-kilometer wavelength range (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Keywords: SOLAR PHYSICS
    Type: Osservatorio Astronomico Solar Radio Storms. Proc. of the 4th CESRA Workshop on Solar Noise Storms; p 70-88
    Format: text
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  • 8
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    Interplanetary radio storms. I - Extension of solar active regions through the interplanetary medium (1984)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: About 100 storms of type-III solar radio bursts have been identified in the ISEE-3 radio-experiment data during the 4-yr period around the maximum of the 21st solar cycle. They demonstrate the very frequent presence of streams of suprathermal electrons. Their durations range from 1 to 10 d or more. They are observed up to 100-170 solar radii. Their rate of occurrence is 2 to 3 per solar rotation near solar maximum. It is shown that the time variations of the daily radio-emission intensities correlate with the sunspot-number variations and with the solar activity in general. More specifically, a very good correlation is found with the meter-wave type-III and type-I storms, which demonstrates that the suprathermal electrons responsible for the radio emission have been accelerated below 2 solar radii heliocentric. The different lags observed between the sunspot-number variations, the S-component, and the type-I and type-III storms are discussed.
    Keywords: ASTROPHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 136; 2, Ju
    Format: text
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  • 9
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    Solar radio burst and in situ determination of interplanetary electron density (1984)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: A few interplanetary electron density scales which were derived from the analysis of interplanetary solar radio burst are discussed and compared to a model derived from 1974 to 1980 Helios 1 and 2 in situ density observations made in the 0.3 to 1.0 AU range. The Helios densities were normalized to 1976 with the aid of IMP and ISEE data at 1 AU, and were then sorted into 0.1 AU bins and logarithmically averaged within each bin. The best fit to these 1976-normalized, bin averages is in N(R(AU)) = 6.1 R(-2.10)/cu cm. This model is in rather good agreement with the solar burst determination if the radiation is assumed to be on the second harmonic of the plasma frequency. This analysis also suggests that the radio emissions tend to be produced in regions denser than the average where the density gradient decreases faster with distance than the observed R(-2.10). Previously announced in STAR as N83-35989
    Keywords: ASTROPHYSICS
    Type: Solar Physics (ISSN 0038-0938); 90; 401-412
    Format: text
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  • 10
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    Interplanetary radio storms. II - Emission levels and solar wind speed in the range 0.05-0.8 AU (1984)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Storms of interplanetary type III radio bursts (IP storms) are commonly observed in the interplanetary medium by the ISEE-3 radio instrument. This instrument has the capability of accurately determining the arrival direction of the radio emission. At each observing frequency, the storm radio sources are tracked as they cross the line-of-sight to the sun. Using a simple model, the emission levels are determined at a number of radio frequencies for four separate storms. The IP storm radiation is found to occur in regions of enhanced density at levels of 0.05 to 0.8 AU. The density in these enhancements falls off faster than R(-2). The solar wind speed in the storm region is also measured. The analysis is consistent with steady conditions in the storm region during a few days around the III storm burst radio emission at the harmonic of the local plasma frequency.
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 141; 1, De; 17-24
    Format: text
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