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  • 1
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    Solar wind thermal electrons in the ecliptic plane between 1 and 4 AU - Preliminary results from the Ulysses radio receiver (1992)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: The radio receiver of the Unified Radio and Plasma experiment aboard the Ulysses spacecraft records spectra of the quasi-thermal plasma noise. The interpretation of these spectra allows the determination of the total electron density Ne and of the cold (core) electron temperature Tc in the solar wind. A single power law does not fit the variations of Ne which result from the contribution from different solar wind structures. The distribution of the values of Tc suggests that, on the average, the solar wind is nearly isothermal.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 19; 12, J; 1295-129
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  • 2
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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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  • 3
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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
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  • 4
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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
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  • 5
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    Coronal mass ejections and coronal structures (1986)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Research on coronal mass ejections (CMF) took a variety of forms, both observational and theoretical. On the observational side there were: case studies of individual events, in which it was attempted to provide the most complete descriptions possible, using correlative observations in diverse wavelengths; statistical studies of the properties CMEs and their associated activity; observations which may tell us about the initiation of mass ejections; interplanetary observations of associated shocks and energetic particles even observations of CMEs traversing interplanetary space; and the beautiful synoptic charts which show to what degree mass ejections affect the background corona and how rapidly (if at all) the corona recovers its pre-disturbance form. These efforts are described in capsule form with an emphasis on presenting pictures, graphs, and tables so that the reader can form a personal appreciation of the work and its results.
    Keywords: SOLAR PHYSICS
    Type: Energetic Phenomena on the Sun: The Solar Maximum Mission Flare Workshop. Proceedings; 71 p
    Format: application/pdf
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  • 6
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    Fundamental and harmonic emission in interplanetary type II radio bursts (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Three interplanetary type II radio bursts which show two prominent and long duration bands in their dynamic spectra were analyzed in detail and compared to similar bands in meter wavelength type II events. These bands, which differ by a factor of about two in frequency, were interpreted in terms of fundamental and harmonic emission. The fundamental component has a greater average intensity than the harmonic, due largely to short intense brightenings. The fundamental spectral profile is more narrow than that of the harmonic, with harmonic band typically exhibiting a larger bandwidth to frequency ratio than the fundamental by a factor of two. The fundamental has a larger source size than the harmonic, 160 degrees versus 110 degrees, on average, as viewed from the sun. Two of the events have source positions which correlate well with the associated flare positions.
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 151; 2, Oc; 215-221
    Format: text
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  • 7
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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
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  • 8
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    Ulysses radio observations of the heliospheric activity in early June 1991 (1995)
    In:  Other Sources
    Details
    Publication Date: 2019-04-02
    Description: The radio receiver of the URAP (Unified Radio and Plasma Wave) experiment on Ulysses has recorded a heliospheric activity particularly intense between late May and early June 1991. Many solar radio emissions of types III and II were observed together with interplanetary (IP) shocks. In the same time, the radio spectrograph ARTEMIS at Nancay (France) observed several intense type II bursts. We investigate the association and/or interaction of these radio emissions, which are remotely observed, with some IP shocks detected in situ, in the context of a Coronal Mass Ejection (CME) induced scenario.
    Keywords: SOLAR PHYSICS
    Type: Advances in Space Research (ISSN 0273-1177); 16; 9; p. (9)345
    Format: text
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  • 9
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    Radio evidence for interplanetary streamers in the range 10-170 solar radii (1983)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Type III radio storms are observed by the radio experiment on board the International Sun Earth Explorer 3 out to 0.5-0.8 AU from the Sun, at a rate of 2 to 3 storms per solar rotation near solar maximum. They correlate with the type I and type III radio storms observed at higher frequencies, originating closer to the Sun. They are associated with an almost continuous injection of suprathermal electrons into the interplanetary medium. Some of the properties of the regions where the particles propagate are discussed, using the radio emission as a tracer.
    Keywords: SOLAR PHYSICS
    Type: JPL Solar Wind Five; p 469-474
    Format: application/pdf
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  • 10
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    Interplanetary radio storms. 2: Emission levels and solar wind speed in the range 0.05-0.8 AU (1982)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Storms of interplanetary type III radio bursts (IP storms) are commonly observed in the interplanetry 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. Usng 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 central meridian passage of the storm. The comparison with average in situ density measurements compiled from the HELIOS 1-2 observations favors type III storm burst radio emission at the harmonic of the local plasma frequency.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-84946 , NAS 1.15:84946
    Format: application/pdf
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