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  • 1
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    Hard X-ray and radio emission at the onset of great solar flares (1987)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A study of the onset phase of ten great hard X-ray bursts is presented. It is shown from hard X-ray and radio observations in different wavelength ranges that the energization of the electrons proceeds on a global time-scale for some tens of seconds. In nine of the bursts, two phases of emission can be distinguished during the onset phase: the preflash phase (during which emission up to an energy limit ranging from some tens of keV to 200 keV is observed) followed ten to some tens of seconds later by the flash phase (where the count rate in all detector channels rises simultaneously to within some seconds). For two of the events, strong gamma-ray line emission is observed and is shown to start close to the onset of the flash phase.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 111; 1, 19
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  • 2
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    A study of starting time in great hard X-ray flares (1986)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: An analysis of the starting time in ten great hard X-ray bursts observed with the X-Ray Burst Spectrometer (HXRBS) is presented. It is shown that the impulsive phase of nine of them is composed of a preflash phase, during which the burst is observed up to an energy limit ranging from some tens of keV to 200 keV, followed ten to some tens of seconds afterwards by a flash phase, where the count rate rises simultaneously in all detector channels. For two events strong gamma-ray line emission is observed and is shown to start close to the onset of the flash phase.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Rapid Fluctuations in Solar Flares; p 79-84
    Format: application/pdf
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  • 3
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    Unusual coronal activity following the flare of 6 November 1980 (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The major two-ribbon flare that occurred on November 6, 1980 is discussed, using data from the hard X-ray imaging spectrometer aboard the SMM satellite. The post-flare X-ray arch and loops are analyzed, showing the flare characteristics, the coronal arch, the time variations of X-rays after the flare, and the time variation of the maximum intensity at the top of the coronal arch in the 3.5-5.5 keV range. A comparison is made with an earlier arch. The post-flare conronal brightness variations are discussed, including a correlation with a 169 MHz noise stomr, the absence of chromospheric excitation, the brightness and temperature of the X-ray arch, the locations of the brightenings, and the details of the first and fifth brightenings. Problems posed by the observations are discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 80; Sept
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  • 4
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    The solar radio corona: Manifestations of energetic electrons (1986)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Radio observations are powerful tools which are complementary to the space missions devoted to the physics of the flares, of the corona, or of the interplanetary medium. To undertake this task two multifrequency radioheliographs presently exist: the Nancay instrument (the multifrequency facility will be in operation by the end of 1985) observes the middle corona at decimeter-meter wavelengths, and the Clark Lake radioheliograph, operating at decameter wavelengths, is the only one in the world to have the ability of observing the outer corona above the disk.
    Keywords: SOLAR PHYSICS
    Type: NASA. Marshall Space Flight Center Solar Flares and Coronal Physics Using P(OF as a Research Tool; p 159-177
    Format: application/pdf
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  • 5
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    Association between gradual hard X-ray emission and metric continua during large flares (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: X-ray radiation is used to study coronal phenomena in conjunction with meter wave observations during some large solar flares. It is found that metric flare continua and moving type IV bursts are associated with gradual and long lasting (a few tens of minutes) microwave and hard X-ray emissions. The detailed temporal analysis reveals that although metric and hard X-ray sources are located at very different heights, both kinds of emission result from a common and continuous/repetitive injection of electrons in the corona. The late part of the metric event (stationary type IV burst) is only associated with soft X-ray radiation. This indicates that the mean energy of the radiating electrons is lower during stationary type IV bursts than during the earlier parts of the event.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 84; April 19
    Format: text
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  • 6
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    Correlated observations of a spatially resolved type III solar radio burst group and the associated hard X-ray emission (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: The first measurements of the spatial structure of a group of type III solar radio bursts associated with an impulsive hard X-ray burst are presented. At 169 MHz the radio source has been found to consist of two principal regions separated by about 300,000 km. The two regions together produced a total of four component bursts in good time correlation with spikes in the hard X-ray emission. The observations indicate that electron acceleration/injection occurs over a region which covers a wide range of magnetic field lines.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 241
    Format: text
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  • 7
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    Skylab observations of the coronal structure overlying a type III producing active region (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 63; Sept
    Format: text
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  • 8
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    An association between coronal structures and type III burst sources (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Observations of the coronal structures overlying type III radio burst producing regions, obtained with the HAO Coronograph/Polarimeter on board the Solar Maximum Mission, have been combined with observations of the type III bursts from the Mark III Nancay Radioheliograph at 169 MHz. A first qualitative comparison of the data, performed for two periods, indicates that the corona overlying type III producing sites is composed of small, discrete, over-dense structures, which are sometimes diverging and short-lived. The type III burst sources are complex, exhibiting elementary components. It is suggested that the type III burst structure follows that of the corona and that discrete structures may play a fundamental role for type III production.
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics; 111; 2, Ju; July 198
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  • 9
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    X-ray and radio emissions in the early stages of solar flares (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 83; March 19
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  • 10
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    Evidnece for non-thermal processes during the build-up phase of solar flares and in absence of flares (1975)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Res. in the Space Sci., Vol. 2, No. 3; 25 p
    Format: text
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