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  • SOLAR PHYSICS  (232)
  • 2020-2022
  • 1975-1979  (232)
  • 1
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    Sources of magnetic fields in recurrent interplanetary streams (1978)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: The paper examines sources of magnetic fields in recurrent streams observed by the Imp 8 and Heos spacecraft at 1 AU and by Mariner 10 en route to Mercury between October 31, 1973 and February 9, 1974, during Carrington rotations 1607-1610. Although most fields and plasmas at 1 AU were related to coronal holes and the magnetic field lines were open in those holes, some of the magnetic fields and plasmas at 1 AU were related to open field line regions on the sun which were not associated with known coronal holes, indicating that open field lines may be more basic than coronal holes as sources of the solar wind. Magnetic field intensities in five equatorial coronal holes, certain photospheric magnetic fields, and the coronal footprints of the sector boundaries on the source surface are characterized.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 83; Sept. 1
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  • 2
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    MSFC solar activity predictions for satellite orbital lifetime estimation (1979)
    In:  CASI
    Details
    Publication Date: 2006-01-16
    Description: The procedure to predict solar activity indexes for use in upper atmosphere density models is given together with an example of the performance. The prediction procedure employs a least square linear regression model to generate the predicted smoothed vinculum R sub 13 and geomagnetic vinculum A sub p(13) values. Linear regression equations are then employed to compute corresponding vinculum F sub 10.7(13) solar flux values from the predicted vinculum R sub 13 values. The output is issued principally for satellite orbital lifetime estimations.
    Keywords: SOLAR PHYSICS
    Type: NOAA Solar-Terrest. Predictions Proc., Vol. 1; p 378-384
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  • 3
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    A solar plasma stream measured by DRVID and dual-frequency range and Doppler radio metric data (1977)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: S- and X-band DRVID, S- and X-band dual-frequency range (SX(p)), and Doppler (SX(p)) measured a 15-fold increase in the line-of-sight electron content of the solar plasma above the normal plasma background. A general increase in the plasma electron content continued for nearly 50 hours: it started about 12:00 (GMT) on 12 March 1976 and continued to grow until 17:00 (GMT) on 14 March. For the next 55 hours, between 17:00 (GMT) on 14 March to 00:54 (GMT) on 17 March, the plasma level diminished as the background level was approached. Not only were the temporal changes and absolute level of the plasma content measured but the measurements were also used to ascertain the mean-plasma-concentration location: it was estimated to be 4.1 light minutes from earth.
    Keywords: SOLAR PHYSICS
    Type: The Deep Space Network; p 43-54
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  • 4
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    Electromagnetic instabilities driven by unequal proton beams in the solar wind (1976)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: The paper sets forth a numerical investigation of the linear dispersion relation for typical solar wind conditions at 1 AU during those times (high-speed streams) when a secondary beam of protons drifting relative to the main proton component is present. Three beam-driven instabilities were found to occur as the beam drift velocity approaches the Alfven speed: (1) a pure, field-aligned magnetosonic wave that is most important at relatively high beta and/or high beam drift speeds; (2) an oblique magnetosonic wave having highest growth rates 15-30 deg from the magnetic field; and (3) an oblique Alfven wave having maximum growth rates at increasing angle to the magnetic field. The linear growth rates for the field-aligned magnetosonic and the Alfven oblique modes are investigated as a function of relative beam density, varying anisotropic pitch angle distributions for the various components, electron temperature, and electron heat flux.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; June 1
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  • 5
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    Observation of an impulsive solar X-ray burst from a coronal source (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Observations of the spatial, spectral, and temporal structure of an impulsive hard X-ray source in a behind-the-limb solar flare have been made with high-time-resolution hard X-ray detectors aboard two spacecraft, the International Sun Earth Explorer 3 (ISEE 3) and the Pioneer Venus Orbiter (PVO), which were separated in heliographic longitude by about 12.5 deg. The principal findings are that (1) the coronal part of the X-ray source is about 600 times less intense than the lower-altitude part of the source; and (2) the coronal X-ray observations are consistent with a power-law electron spectrum which extends down to about 5 keV.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; vol. 233
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  • 6
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    An investigation of the 1.9 A feature in solar-flare X-ray spectra (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The 1.9 A feature, observed in the X-ray spectra of three solar flares with the Columbia University and Lockheed Palo Alto Research Laboratory spectrometers on the OSO 8 satellite, is shown to be due to a blend of 1s-2p transitions in a range of Fe ions. In the temperature range 9-16 x -10 to the 6th K, the feature has a mean wavelength of 1.900 + or - 0.009 A and is 0.04 A wider than a single line, indicating that the main contributors are Fe XIX-Fe XXII. Most of the emission originates from the dielectronic recombination process, and when inner-shell excitation is included together with normal collisional excitation, the observed intensity of the feature can be accounted for adequately. For these events, if the electron density is below approximately 10 to the 12th/cu cm, deviations from ionization equilibrium will be significant for ions more highly ionized than Fe XXI.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; vol. 231
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  • 7
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    A survey on initial results of the Helios plasma experiment (1977)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The reported results are mainly based on data obtained during the first part of the Helios-1 mission. The sun was very quiet during the considered period. The data are, therefore, representative for comparatively stationary conditions in the solar corona. Data obtained concerning the protons were evaluated by means of a special computer routine. The significance of the data is discussed, taking into account the status of the corona and the interplanetary plasma during the considered part of the Helios-1 mission, fast stream structures in the region between 0.3 and 1 AU, radial gradients of fast and slow solar wind, and the separation of proton double streams and alpha-particles. Attention is also given to the 'strahl' in the electron distribution, differences between fast streams and slow plasma on the basis of the observed electron distributions, and radial gradients in the case of solar wind electron parameters.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysics - Zeitschrift fuer Geophysik; 42; 6, 19; 1977
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  • 8
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    Synoptic analysis of interplanetary radio scintillation spectra observed at 34 MHz (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Synoptic observations of the temporal power spectrum of interplanetary scintillations were made in the summer of 1976 on the University of Iowa's Cocoa Cross radio telescope and the University of Maryland's TPT array. Most of the observations were at large (larger than 40 deg) solar elongations. It was found that the power spectrum broadens when enhanced turbulence at the front of a high-speed solar wind stream sweeps over the earth. In the case with sufficient synoptic coverage, the broadening appeared to result from the relative closeness of the enhanced scattering region rather than from an increase in velocity. A small percentage of the spectra displayed two power law components with a plateau between them. These may result from a flattening in the spatial turbulence spectrum such as has been observed by spacecraft.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 83; Sept. 1
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  • 9
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    Does the emission measure decrease during the start of a soft X-ray flare (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: It is suggested that the apparent emission dip found in soft X-ray flare observations, interpreted as the emission from a single temperature plasma, is an artifact. According to this hypothesis, the flare phenomenon represents a combination of flare plus a stable active region plasma. A small amount of hot flare plasma will dominate the total emission, and the calculated isothermal plasma parameters will trend towards those of the hot flare plasma, so that a decrease in emission measure will be inferred. It is claimed that observed data fit the model of a stable plasma plus a flare plasma better than it does the model of a single plasma, in accordance with a chi square statistic. The model of stable plasma plus flare plasma is also supported by the observation that the plasma parameters in the postflare condition are indistinguishable from those during preflare.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 59; Oct. 197
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  • 10
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    Evidence of outward flow of plasma in a coronal hole (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The solar spectrum was photographed in the range 200-700 A with a grazing-incidence stigmatic rocket spectrograph. Doppler shifts of the three coronal lines Si XI (303 A), Mg X (610 A), and Mg IX (368 A) were measured for various regions of the solar disk, including a coronal hole. From the relative shifts in the latter region, an average outward velocity of 16 km/s was computed for the plasma in the coronal hole. The full widths at half-maximum for the above lines were appreciably less in the coronal-hole region than in a quiet region, indicating a lower temperature in the hole. Both the measured velocity and the temperature results are consistent with solar-wind data and with current theories of coronal holes.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 207; July 1
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