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  • SOLAR PHYSICS  (28)
  • 2020-2024
  • 2010-2014
  • 1975-1979  (28)
  • 1955-1959
  • 1940-1944
  • 1978  (28)
  • 1
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    Energetic particles in solar flares. Chapter 4 in the proceedings of the 2nd Skylab Workshop on Solar Flares (1978)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The recent direct observational evidence for the acceleration of particles in solar flares, i.e. radio emission, bremsstrahlung X-ray emission, gamma-ray line and continuum emission, as well as direct observations of energetic electrons and ions, are discussed and intercorrelated. At least two distinct phases of acceleration of solar particles exist that can be distinguished in terms of temporal behavior, type and energy of particles accelerated and the acceleration mechanism. Bulk energization seems the likely acceleration mechanism for the first phase while Fermi mechanism is a viable candidate for the second one.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-79660 , Jan 01, 1976 - Dec 31, 1977; Boulder, CO; United States
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 2
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    Time delay occultation data of the Helios spacecraft for probing the electron density distribution in the solar corona (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: S-band time delay measurements were collected from the spacecraft Helios A and B during three solar occultations in 1975/76 within heliocentric distances of about 3 and 215 earth radius in terms of range, Doppler frequency shift, and electron content. Characteristic features of measurement and data processing are described. Typical data sets are discussed to probe the electron density distribution near the sun (west and east limb as well) including the outer and extended corona. Steady-state and dynamical aspects of the solar corona are presented and compared with earth-bound-K-coronagraph measurements. Using a weighted least squares estimation, parameters of an average coronal electron density profile are derived in a preliminary analysis to yield electron densities at r = 3, 65, 215 earth radius. Transient phenomena are discussed and a velocity of propagation v is nearly equal to 900 km/s is determined for plasma ejecta from a solar flare observed during an extraordinary set of Helios B electron content measurements.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-156950 , BMFT-FB-W-78-03
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 3
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    An observational search for large-scale organization of five-minute oscillations on the sun (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The large-scale solar velocity field has been measured over an aperture of radius 0.8 solar radii on 121 days between April and September, 1976. Measurements are made in the line Fe I 5123.730 A, employing a velocity subtraction technique similar to that of Severny et al. (1976). Comparisons of the amplitude and frequency of the five-minute resonant oscillation with the geomagnetic C9 index and magnetic sector boundaries show no evidence of any relationship between the oscillations and coronal holes or sector structure.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 57; Mar. 197
    Format: text
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  • 4
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    Transmission media effects on precise Doppler tracking (1978)
    In:  CASI
    Details
    Publication Date: 2006-01-16
    Description: The effects of the transmission media - the earth's troposphere and ionosphere, and the solar wind - on precise Doppler tracking are discussed. The charged particle effects can be largely removed by dual frequency observations; however there are limitations to these corrections (besides system noise and/or finite integration times) including the effects of magnetic fields, diffraction, and differential refraction, all of which must be carefully evaluated. The earth's troposphere can contribute an error of delta f/f approximately 10 to the minus 14th power.
    Keywords: SOLAR PHYSICS
    Type: A Close-up of the Sun; p 450-456
    Format: text
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    NASA TECHNICAL REPORTS
  • 5
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    Solar Terrestrial programs: A five year plan (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Major projects to be initiated in the 1980-1985 period, designed to study the Sun, the heliosphere, Earth's magnetosphere, and the upper atmosphere involve the use of spacelab as well as free flying spacecraft. Current and recent investigations in these areas are reviewed and the guiding principles followed in planning future missions are examined. The implementation strategy, the planning process, and supporting research and technology are discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-82351
    Format: application/pdf
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  • 6
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    Electron studies of acceleration processes in the corona (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The solar probe mission can obtain unique and crucially important measurements of electron acceleration, storage, and propagation processes in the corona and can probe the magnetic field structure of the corona below the spacecraft. The various energetic electron phenomena which will be sampled by the Solar Probe are described and some new techniques to probe coronal structures are suggested.
    Keywords: SOLAR PHYSICS
    Type: JPL A Close-up of the Sun; p 191-204
    Format: text
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  • 7
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    A new use of high resolution magnetograms (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Ground-based solar magnetograms are frequently in error by as much as twenty percent and contribute to the poor correlation between magnetic changes and solar flares. High resolution measurement of the magnetic field component, which is normal to the photosphere and measured at photospheric height, can be used to construct a magnetic flux partition function F. Therefore, dF/dt is an EMF which drives atmospheric currents in reconnecting solar active regions. With a high quality magnetograph, the solar probe can be used to obtain good estimates of F and dF/dt and thereby the energy stored as induced solar atmospheric currents during quiescent interflare periods. Should a flare occur during a favorable observing period, the present method of analysis should show characteristic signatures in F, DF/dt, and especially, in the stored flux computed from dF/dt.
    Keywords: SOLAR PHYSICS
    Type: JPL A Close-up of the Sun; p 159-169
    Format: text
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  • 8
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    Solar activity during Skylab: Its distribution and relation to coronal holes (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Solar active regions observed during the period of Skylab observations (May 1973-February 1974) were examined for properties that varied systematically with location on the sun, particularly with respect to the location of coronal holes. Approximately 90 percent of the optical and X-ray flare activity occurred in one solar hemisphere (136-315 heliographic degrees longitude). Active regions within 20 heliographic degrees of coronal holes were below average in lifetimes, flare production, and magnetic complexity. Histograms of solar flares as a function of solar longitude were aligned with H alpha synoptic charts on which active region serial numbers and coronal hole boundaries were added.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-78166
    Format: application/pdf
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  • 9
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    The role of O-type neutral lines in magnetic merging during substorms and solar flares (1978)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: An analytical model of O-type configurations was derived, for visualizing the geometry and for numerical treatment of plasma flows. It was found that at a certain distance from the neutral line the mean particle motion became decoupled from that of magnetic field lines (which obey the MHD condition). The decoupling distance depended on initial conditions in momentum space, suggesting that the MHD approximation which averages out such conditions may not suffice for describing plasma dynamics near the neutral line. It was also found that after inflowing particles are decoupled from the field line motion, they go over to a mode of runaway acceleration along the neutral line. It is concluded that if merging occurs at an X-O pair, two particle populations may be expected - low energy particles accelerated adiabatically by earthward convection past the X-type line and high-energy particles convected towards the O-type line. The second acceleration process depends critically on the rapidity of merging and is therefore expected to vary considerably from event to event.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-78093
    Format: application/pdf
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  • 10
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    Solitons and second harmonic radiation in type III bursts (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The emission at the second harmonic of the plasma frequency from self-consistent Langmuir solitons is calculated. The theory predicts, in a natural way, the observed transition from the region where the intensity is linearly proportional to the electron flux to the region where the radio intensity is proportional to the square of the electron flux. A detailed comparison of the radiation observed at the second harmonic for the burst of 18:10 UT March 31, 1976, with the one expected on the assumption of radiation from solitons, using the correlated in situ measurements of the electric fields at the second harmonic, and their spatial structure, provides strong evidence that, for the first time, Langmuir solitons have been observed in space.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 5; Oct. 197
    Format: text
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