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  • Other Sources  (130)
  • Cell & Developmental Biology
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  • Lunar and Planetary Science and Exploration
  • SOLAR PHYSICS
  • 1970-1974  (130)
Collection
Source
Keywords
Years
Year
  • 1
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    Phänologie und Reife des Körnermaises in der Bundesrepublik Deutschland in Abhängigkeit von Witterung und Klima (1974)
    In:  Diss. Weihenstephan.
    Details
    Publication Date: 1974
    Description: Analyse des Klimas und der Witterung in Bezug zu den Maiserträgen des Versuchsfeldes KATASTER-BESCHREIBUNG: KATASTER-DETAIL:
    Keywords: Deutschland ; 1956-74 ; Ertrag ; Klima ; Korrelationsmethode ; Mais ; Niederschlag ; Temperatur
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    BIBLIOGRAPHY INKA BB
  • 2
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    Low-energy protons of solar origin and investigation of the interplanetary medium (1974)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: Experimental data on low energy solar protons are presented. A phenomenological classification of the fluxes of these particles is suggested. Contemporary model conceptions of the propagation of low energy proton fluxes are examined, along with information that has been obtained on the properties of the interplanetary medium from study of solar proton fluxes.
    Keywords: SOLAR PHYSICS
    Type: Interplanet. Medium and Phys. of the Magnetosphere (NASA-TT-F-784); p 175-202
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  • 3
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    The internal structure of the convective envelope of the sun (1974)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: An axisymmetric hydrodynamic model of the sun consisting of a core at radiant equilibrium and a convective envelope is studied with consideration of gravitational forces, rotation, turbulence effects, and electromagnetic forces. The dimensionless parameters that control the equations of plasma motion within the sun and the boundary conditions are investigated; estimates are given for these parameters on the basis of experimental data and the existing theoretical models. Stability conditions are derived for convective equilibrium, developed cellular convection, and developed turbulent convection with consideration of rotation and turbulent Reynolds stresses. These conditions characterize the possible physical state of the matter in the convective envelope. Using estimates of the dimensionless parameters and models of some of them, a method of successive approximations is proposed for solution of the problem as a whole.
    Keywords: SOLAR PHYSICS
    Type: Interplanet. Medium and Phys. of the Magnetosphere (NASA-TT-F-784); p 124-150
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  • 4
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    Magnetic measurements in model experiments (1974)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: Plasma parameters for modeling of the interaction between the solar wind and the earth's magnetic field are selected on the limited modeling principle (plasma velocity 3 x 10 to the 7th power cm/sec, density 10 to the 13th power cm/3, electron temperature approximately 15 eV). Measurements were made with magnetic probes capable of developing all 3 components inside the magnetic field. The resulting magnetic field charts indicate that a neutral layer forms on the night side in the model experiments. A magnetosphere free of plasma streams is established on the daytime side. A shock wave forms on the boundary of the magnetosphere, its width c/omega sub 0 in accordance with theory, where omega sub 0 is the total Langmuir width.
    Keywords: SOLAR PHYSICS
    Type: Interplanet. Medium and Phys. of the Magnetosphere (NASA-TT-F-784); p 45-58
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  • 5
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    Solar neutrinos and the influence of radiative opacities on solar models (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Dec. 15
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  • 6
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    Observation of sectored structure in the outer solar corona - Correlation with interplanetary magnetic field (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Review of the daily images of the white light corona between 3 and 10 solar radii recorded by a coronagraph aboard the OSO-7 unmanned satellite since October 3, 1971. The observed sectored structure in the outer solar corona is discussed and correlated with the interplanetary magnetic field. The correlations support the observation of Hansen et al. (1973).
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 7
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    Polarization results of solar X-rays from OSO-7 (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Polarization measurements of solar X-ray events that were obtained with an instrument on OSO-7 are presented. The results appear to be consistent with the results of Tindo et al. on the existence and magnitudes of polarization. A comparison with polarization predictions when X-rays are produced by radial beams of electrons gives two examples of deviations from such a model.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 8
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    Magnetoacoustic instability and termination of solar wind (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Stability of a system composed of two interstreaming plasmas in the presence of a transverse magnetic field is investigated, and the theory is applied to solar-wind interaction with interplanetary gas. The system is susceptible to magnetoacoustic instability provided the ratio of densities of solar-wind protons to interplanetary protons is below a critical value. The turbulence produced by this instability will reduce the solar-wind speeds to subsonic values. This transition for the solar wind occurs at heliocentric distances between 5 and 20 AU.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 192; Sept. 15
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  • 9
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    Limb-brightening observations from the OSO-7 satellite. I - Electron density and temperature of the non-equatorial corona from EUV lines of Fe XIV and other Fe ions (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics; 37; 2, De; Dec. 197
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  • 10
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    Non-LTE H2+ as the source of missing opacity in the solar atmosphere (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: The population of the various vibrational levels of the H2+ molecule has been calculated from the consideration of formation and destruction mechanisms. The resulting population is used in calculating the total absorption due to H2+ and is compared with the other known sources of opacity at several optical depths of the solar atmosphere. It is shown that the absorption due to H2+ can probably account for the missing ultraviolet opacity in the solar atmosphere.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Dec. 15
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  • 11
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    Long-term variations of the solar wind proton parameters (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Interplanetary plasma data taken near 1 AU by a variety of spacecraft (Imp 1, Vela 2-4, Explorer 33-35, and Heos 1) from 1963 to 1971 are used to study the long-term variations of the solar wind proton properties. An intercalibration among the different experiments is performed in order to obtain a coherent set of data. The most interesting result is a 40% reduction of the proton density between the minimum and the maximum of the solar activity cycle. The observed density variation occurs throughout the velocity range; however, a limited sample of data could suggest that at very low velocities (below 300 km/sec) the density is independent of the solar activity. The proton bulk velocity is remarkably constant during the period considered; small increases of the average speed occurring in 1968 and 1971 cannot be attributed to the solar cycle. No clear trend is exhibited by the proton temperature; differences among the various experiments probably have an instrumental origin.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 79; Dec. 1
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  • 12
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    Numerical calculation of Thomson scattering from inhomogeneous models of the corona, and application to streamers of the 1970 and 1972 eclipses (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 13
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    Spectrophotometry of prominences in the phase preceding decay (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The results are presented of spectrophotometric processing of prominence spectra in both the quiet and the decay phases. A catalog was compiled of equivalent widths, central intensities, Doppler half-widths, and half-widths of emission lines. The reduced Doppler half-widths of D3 and of the H, K Ca(+) lines obtained in a prominence active phase are much larger than those obtained during a quiet phase. Comparison of the equivalent widths and central intensities of H sub alpha, H sub beta hydrogen and D3 helium lines shows that the values increase in the active phase for the D3 lines and decrease for the H sub alpha, H sub beta lines.
    Keywords: SOLAR PHYSICS
    Type: Astrometrics and Astrophysics, No. 17 (NASA-TT-F-15768); p 75-109
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  • 14
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    Luminosity conditions of Cr IX and Fe XI in the corona (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Coronal lines of wavelength 4566 A Cr IX and wavelength 3986 A Fe XI were studied. The electron temperature in the corona was found along with the electron density, and calculations were performed for Cr IX ion populations of levels. The lines were scanned photometrically within the limits of altitudes of 48,000-110,000 km.
    Keywords: SOLAR PHYSICS
    Type: Astrometrics and Astrophysics, No. 17 (NASA-TT-F-15768); p 69-74
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  • 15
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    Effect of deviation from local thermodynamic equilibrium on the Goldberg-Unno method (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The dependence of turbulent velocity on optical depth was studied by use of the Goldberg-Unno method, with allowance made for the influence of deviation from the local thermodynamic equilibrium. It was found that allowance for deviation from local thermodynamic equilibrium displaces the curve of dependence of turbulent velocity on optical depth along two axes.
    Keywords: SOLAR PHYSICS
    Type: Astrometrics and Astrophysics, No. 17 (NASA-TT-F-15768); p 62-68
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  • 16
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    Effect of a progressive sound wave on the profiles of spectral lines. 2: Asymmetry of faint Fraunhofer lines (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The absorption coefficient profile was calculated for lines of different chemical elements in a medium with progressive sound waves. Calculations show that (1) the degree and direction of asymmetry depend on the atomic ionization potential and the potential of lower level excitation of the individual line; (2) the degree of asymmetry of a line decreases from the center toward the limb of the solar disc; and (3) turbulent motions 'suppress' the asymmetry.
    Keywords: SOLAR PHYSICS
    Type: Astrometrics and Astrophysics, No. 17 (NASA-TT-F-15768); p 56-61
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  • 17
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    Solar flare emissions and geophysical disturbances (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Various geophysical phenomena are produced by both wave and particle emission from solar flares. In understanding these phenomena, it is necessary to investigate the nature of these emissions and solar flare phenomena. Using the observed data for these emissions, a review is given on the nature of solar flares and their development. Geophysical phenomena are discussed by referring to the results for solar flare phenomena.
    Keywords: SOLAR PHYSICS
    Type: Indian Journal of Radio and Space Physics; 3; Sept
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  • 18
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    Magnetic fields in flares and active prominences. II - The field configuration in some active prominences (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Study of the longitudinal magnetic field in a number of active limb prominences showing fields in excess of 30 G. The objects fall into three groups: surges, caps, and active-region prominences. There appears to be an upper limit of 150 to 200 G for the field strength in prominences. A model of surges is presented in which a presurge axisymmetric magnetic field is established by a line current in the corona. Particle acceleration in surges is observed, which indicates that V x B is not equal to zero in these objects during periods comparable to the Alfven transit time. The strong fields observed in caps seem to run between parts of active regions in accordance with Hale's law of sunspot group polarities.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Nov. 197
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  • 19
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    Solar cosmic ray composition above 10 MeV/nucleon and its energy dependence in the 4 August 1972 event (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Dec. 197
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  • 20
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    Visual and photographic white light flare observations of 4 July 1974 (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Visual impressions and a photograph of an intense white-light flare are presented. A densitometer trace across the July 4, 1974, flare showing relative intensity of the white-light flare, photosphere, and umbra is also shown. A second white-light flare is suspected on a photograph taken 4-3/4 hr later. Both flares coincide in time with major H alpha-flare activity.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Dec. 197
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  • 21
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    Rigid and differential rotation driven by oscillations within the sun (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Long-period oscillations involving the entire mass of the sun rotate like rigid bodies, and their oscillatory power is distributed nonuniformly across the solar surface. A mostly qualitative theory is constructed showing how the oscillations drive convective flows of global scale, which then organize photospheric and coronal magnetic fields into patterns which rotate rigidly. The convection rises along long graceful curves, creating the magnetic-arcade structures in the corona and unipolar photospheric regions on each side by dynamo action. These are thought to be the origin of the sector structure in the solar wind. The rigid patterns of convective upwelling also force nonrigid horizontal winds on the solar surface. Under the action of the Coriolis force, the main horizontal motions are converted into polar and equatorial wind currents which have the proper directions to drive the differential rotation long observed on the sun's surface.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Dec. 1
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  • 22
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    Calibration of OSO-7 Fe XV 284 A spectroheliograms in solar-geophysical data bulletin (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Oct. 197
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  • 23
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    Slowly varying component of extreme ultraviolet solar radiation and its relation to solar radio radiation (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: A study of the correlations between solar EUV line fluxes and solar radio fluxes has been carried out. A calibration for the Goddard Space Flight Center EUV spectrum is suggested. The results are used to obtain an equation for the absolute EUV flux for several lines in the 150- to 400-A region and the total flux of 81 intense lines in the region, the 2800-MHz radio flux being used as independent variable.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 79; Oct. 1
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  • 24
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    Solar energetic particle event with He-3/He-4 greater than 1 (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: An unusual solar event involving the detection of a He-3/He-4 ratio of about 1.5 was observed with the aid of the cosmic-ray telescopes of OGO-V on May 28, 1969. A theory dealing with the production of H-2, H-3, and He-3 in solar events is considered together with the conditions which would have to be satisfied in order to explain the observed very high helium isotope ratio in terms of the theory.
    Keywords: SOLAR PHYSICS
    Type: Nature; 252; Dec. 6
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  • 25
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    Deuterium, tritium, and helium-3 production in solar flares (1974)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 193; Nov. 1
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  • 26
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    A search for solar neutrons during solar flares (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A new upper limit to the 1-20 MeV neutrons produced at the sun during large solar flares was obtained as a result of measurements made by a neutron detector on board the OGO-6 satellite. It was found that the 1-20 MeV solar neutron flux for the Nov. 2, June 13, June 15, Sept. 25, and Dec. 19, 1969, solar flare events cannot be greater than 0.05 n per sq cm per sec at the 95% confidence level. These measurements are consistent with the models proposed by Lingenfelter (1969) and Lingenfelter and Ramaty (1967) for solar neutron production during solar flares.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Nov. 197
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  • 27
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    OSO-7 observations of solar X-rays in the energy range 10-100 keV (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Data on 123 hard X-ray bursts observed by the satellite OSO-7 between Oct. 10, 1971 and June 6, 1972 are described and evaluated. Typical duration of a burst is 100 sec. Average spectral indices lie between 3.5 and 5.5 for two-thirds of the 123 bursts, with a median of 4.6. In some events a soft-hard-soft pattern is observed, but there are numerous examples in which the spectrum softens continuously throughout the burst. The mean shape of the hard X-ray time profile as measured by the full width at half maximum does not depend on burst amplitude; nor does the spectral hardness correlate with the flux. The distribution of burst peak fluxes and the observation of large soft X-ray bursts without accompanying hard X rays suggest the existence of a distinct class of solar flares which emit only soft X rays. No center-to-limb variation was found in the frequency of occurrence of bursts or in the fraction with a nonthermal component. Estimates of the energy in the form of nonthermal electrons and in the flare plasma derived from these data indicate that the total amounts in each are comparable.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Nov. 197
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  • 28
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    Physical properties of solar chromospheric plages. II - Chromospheric plage models (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Chromospheric models of plages are proposed to explain profiles of the Ca II H, K, 8498-A, 8542-A, and 8662-A lines. These models are consistent with boundary conditions imposed by the photosphere and the Lyman continuum. It is found that increasing emission in these lines is consistent with a picture of increasing temperature gradient in the low chromosphere and the resulting increase in pressure and electron density at similar line optical depths. With this picture it is shown how the distribution of chromospheric parameters across the solar disk can be empirically determined directly from Ca II filtergrams. It is also proposed that the high-density aspects of solar activity are produced by steep temperature gradients in the low chromosphere and thus by the enhanced heating mechanisms that steepen these gradients.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Nov. 197
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  • 29
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    A brief study of the interaction mechanism of magnetized solar wind streams with the geomagnetic field - Vela 3, Explorers 33 and 35, and Mariner 5 (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
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  • 30
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    Solar wind model predictions for the sources of streams observed at 1 AU - Coronal enhancements or coronal holes (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The present paper discusses attempts which have been made to locate the solar sources of the solar wind streams observed at or near 1 AU. Solar-wind data collected by the Mariner 2, Mariner 5, and IMP-1 spacecraft are considered. It is concluded that the type of solar feature considered as the source of solar-wind velocity enhancements depends upon the solar-wind model used. All single-fluid models predict the source to have a significantly higher temperature and lower density than the surrounding region, while the two-fluid model predicts a change in temperature that is much smaller than the predicted change in density.
    Keywords: SOLAR PHYSICS
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  • 31
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    Initial results from the EUV spectroheliometer on ATM (1974)
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    Publication Date: 2019-07-27
    Description: The Harvard College Observatory photoelectric spectroheliometer on the Apollo Telescope Mount operated correctly in orbit from May 29, 1973 to Feb. 7, 1974. During this period many thousands of spatial and spectral scans at extreme ultraviolet wavelengths were recorded during observations of a variety of solar features. The construction and modes of operation of the instrument are outlined and the principal scientific results from a preliminary analysis of the data are described.
    Keywords: SOLAR PHYSICS
    Type: AIAA PAPER 74-1258
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  • 32
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    Solar flares (1974)
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    Publication Date: 2019-06-27
    Description: A review of the knowledge about solar flares which has been obtained through observations from the earth and from space by various methods. High-resolution cinematography is best carried out at H-alpha wavelengths to reveal the structure, time history, and location of flares. The classification flares in H alpha according to either physical or morphological criteria is discussed. The study of flare morphology, which shows where, when, and how flares occur, is important for evaluating theories of flares. Consideration is given to studies of flares by optical spectroscopy, radio emissions, and at X-ray and XUV wavelengths. Research has shown where and possibly why flares occur, but the physics of the instability involved, of the particle acceleration, and of the heating are still not understood.
    Keywords: SOLAR PHYSICS
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  • 33
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    Studies of solar magnetic fields. III - The east-west orientation of field lines (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Dec. 197
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  • 34
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    The instability of strong magnetic fields in stellar interiors (1974)
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    Publication Date: 2019-06-27
    Description: There has been discussion of the possibility of resolving the solar neutrino dilemma with a sufficiently strong magnetic field (500 MG) in the solar interior to relieve the gas pressure by some 10% or more. The time in which magnetic buoyancy will bring a strong field to the surface is examined and is found to be less than 100 m.y. No possibility is seen for retaining a suitably strong magnetic field in the solar interior.
    Keywords: SOLAR PHYSICS
    Type: Astrophysics and Space Science; 31; Nov. 197
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  • 35
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    Observations of broad-band circular polarization in sunspots - Magnetic field correspondence (1974)
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    Publication Date: 2019-06-27
    Description: The present work proposes a general rule relating the polarity of broad-band (spectral range: 5250 A to 5350 A) circular polarization fields observed in sunspots to that of the corresponding magnetic fields. The rule is illustrated with observations of particular spots.
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics; 37; 1, De; Dec. 197
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  • 36
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    Solar prominences in the extreme ultraviolet as observed from the Apollo Telescope Mount (1974)
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    Publication Date: 2019-06-27
    Description: Observations of quiescent solar prominences with the Harvard College Observatory spectrometer aboard Skylab show that prominence material is optically thick in the Lyman alpha line and the Lyman continuum. The color temperature of the Lyman continuum has a mean of 6600 K and an upward gradient toward the top of the prominence. The departure coefficient of the ground state of hydrogen is found to be of the order of unity, as expected from theory. The optical depth of the C III sheath region is determined directly from the observation of the limb through the prominence and is used to infer the mean electron density and the temperature gradient of the sheath. The result implies that the sheath density is about 0.4, and the temperature gradient about 1.4 times the respective value in the C III transition zone of the quiet sun. The C III triplet-singlet ratio for the prominence is found to give a density compatible, within the uncertainty of the atomic parameters, with the density obtained from the optical depth.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Dec. 197
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  • 37
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    The polarization of continuum radiation in sunspots. I - Rayleigh and Thomson scattering (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Expressions are derived for the Stokes parameters of light scattered by a layer of free electrons and hydrogen atoms in a sunspot. A physically reasonable sunspot model was found so that the direction of the calculated linear polarization agrees reasonably with observations. The magnitude of the calculated values of the linear polarization agrees generally with values observed in the continuum at 5830 A. Circular polarization in the continuum also accompanies electron scattering in spot regions; however for commonly accepted values of the longitudinal magnetic field, the predicted circular polarization is much smaller than observed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 39; Nov. 197
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  • 38
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    Solar flux and its variations (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Data on the solar irradiance as derived from a number of sources are presented. An attempt was made to bring these data onto a uniform scale. Summation of fluxes at all wavelengths yields a figure of 1357.826 per sq m for the solar constant. Estimates are made of the solar flux variations due to flares, active regions (slowly varying component), solar rotation and the 11-year cycle. Solar activity does not produce a significant variation in the value of the solar constant. Nevertheless, variations in the X-ray and extreme ultraviolet portions of the solar flux may be several orders of magnitude during solar activity, especially at times of major flares. It is well established that these short wavelength flux enhancements cause significant changes in the terrestrial ionosphere.
    Keywords: SOLAR PHYSICS
    Type: Space Science Reviews; 16; Nov
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  • 39
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    Extreme-ultraviolet observations of coronal holes - Initial results from Skylab (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: We compare the appearance and physical parameters of the solar chromosphere, transition zone, and corona in areas of coronal holes with that of quiet areas outside the hole. Measurements of the height of emission of various ions in a coronal hole appearing at the polar limb give a quantitative indication of the increased thickness of the transition zone underlying coronal holes.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Dec. 1
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  • 40
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    On the Fe XXIV emission in the solar flare of 1973 June 15 (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The double ribbon flare of 1973 June 15 was observed in the XUV wavelength region with the NRL objective grating spectroheliograph during the Skylab missions. The Fe XXIV emissions at 192.1 and 255.2 A are prominent in the early phase of the flare. The Fe XXIV emission is centered over the neutral line, forming a bridgelike structure between magnetic regions of opposite polarity. This is unlike the emission pattern of He II, the transition zone ions, and Fe IX-XVI, which are relatively brighter in the adjacent flare ribbons overlying strong vertical magnetic field. An electron density of 5 times 10 to the 10th per cu cm for the Fe XXIV emission region is deduced from the observational data, and the cooling rate is briefly discussed.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Dec. 1
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  • 41
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    The solar cycle variation of the solar wind helium abundance (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: NSSDC-ID-68-014A-17-OS , Journal of Geophysical Research; 79; Nov. 1
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  • 42
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    Mass ejections from the sun - A view from Skylab (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: More than 30 instances of sudden mass ejections from the sun were observed with the white light coronagraph experiment aboard Skylab during the first 118 days of the mission. Typically, these ejections appear as large magnetic loops rooted at the sun, yet expanding outward through the solar corona at speeds of the order of 400 km/sec. The loops always appear to retain their magnetic connection to the sun. Eighteen of these ejections were associated with active and eruptive prominences and surges; only three ejections appear to have been flare initiated. Associations with ground-detected metric wavelength type 2 and 4 radio bursts occur for about 30% of these events; however, ground-detected type 2 and 4 radio bursts originating near the limb are almost invariably accompanied by coronagraph-observed ejections. Pressure or MHD waves run out ahead of the transient material ejecta; at times these waves can be detected by their effects on nearby coronal structures.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 79; Nov. 1
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  • 43
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    Acceleration of electrons in absence of detectable optical flares deduced from type III radio bursts, H alpha activity and soft X-ray emission (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: NSSDC-ID-68-014A-04-PS , NSSDC-ID-69-051A-18-PM , Solar Physics; 38; Oct. 197
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  • 44
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    Solar cycle variation of large-scale coronal structures (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A green line intensity variation is associated with the interplanetary and photospheric magnetic sector structure. This effect depends on the solar cycle and occurs with the same amplitude in the latitude range 60 N-60 S. Extended longitudinal coronal structures are suggested, which indicate the existence of closed magnetic field lines over the neutral line, separating adjacent regions of opposite polarities on the photospheric surface.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Oct. 197
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  • 45
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    Broad-band circular and linear polarization in sunspots Center-to-limb variation (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics; 35; 3, Oc; Oct. 197
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  • 46
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    Magnetic fields in the sun (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The observed properties of solar magnetic fields are reviewed, with particular reference to the complexities imposed on the field by motions of the highly conducting gas. Turbulent interactions between gas and field lead to heating or cooling of the gas according as the field energy density is less or greater than the maximum kinetic energy density in the convection zone. The field strength above which cooling sets in is 700 G. A weak solar dipole field may be primeval, but dynamo action is also important in generating new flux. The dynamo is probably not confined to the convection zone, but extends throughout most of the volume of the sun. Planetary tides appear to play a role in driving the dynamo.
    Keywords: SOLAR PHYSICS
    Type: Franklin Institute; vol. 298
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  • 47
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    Structures in a non-magnetic solar corona (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A fluid mechanical convective instability is examined under the conditions found in the solar corona. Linearized density perturbations are shown to grow as they are carried outward by the solar wind. The non-linear instability may be proposed as a cause of coronal structures in nonmagnetic stars, or in regions of the solar corona with weak magnetic fields.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 48
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    The fine structure of the solar atmosphere in the far ultraviolet (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The paper describes qualitatively the spatial distribution of UV emission obtained from high resolution spectroheliograms in the UV emission lines He I, He II, O IV, O V, and Ne VII photographed during a sounding rocket flight. Broad band filtergrams of the far UV solar corona were also obtained. The results confirmed that spicules are the location of UV emission. Most of the UV emission in the temperature range from 100,000 to 200,000 K is concentrated in and around the spicules and this concentration decreases with increasing temperatures. Four different areas of UV emission are discussed. The He I and He II spectroheliogram observations showed He to be suppressed in the coronal holes, polar caps, and sunspots.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 49
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    Studies of K line filtergrams (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The paper describes the material obtained on a Lyot filter for K at the Big Bear Solar Observatory. This material is compared with simultaneous H-alpha observations. K-line filtergrams are used to interpret K-line double reversal. The structure of the general chromosphere is discussed. It is found that the absorption of the cool clouds of the chromosphere, covering about one third of the area inside the cells, oscillating rapidly, and having a vertical extent around 3000 km, is not clearly seen in K3. In active regions K is close to H-alpha. Here all plagettes and plages are bounded by systems of strongly inclined bright and dark fibrils. Umbral flashes are found to be less visible in H-alpha, except that the running penumbral waves are bright in K and dark in H-alpha.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 50
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    Is magnetic convection important in the sun (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: It is found that magnetic convection most probably operates inside the sun. The energy flux which it can carry is five to six orders of magnitude smaller than the total solar flux. The velocity with which magnetic flux rises from the interior of the sun towards the surface is measured. Under conditions where the entire stellar flux is carried by convection, the velocities of magnetic buoyancy are compared with the velocities of convective elements inside stars. Observation shows magnetic convection effects on the internal temperature structure of the sun to be small.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 51
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    Studies of solar magnetic fields. II - The magnetic fluxes (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Magnetic flux data from the Mount Wilson magnetograph are examined over the interval 1967-1973. The total flux in the north is greater than that in the south by about 7% over this interval, reflecting a higher level of activity in the northern hemisphere. Close to 95% of the total flux is confined to latitudes equatorward of 40 degrees, which means that close to 95% of the flux cancels with flux of opposite polarity before it can migrate poleward of 40 degrees. It is pointed out that a consequence of this flux distribution is that ephemeral regions must make a negligible contribution to the long-term large-scale magnetic flux distribution. A broad peak in the total flux may be seen centered about one year after activity maximum in the north below 40 degrees. In the south there is a very sharp increase in flux about the same time. In the north, several poleward migrations of flux may be seen.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 38; Sept
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  • 52
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    The interstellar wake of the solar wind (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The present work examines theoretically the cooling of the subsonic solar wind by the interstellar hydrogen gas entering the solar system. It is assumed that the interstellar hydrogen gas is distributed uniformly in the space where the solar wind is subsonic, and the solar-wind wake is represented by an idealized column flow of plasma in which the flow velocity is constant and the temperature varies along, not across, the wake. The results are therefore to be taken only in their order of magnitude. In the hot region near the shock sphere the electrons are cooled mainly through electron ionization while the protons cool through charge exchange. In the cooler regions far away from the shock, the protons are still cooled by charge exchange and the electron is cooled by collisions with protons. As the temperature of the solar wind decreases, the magnetic field becomes relatively more important. When the spin axis of the sun is parallel to the direction of the incident interstellar gas flow, the lines of force are in spiral form and the tension causes the plasma to be concentrated along the center of the wake.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 194; Nov. 15
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  • 53
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    Extreme-ultraviolet observations of sunspots with the Harvard spectrometer on the Apollo Telescope Mount (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 193; Nov. 1
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  • 54
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    The solar X-ray spectrum (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The characteristics of X-ray emission from the normal corona are considered, giving attention to questions of spatial and spectral distribution. Aspects of X-ray emission from solar flares are also investigated. Details of X-ray spectroscopy for coronal plasma diagnosis are discussed, taking into account techniques, the diagnosis of equilibrium plasmas, and the diagnosis of nonthermal events. The study of continuum emission and line emission is reported along with investigations of departures from equilibrium.
    Keywords: SOLAR PHYSICS
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  • 55
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    Shock waves generated by the intense solar flare of 1972, August 7, 15:00 UT (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The dynamic radio spectrum of the class 3B solar flare of 1972, August 7, 15:00 UT, over the band 10 to 2000 MHz is examined. Type II and type IV bursts in the spectrum are interpreted in terms of a piston-driven shock, which appeared to be traveling at a velocity of about 1500 km per sec and which generated pulsations in the band 100 to 200 MHz as it passed through the corona. The progress of the shock through the interplanetary plasma was subsequently monitored by Malitson et al. with radio equipment covering the band 0.03 to 2.6 MHz on the IMP-6 satellite.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 56
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    Multi-slit spectrograph and H alpha Doppler system (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Description of the design and operation of a multiple-entrance-slit spectrograph, built for time-lapse photography of the spectra of flares and other transient solar phenomena. This spectrograph employs narrow-band filters to limit the wavelength range of the spectrograph to a few angstroms centered at H-alpha or other spectral lines. A polarizing beamsplitter, prior to the slits, provides a prefiltered second solar image to a narrow band H-alpha Doppler filter for simultaneous photography in the wings of the H-alpha line. The spectrograph and the H-alpha Doppler system constitute a flexible instrument in which components may be substituted to achieve different passband widths, image scales, dispersions, and corresponding numbers and spacings of adjacent spectra at a selected wavelength.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 57
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    A three-component concept of the chromosphere and transition region (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: It is proposed that present observations of the chromosphere and transition region in EUV, optical and mm wavelengths are best described by a three-component concept. The three components are taken to be the interiors of supergranular cells, the hot plagettes overlying faculae, and the cooler, transient mottles which surround them in the network boundaries. The enhanced emission of the hot plagettes in transition ions is interpreted as a direct result of the increased pressure scale height over faculae relative to the cell interiors.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 58
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    Magnetic field and electric current structure in the chromosphere (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The three-dimensional vector magnetic field structure in the chromosphere above an active region is deduced by using high-resolution H-alpha filtergrams together with a simultaneous digital magnetogram. An analog model of the field is made with 400 metal wires representing field lines that outline the H-alpha structure. The height extent of the field is determined from vertical field-gradient observations around sunspots, from observed fibril heights, and from an assumption that the sources of the field are largely local. The computed electric currents (typically 10 mA/sq m) are found to flow in patterns not similar to observed features and not parallel to magnetic fields. Force structures correspond to observed solar features; the dynamics to be expected include: downward motion in bipolar areas in the lower chromosphere, an outflow of the outer chromosphere into the corona with radially outward flow above bipolar plage regions, and motion of arch filament systems.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 37; Aug. 197
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  • 59
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    Pioneer 9 plasma wave and solar plasma measurements for the August 1972 storm period (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The solar disturbances of August 1972 produced large-scale solar wind perturbations that were detected by the Pioneer 9 plasma probe, electric field detector, and magnetometer for an extended time period commencing early on August 3. During this ten-day interval the interplanetary plasma parameters at r approximately equal 0.8 AU varied over unusually wide ranges, so that the conditions for generation of high and low VLF wave levels could be identified fairly readily. It is demonstrated that no measurable signals were detected in the broadband electric field channel (sensitive to waves with f greater than or equal to 100 Hz in the spacecraft frame of reference) unless the proton density was high enough to yield a proton plasma frequency with f greater than or about equal to 100 Hz. The analysis suggests that waves related to ion acoustic oscillations were detected throughout the extended storm period.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 79; Oct. 1
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  • 60
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    Solar flare proton rigidity spectra deduced from cosmic ray neutron monitor observations (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The solar flare proton rigidity spectra for several flares occurring between 1967 and 1972 have been deduced from the ground level cosmic ray neutron monitor observations. To obtain consistent agreement for all the ground level events (GLEs) analyzed, the specific yield functions of Lockwood and Webber (1967) must be reduced slightly below P = 1.6 GV. The typical spectral indices of solar cosmic rays deduced for GLEs vary from 4 to 6 if the differential spectrum is represented by KP to the minus gamma power. Only occasionally is the spectrum as steep as 8 or 9. The observed spectral index is independent of the magnitude of the integral solar proton flux above 1 GV.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 79; Oct. 1
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  • 61
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    Monte Carlo analysis of the solar-wind modulation of galactic C-N-O at solar maximum (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A previous (Moss and Giuli, 1971) Monte Carlo analysis of the solar-wind modulation of galactic cosmic-ray rigidity spectra is extended to include particles in the C-N-O group. A solar cavity 'radius' of 7 AU is found to be consistent with observations of the C-N-O component at solar maximum. The variation in modulation between solar maximum and solar minimum may be explained solely by variation of the solar cavity size, with no change in the scattering mean free path.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 192; Sept. 15
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  • 62
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    The small-scale, quasi-periodic, disk component of solar radio radiation (1974)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Interferometric observations of the sun at wavelengths of 3.7 and 11 cm show that small-scale, quasi-periodic radio emission is coming from the sun. The periods occur in a band of periods with a midband frequency of 3.75 mHz and a bandwidth of 2.5 mHz. The peak-to-peak fluctuations in brightness temperature, lie between 4,000 and 500,000 K. The radio emission is less than about 10% linearly or circularly polarized; the angular size of the emitting regions is of the order of 10 seconds. The radio emission originates at the base of the chromosphere-corona transition region at approximately 2200 km above the level at which the optical depth at 5000 A is unity.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 192; Sept. 15
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  • 63
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    The relationship between solar flares and solar sector boundaries (1974)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: A superposed epoch analysis of 1964-1970 solar flares shows a marked increase in flare occurrence within a day of (-+) solar sector boundaries, as well as a local minimum in flare occurrence near (+-) sector boundaries. This perference for (-+) boundaries is more noticeable for Northern Hemisphere flares, where these polarities match the Hale polarity law, but is not reversed in the south. Plage regions do not show such a perference.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-140856 , SU-IPR-597
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  • 64
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    Simulation of colliding solar wind streams with multifluid codes (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 65
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    The power associated with density fluctuations and velocity fluctuations in the solar wind (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Direct observations from Pioneer 6 of solar-wind-proton fluctuations have been used to obtain the power spectra associated with solar-wind-proton number density and velocity fluctuations in the frequency range of 0.001 to 0.01 Hz, extending previous analyses by an order of magnitude at the higher frequencies. The slopes of the power spectra associated with the density fluctuations and the velocity fluctuations are similar and are in agreement with the shape of the power spectra found at the lower frequencies. The power spectra indicate that the power-law density spectrum observed at lower frequencies extends to at least 0.01 Hz. This smooth variation in the spectrum at these frequencies is consistent with previous extrapolations of both spacecraft and interplanetary scintillation observations.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 66
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    The latitude dependencies of the solar wind (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The motion of spacecraft following the earth's orbit occurs within the solar latitude range of 7 deg 15 min N on approximately September 7 to 7 deg 15 min S on approximately March 6. The latitude dependencies so far detected within this range have shown that the photospheric dipole-like field of the sun makes very important contributions to the interplanetary magnetic field (IMF) observed near the ecliptic. Changes in geomagnetic activity from even to odd numbered 11-year solar cycles are related to changes in the sun's dipolar field. The north-south IMF component and meridional, nonradial flow are important to a complete understanding of steady-state solar wind dynamics. Coronal conditions must be latitude-dependent in a way that accounts for the observed latitude dependence of the velocity and density of the solar wind.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 67
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    Nuclear composition of solar cosmic rays (1974)
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    Publication Date: 2019-07-13
    Description: Experimental observations of the elemental and isotopic composition of solar flare particles are discussed. Sources and characteristics of particle-emitting solar flare events are reviewed, and techniques for separating particle species are briefly described. Data are presented for the elemental composition of the solar atmosphere, and the possibility of determining the solar helium abundance from solar cosmic-ray observations is explored. The main experimental determinations of heavy element abundances at energies greater and less than 10 MeV/nucleon are summarized, and techniques for measuring the ionic charge composition of solar cosmic rays are outlined. Models explaining heavy element enhancements are described along with processes leading to gamma-ray emission during solar flare events. Observations of the rare isotopes of hydrogen and helium during solar flare events are noted, and a lower atmospheric limit is derived for nuclear reactions leading to positron decay. The possibility of investigating low-energy solar cosmic rays by measuring the relative abundances of different elements is evaluated.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 68
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    Rocket spectrometer for investigation of the far ultraviolet solar spectrum (1974)
    In:  CASI
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    Publication Date: 2019-07-13
    Description: A rocket-borne Ebert spectrometer and telescope were used for analysis of the solar spectrum. The instrument was arranged in the high resolution line scanning mode. Selected emission lines between 1170 and 1640 A were scanned, and a complete wavelength scan was made from 1170 A to 1850 A. Accurate measurements were made of the line profiles of the He II lines at 1640 A, C IV lines at 1550 A, Si IV lines at 1400 A, C II lines at 1335 A, the N V lines at 1240 A, and the C III lines at 1175 A. Accurate intensity measurements of the quiet sun spectrum for wavelengths between 1174 A and 3220 A were obtained. Spectral resolution was better than 0.03 A over most of the range and spatial resolution was relatively low so that the observations are averaged over the chromospheric network. Plots of absolute intensity versus wave length were prepared for the full wavelength range of the observations.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-119089 , SASR-9 , SASR-10
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  • 69
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    Estimates of radiation exposure from solar cosmic rays in SST altitudes (1974)
    In:  CASI
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    Publication Date: 2019-07-13
    Description: Factors influencing crew and passenger exposure to solar and galactic cosmic rays that is expected to occur during flights of supersonic transport aircraft are discussed, and some possibilities are considered for decreasing such exposure.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-71990 , FAUSST 6 Meeting; Feb 01, 1968; London; Egland
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  • 70
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    The Third Solar Wind Conference: A summary (1974)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The Third Solar Wind Conference consisted of nine sessions. The following subjects were discussed: (1) solar abundances; (2) the history and evolution of the solar wind; (3) the structure and dynamics of the solar corona; (4) macroscopic and microscopic properties of the solar wind; (5) cosmic rays as a probe of the solar wind; (6) the structure and dynamics of the solar wind; (7) spatial gradients; (8) stellar winds; and (9) interactions with objects in the solar wind. The invited and contributed talks presented at the conference are summarized.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-141322 , PUBL-1354-51-REV , Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA; United States
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  • 71
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    Relation of coronal magnetic structure to the interplanetary proton events of August 2-9, 1972 (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: In order to interpret the time history of protons of energy greater than about 13.5 MeV observed on Pioneers 9 and 10 and IMP 5 from the flares of Aug. 2, 4 and 7, the coronal connection longitudes of the interplanetary field lines were estimated using the solar wind velocities measured on the spacecraft. There is reasonable agreement between the observed magnetic field polarity at Pioneer 9 and the equatorial chromospheric polarity at the inferred connection longitudes. The protons appear to be released preferentially in a large magnetic neutral-line complex that surrounds the flare region (McMath 11976) from Carrington longitudes 0 to 60. Although impulsive proton events were observed from all three flares by Pioneer 9, only the second two were seen at earth, and Pioneer 10 never showed comparable impulsive response. These apparent discrepancies are resolved by comparison with magnetic neutral line structure.
    Keywords: SOLAR PHYSICS
    Type: Correlated interplanetary and magnetospheric observations; Seventh ESLAB Symposium; May 22, 1973 - May 25, 1973; Saulgau
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  • 72
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    Gamma ray observations during the August 1972 solar activity (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: During the solar activity period in August 1972, the UNH gamma ray monitor on the OSO-7 satellite measured gamma ray line and continuum fluxes of solar origin on at least two occasions; August 4 and 7. In this discussion, the experiment and the gamma ray line observations are reviewed with a few brief remarks on interpretation. The specific observations discussed are measurements of gamma ray lines at 0.51 and 2.2 MeV during two of the largest optical solar flares. Evidence for lines at other energies is also given.
    Keywords: SOLAR PHYSICS
    Type: Correlated interplanetary and magnetospheric observations; Seventh ESLAB Symposium; May 22, 1973 - May 25, 1973; Saulgau
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  • 73
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    Design characteristics of a Skylab soft X-ray telescope (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: An unprecedented amount of high-quality scientific data has been obtained by the S-056 soft X-ray telescope experiment, together with five other major solar experiments aboard the Skylab Apollo Telescope Mount. A 10-year period will be required to get the 26,000 frames of data into proper form. The optical schematic of the instrument is discussed, and the instrument and its subsystems are described.
    Keywords: SOLAR PHYSICS
    Type: Instrumentation in astronomy II; Seminar-in-Depth; Mar 04, 1974 - Mar 06, 1974; Tucson, AZ
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  • 74
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    The photoelectric spectroheliometer on ATM (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The Harvard College Observatory instrument on the Skylab Apollo Telescope Mount is a photoelectric spectroheliometer designed to obtain up to seven simultaneous spectroheliograms in the range between 280 and 1340 A with a spatial resolution of 5 arc sec, as well as spectral scans with a resolution of 1.6 A over the same range of wavelengths. The optical schematic of the instrument is illustrated and discussed. Because of its large size, the instrument has a sensitivity far greater than that of any other EUV spectroheliometer flown to date. The instrument has operated correctly in orbit since May 1973. Valuable data have been obtained during this period on a variety of solar phenomena, on the comet Kohoutek, and on the atmospheres of the earth and Mercury. The instrument was successfully recalibrated in orbit by comparing the response with that of recently calibrated spectroheliometers flown on sounding rockets.
    Keywords: SOLAR PHYSICS
    Type: Instrumentation in astronomy II; Seminar-in-Depth; Mar 04, 1974 - Mar 06, 1974; Tucson, AZ
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  • 75
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    The X-ray spectrographic telescope (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The S-054 X-ray telescope, which operated successfully throughout the eight-month Skylab mission, is a grazing incidence instrument with a spatial resolution of the order of 2 arc sec on axis. The total wavelength range observed by the instrument is 2 to 60 A. Crude spectral resolution within this range is achieved by means of a series of six X-ray filter materials. A spectrographic mode of operation, employing an objective grating, is used to obtain spectra of flare events and selected coronal features.
    Keywords: SOLAR PHYSICS
    Type: Instrumentation in astronomy II; Seminar-in-Depth; Mar 04, 1974 - Mar 06, 1974; Tucson, AZ
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  • 76
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    Apollo 17 lunar surface cosmic ray experiment - Measurement of heavy solar wind particles (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: During the Apollo 17 mission a series of metal foils and nuclear track detectors were exposed both in the sun and in the shade on the surface of the moon. Here we give the analysis of the mica detectors which were used to measure the flux of solar wind particles of Fe-group and heavier elements. These particles register as shallow pits after etching in hydrofluoric acid. Calibration experiments were performed to determine the registration properties of different ions and to simulate the lunar environment. We obtain an Fe-group flux of 39,000 per sec per sq cm, which together with the H flux measured on IMP-7 gives an Fe/H ratio of 0.000041. For elements with Z exceeding 45 we can set only an upper limit on the abundance, ruling out an overabundance of extremely heavy elements relative to iron by a factor of 4.
    Keywords: SOLAR PHYSICS
    Type: Lunar Science Conference; Mar 18, 1974 - Mar 22, 1974; Houston, TX
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  • 77
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    Early active sun - Radiation history of distinct components in fines (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Plagioclase feldspars were separated from lunar soil samples and their compositions were determined by electron-microprobe analysis followed by etching and track counting in an effort to find effects of early solar activity. The feldspars were assigned on this basis to three major lithologies: mare basalts, anorthositic rocks, and KREEP rock. The results are in sharp contrast to Poupeau et al.'s (1973) observations on track densities in plagioclase crystals in the Luna 16 soil: no evidence is found for an early active sun, although the evidence does not preclude this possibility, either.
    Keywords: SOLAR PHYSICS
    Type: Lunar Science Conference; Mar 18, 1974 - Mar 22, 1974; Houston, TX
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  • 78
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    Cosmic ray anisotropies late in a solar flare event (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The detailed relationship between the anisotropy characteristics observed during late times in the decay of a solar flare event and the interplanetary magnetic field parameters is investigated. The anisotropy always is from 45 deg east of the earth-sun line. This direction is approximately perpendicular to the nominal Archimedean spiral, independent of the particle energy. The amplitude of the anisotropy increases as the magnetic field azimuthal direction shows greater departure from the radial direction. These results are discussed in terms of current ideas about solar particle propagation in the interplanetary space.
    Keywords: SOLAR PHYSICS
    Type: International Symposium on Solar-Terrestrial Physics; Jun 17, 1974 - Jun 22, 1974; Sao Paulo; Brazil
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  • 79
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    Model of an anisotropy solar proton event (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: The anisotropy of the particle distribution and its variation with time at 1 AU early in a solar cosmic-ray event can provide information on the pitch-angle scattering of the particles in the interplanetary medium. One proton event (7.6-55 MeV) is described in which the anisotropy remained large well into the decay of the omnidirectional intensity. A Monte Carlo technique which gives the pitch-angle distribution is employed to investigate two models put forward to explain the sustained anisotropy. It is shown that the observed event is consistent with a model in which the injection of particles at the sun reaches a peak 1.5 hours after flare maximum before decaying with an e-folding time of 7 hours. The uniform diffusion coefficient in this model corresponds to a classical mean free path of 1.6 AU.
    Keywords: SOLAR PHYSICS
    Type: International Symposium on Solar-Terrestrial Physics; Jun 17, 1974 - Jun 22, 1974; Sao Paulo; Brazil
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  • 80
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    Coronal transient phenomena (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: A hydrodynamical description of outward propagating disturbances from the sun's surface in a model solar atmosphere is considered. Use is made of this model to explain the coronal transient phenomenon. It was found that this radial flow model clearly indicates the mass flow as being continuous, going out from the surface of the sun. Detailed results are presented for the disturbed density, velocity and temperature of the corona up to 6 solar radii.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 81
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    Pioneer Solar Plasma and Magnetic Field Measurements in Interplanetary Space During August 2-17, 1972 (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Solar wind plasma and magnetic field measurements from Pioneers 9 and 10 during August 2-17, 1972, reveal complex and large-amplitude variations on a one-hour time scale and numerous discontinuities. During this time period an approximate radial alignment of the two spacecraft as seen from the Sun occurred with heliocentric distances of 0.8 AU for Pioneer 9 and 2.2 AU for Pioneer 10, both at 45 deg east of the Earth's solar longitude. The peak hourly average solar wind proton bulk velocity measured at Pioneer 9 was 990 km sec (exp -1) during hour 0 UT of August 5. The peak hourly average proton number density was 62 cm (exp -3) during hour 11 UT of August 3. The peak solar wind speeds are generally much reduced at Pioneer 10 compared with those observes at Pioneer 9. The peak 30 minute average magnetic field magnitude was 85 gamma during 1245 - 1315 UT of August 3. The Pioneer 9 data indicate passage of four fast forward interplanetary shocks, and one slow forward interplanetary shock.
    Keywords: SOLAR PHYSICS
    Type: Correlated interplanetary and magnetospheric observations; Seventh ESLAB Symposium; May 22, 1973 - May 25, 1973; Saulgau
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  • 82
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    Mariner Venus/Mercury 1973 solar radiation force and torques (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The need for an improvement of the mathematical model of the solar radiation force and torques for the Mariner Venus/Mercury spacecraft arises from the fact that this spacecraft will be steering toward the inner planets (Venus and Mercury), where, due to the proximity of the Sun, the effect of the solar radiation pressure is much larger than it was on the antecedent Mariner spacecraft, steering in the opposite direction. Therefore, although the model yielded excellent results in the case of the Mariner 9 Mars Orbiter, additional effects of negligible magnitudes for the previous missions of the Mariner spacecraft should now be included in the model. This study examines all such effects and incorporates them into the already existing model, as well as using the improved model for calculation of the solar radiation force and torques acting on the Mariner Venus/Mercury spacecraft.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-142092 , JPL-TM-33-698
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  • 83
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    Solar radio continuum storms (1974)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: Radio noise continuum emission observed in metric and decametric wave frequencies is discussed. The radio noise is associated with actively varying sunspot groups accompanied by the S-component of microwave radio emissions. It is shown that the S-component emission in microwave frequencies generally occurs several days before the emission of the noise continuum storms of lower frequencies. It is likely that energetic electrons, 10 to 100 Kev, accelerated in association with the variation of sunspot magnetic fields, are the sources of the radio emissions. A model is considered to explain the relation of burst storms on radio noise. An analysis of the role of energetic electrons on the emissions of both noise continuum and type III burst storms is presented. It is shown that instabilities associated with the electrons and their relation to their own stabilizing effects are important in interpreting both of these storms.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-139176
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  • 84
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    Directional discontinuities from Mariner 5 and solar wind structure (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Directional discontinuities from Mariner 5 are studied. A substantial majority of the events have properties which are consistent with their being identified as tangential discontinuties. The results presented here agree in several respects with those of Burlaga from Pioneer 6. In addition, new results are presented. Previous Mariner 5 work on this subject is summarized with an explanation of apparent inconsistencies.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-70733 , X-693-74-234
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  • 85
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    Solar particle events with anomalously large relative abundance of He-3 (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Experimental results are reported on three energetic particle events with extremely high abundance of He-3. The measurements were taken onboard the OGO-5 satellite. It was shown that the abundance of protons relative to He nuclei were significantly low in these events. Not more than four H-2 and three H-3 were detected during the entire period under study compared to 1110 H-3 nuclei. The limitations these observations place on theoretical models are discussed to explain He-3 flares.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-70780 , X-661-74-312
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  • 86
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    Coordinated rocket and satellite observations of the solar corona (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Coronal condensations associated with active regions are investigated by comparing their X-ray and EUV line intensities. The EUV line measurements were made with the OSO-H satellite, and the X-ray measurements were made with an ATM support rocket. The data obtained from these observations are used to find the emission measure distribution at low temperatures.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-140581 , LMSC-D404808
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  • 87
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    Dynamics of the solar wind and its interaction with bodies in the solar system (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The results of the research related to solar winds are presented. Also included is a summary of papers and publications completed.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-140702
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  • 88
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    Termination of the solar wind in the hot, partially ionized interstellar medium (1974)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Theoretical foundations for understanding the problem of the termination of the solar wind are reexamined in the light of most recent findings concerning the states of the solar wind and the local interstellar medium. The investigation suggests that a simple extention of Parker's (1961) analytical model provides a useful approximate description of the combined solar wind, interstellar wind plasma flowfield under conditions presently thought to occur. A linear perturbation solution exhibiting both the effects of photoionization and charge exchange is obtained for the supersonic solar wind. A numerical algorithm is described for computing moments of the non-equilibrium hydrogen distribution function and associated source terms for the MHD equations. Computed using the algorithm in conjunction with the extended Parker solution to approximate the plasma flowfield, profiles of hydrogen number density are given in the solar wind along the upstream and downstream axes of flow with respect to the direction of the interstellar wind. Predictions of solar Lyman-alpha backscatter intensities to be observed at 1 a.u. have been computed, in turn, from a set of such hydrogen number density profiles varied over assumed conditions of the interstellar wind.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-140699
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  • 89
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    The solar corona as seen from Skylab (1974)
    In:  Other Sources
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    Publication Date: 2019-07-27
    Description: The white light coronagraph (WLC) experiment of the Skylab/ATM obtained an unprecedented series of observations of the solar corona from 1.5 to 6 solar radii for approximately eight and one-half months. Coronal evolution and disruptions seen by the WLC occur on many different time scales. Some illustrative examples will be shown. The characteristics of mass ejection coronal transients - as we presently know them - will be given. These include: the greater than expected frequency of occurrence; the correlation with solar activity; the quantity of mass and energy contained in a transient; etc.
    Keywords: SOLAR PHYSICS
    Type: AIAA PAPER 74-1232
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  • 90
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    San Marco C-2 Explorer (1974)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: The San Marco C-2 spacecraft will be launched no earlier than 18 February 1974 from the San Marco Range located off the coast of Kenya, Africa, by a Scout launch vehicle. The launch will be conducted by an Italian crew. The San Marco C-2 is the fourth cooperative satellite project between Italy and the United States. The purpose of the mission is to obtain measurements of the diurnal variations of the equatorial neutral atmosphere density, composition, and temperature and to use these data for correlation with AE-C (Explorer 51) data for studies of the physics and dynamics of the thermosphere. The San Marco C-2 project is a joint undertaking of the National Aeronautics and Space Administration (NASA) and the Italian Space Commission officially initiated with a Memorandum of Understanding in August of 1973. Project management responsibility for the Italian portion of the project has been assigned to the Centro Ricerche Aerospaziali (CRA) while the Goddard Space Flight Center (GSFC) has responsibility for the United States portion.
    Keywords: Lunar and Planetary Science and Exploration
    Type: MOR-S-894-74-04 , HQ-E-DAA-TN40131
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  • 91
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    Our prodigal sun (1974)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: Characteristics of the sun are reported indicating it as a source of energy. Data from several space missions are discussed, and the solar activity cycle is presented. The corona, flares, prominences, spots, and wind of the sun are also discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-EP-118
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  • 92
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    Intercomparison of ground-based and space solar flux measurements (1974)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: Detailed temporal measurements of the solar flux at one location are performed. These data are then analyzed and compared to the potential of space measurements which allow one to consider the flux falling on areas of the earth. An important result of the research is that the temporal characteristics of the flux in the presence of a real atmosphere would be difficult to obtain from space and that the variations in the flux can be highly significant in regard to most solar conversion schemes. The detailed results of the research are presented. The instruments developed to separate the direct and scattered solar flux, the computer analysis methods developed, and the results of the research, presented as both graphical and tabular data, are discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-146087
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  • 93
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    Particle acceleration in solar flares (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: A review of observational data supports the proposal that there are two distinct phases of particle acceleration in solar flares. 'Phase 1' is associated with the flash phase and is here interpreted as acceleration during field-line reconnection. 'Phase 2' is associated with type II and type IV radio bursts, and is ascribed to stochastic acceleration in the turbulent plasma behind a magnetohydrodynamic shock formed ahead of an ejected plasmoid.
    Keywords: SOLAR PHYSICS
    Type: Coronal disturbances; Symposium, Surfer''s Paradise; Sep 07, 1973 - Sep 11, 1973; Queensland; Australia
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  • 94
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    The flash phase of solar flares - Satellite observations of electrons (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Satellite observations of solar electrons bearing on flare particle acceleration and the generation of radio and X-ray emission are reviewed. The observations support a two-stage acceleration process for electrons, one stage commonly occurring at the flare flash phase and accelerating electrons up to about 100 keV, and a second stage occurring only in large proton flares and accelerating electrons up to relativistic energies. The location of the acceleration region appears to be no lower than the lower corona. The accelerated non-relativistic electrons generate type III radio burst emission as they escape from the sun. Direct spacecraft observations of the type III emission generated near 1 AU and the energetic electrons, provide quantitative information on the characteristics of the electrons exciting type III emission, the production of plasma waves, and the conversion from plasma waves to electromagnetic radiation.
    Keywords: SOLAR PHYSICS
    Type: Coronal disturbances; Symposium, Surfer''s Paradise; Sep 07, 1973 - Sep 11, 1973; Queensland; Australia
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  • 95
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    Impulsive /flash/ phase of solar flares - Hard X-ray, microwave, EUV and optical observations (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Keywords: SOLAR PHYSICS
    Type: Coronal disturbances; Symposium, Surfer''s Paradise; Sep 07, 1973 - Sep 11, 1973; Queensland; Australia
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  • 96
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    The enhancement of solar wind fluctuations with scale size near the proton gyroradius (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 97
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    Theoretical predictions of latitude dependencies in the solar wind (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Results are presented which were obtained with the Winge-Coleman model for theoretical predictions of latitudinal dependencies in the solar wind. A first-order expansion is described which allows analysis of first-order latitudinal variations in the coronal boundary conditions and results in a second-order partial differential equation for the perturbation stream function. Latitudinal dependencies are analytically separated out in the form of Legendre polynomials and their derivative, and are reduced to the solution of radial differential equations. This analysis is shown to supply an estimate of how large the coronal variation in latitude must be to produce an 11 km/sec/deg gradient in the radial velocity of the solar wind, assuming steady-state processes.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 98
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    Radial gradient of solar wind velocity from 1 to 5 AU (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Solar wind velocity measurements made by Pioneers 10 and 11 are compared to investigate radial variations in the velocity at heliocentric distances of 1 to 5 AU. Two hundred days of corresponding Pioneer 10 and 11 data are plotted, the velocity profiles for 25-day segments are compared, and the same general pattern of peaks and troughs is found in the corresponding profiles. A comparison of the relative smoothness of the profiles clearly shows that velocity amplitudes in the solar wind stream structure decrease dramatically with increasing radial distance from the sun, although the rate of decrease is not as clear. It is hypothesized that stream-stream interactions play a dominant part in inhibiting the classical radial expansion process in the solar wind and produce scattering centers which prevent the observation of a significant galactic cosmic ray gradient in this region of space.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 99
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    Travelling solar radio bursts (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: This review considers the properties of solar radio bursts originating in the outer corona and interplanetary medium between approximately 0.5 solar radius and one AU from the sun as observed between meter and kilometer wavelengths. Traveling radio bursts, such as type II's, III's, moving IV's, and noise storms, are of interest in their own right as they relate to questions of the generation of nonthermal coherent emission and the transport of radiation in an astrophysical plasma. In the context of this review, however, emphasis will be on how traveling radio bursts provide information on the solar plasma environment, gross magnetic field configuration, and disposition of solar ejecta along the trajectory of the radio source as it propagates outward through the solar atmosphere.
    Keywords: SOLAR PHYSICS
    Type: Solar wind three; Third Conference; Mar 25, 1974 - Mar 29, 1974; Pacific Grove, CA
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  • 100
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    Millimeter radio evidence for containment mechanisms in solar flares (1974)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Recent theories of solar flares are reviewed with emphasis on the aspects of pre-flare heating. The heating evident at 3.3-mm wavelength is analyzed in the form of daily maps of the solar disk and synoptic maps compiled from the daily maps. It is found that isotherms defining antenna temperature enhancements of 340 K correspond in shape and location to facular areas reported by Waldmeier. Maximum enhancements occur over sunspots or near neutral lines of the longitudinal magnetic fields which indicates heating associated with chromospheric currents. These enhancements are correlated with flare importance number and are observed to increase during several days preceding flaring. This evidence for a containment mechanism in the chromosphere is collated with current theories of solar flares.
    Keywords: SOLAR PHYSICS
    Type: Coronal disturbances; Symposium, Surfer''s Paradise; Sep 07, 1973 - Sep 11, 1973; Queensland; Australia
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