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  • Chemical Engineering  (366)
  • Cell & Developmental Biology  (276)
  • SOLAR PHYSICS  (258)
  • 1980-1984
  • 1975-1979  (900)
  • 1976  (900)
Collection
Keywords
Publisher
Years
  • 1980-1984
  • 1975-1979  (900)
Year
  • 1
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    Some basic considerations of measurements involving collimated direct sunlight (1976)
    In:  CASI
    Details
    Publication Date: 2006-08-09
    Description: For abstract, see N77-26622.
    Keywords: SOLAR PHYSICS
    Type: Terrest. Photovoltaic Meas., 2; p 233-246
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  • 2
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    The solar spectrum at typical clear weather days (1976)
    In:  CASI
    Details
    Publication Date: 2006-08-09
    Description: The solar spectrum in the range of 300 is less than lambda is less than 1500nm is given for five typical clear weather days. These days are selected to represent typical seasonal conditions in respect to airmass water vapor, ozone, and turbidity. Present data are reviewed, and specific conditions are selected. The spectral distribution of the irradiance is given for the direct component, the scattered skylight, the total flux on a horizontal surface, and the flux on an inclined surface normal to the direct beam.
    Keywords: SOLAR PHYSICS
    Type: NASA. Lewis Res. Center Terrest. Photovoltaic Meas., 2; p 17-58
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  • 3
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    Monitoring solar radiation: The ERDA program (1976)
    In:  CASI
    Details
    Publication Date: 2006-08-09
    Description: An overview of the Energy Research and Development Administration planned insolation data network is described. The design of the network is predicated on an analysis and definition of user requirements. Research and analysis projects covering data collection, forecasting and extrapolation are presented.
    Keywords: SOLAR PHYSICS
    Type: NASA. Lewis Res. Center Terrest. Photovoltaic Meas., 2; p 1-17
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  • 4
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    Artificial solar eclipse experiment MA-148 (1976)
    In:  CASI
    Details
    Publication Date: 2006-01-12
    Description: On July 19, 1975, the Apollo spacecraft successfully occulted the solar disk from the field of view of a camera mounted in the Soyuz spacecraft while performing a spacecraft separation maneuver to permit the outer solar corona to be viewable by the Soyuz camera. The camera operated automatically, and 55 frames were developed for scientific analysis.
    Keywords: SOLAR PHYSICS
    Type: Apollo-Soyuz Test Project; 5 p
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  • 5
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    Stratospheric aerosol measurement experiment MA-007 (1976)
    In:  CASI
    Details
    Publication Date: 2006-01-12
    Description: The Apollo Soyuz Test Project Stratospheric Aerosol Measurement Experiment was flown to demonstrate that direct solar occultation measurements by photometers and photographs can be used for defining stratospheric aerosol concentrations. Supporting ground truth data were provided by laser radar and balloon borne dustsonde. Initial results show a significant difference in aerosol concentrations between the Northern and Southern Hemispheres.
    Keywords: SOLAR PHYSICS
    Type: Apollo-Soyuz Test Project; 8 p
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  • 6
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    DSS 14 operating noise temperature during Helios 1 near-sun tracking (1976)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: When spacecraft are tracked near the line-of-sight of the sun, the ground antenna sidelobes see the solar noise. The solar noise increases the ground system operating noise temperature and degrades the downlink RF reception performance. At specific antenna azimuthal angles relative to the sun, noise peaks and nulls occur periodically throughout a day's tracking pass due to the quadripod support leg-generated sidelobes. This article documents this effect while tracking Helios 1, illustrates the time of the peaks, and compares the predicted time of the noise temperature peaks with the measured data.
    Keywords: SOLAR PHYSICS
    Type: The Deep Space Network; p 68-76
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  • 7
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    The solar wind and its influence on the atmospheres of moon, Mercury and Venus (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: The solar wind is expected to have an important influence on the atmospheres of the moon, Mercury and Venus and therefore a brief outline of solar wind theory is presented along with the predicted properties of the wind at the orbits of these planets. Since the atmospheres of the moon and possibly Mercury are formed primarily by solar wind accretion, we present the latest accretion models for these bodies. The expected role the solar wind plays on both the ionization and termination of the ionosphere of Venus is discussed.
    Keywords: SOLAR PHYSICS
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  • 8
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    The solar brightness temperature at millimeter wavelengths (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Measurements of the brightness temperature of the sun near 36 GHz and 93 GHz were made using the new moon as a calibration source. Provided the brightness temperature of the moon is known and all measurements are reduced to the same zenith angle, a simple expression can be used for the sun-to-new moon ratio which is independent of antenna gain, atmospheric absorption and reemission, and radiometer calibration constants. This ratio was measured near 36 GHz and at two frequencies near 93 GHz with a Dicke switched superheterodyne radiometer system and a 2.4 m Cassegrain antenna. The slopes of the solar brightness temperature spectrum based on these ratios were measured. The absolute solar brightness spectrum derived from all current available measurements supplemented by the present ones is also plotted and discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 48; May 1976
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  • 9
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    Evidence for the regulation of solar wind heat flux at 1 AU (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Observational evidence favoring the local regulation of solar-wind heat flux at 1 AU is reviewed, and four months of IMP 6 plasma and magnetic-field data are merged and analyzed in order to investigate what might be regulating the heat flux. A statistical analysis of the data shows that the solar-wind Alfven speed is probably regulating the heat flux locally at 1 AU and that the Alfven speed, the velocity difference between the peak of low-energy electrons and the bulk plasma velocity, and the solar-wind velocity component projected along the local spiral angle are statistically well correlated for Alfven speeds not exceeding about 70 km/s. A time-series analysis of the data indicates that only the Alfven speed and the velocity difference between the peak of low-energy electrons and the bulk plasma velocity are well correlated both qualitatively and quantitatively on a microscopic time scale. It is strongly suggested that, at times, the solar-wind heat flux is locally regulated by the magnitude of the Alfven speed at 1 AU. Uncertainties in the results are discussed.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Oct. 1
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  • 10
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    High-speed solar wind flow parameters at 1 AU (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Nineteen high-speed solar-wind streams observed at 1 AU between March 1971 and July 1974 are studied to develop a more realistic set of constraints for theories on such streams. The streams were chosen because their speeds exceeded 650 km/s for at least several consecutive three-hour periods and because their properties met certain other criteria. A comparison of average stream parameters with predictions of existing steady-state models shows that no single model is adequate to explain the observations. In particular, it is found that no existing model consistent with reasonable coronal conditions predicts the particle fluxes, the convected proton bulk-flow-energy fluxes, and the convected proton enthalpy fluxes observed at 1 AU when the flow speed exceeds 650 km/s.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Oct. 1
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  • 11
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    Forbidden transition probabilities for ground terms of ions with p or p5 configurations (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Forbidden transition probabilities are given for ground term transitions of ions in the isoelectronic sequences with outer configurations 2s2 2p (B I), 2p5 (F I), 3s2 3p (Al I), and 3p5 (Cl I). Tables give, for each ion, the ground term interval, the associated wavelength, the quadrupole radial integral, the electric quadrupole transition probability, and the magnetic dipole transition probability. Coronal lines due to some of these ions have been observed, while others are yet to be observed. The tales for the Al I and Cl I sequences include elements up to germanium.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 46; Jan. 197
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  • 12
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    Hectometric and kilometric solar radio emission observed from satellites in August 1972 (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Type II, type III, and continuum solar radio events, as well as intense terrestrial magnetospheric radio emissions, were observed at low frequencies (10 MHz to 30 kHz) by the IMP-6 satellite during the period of high solar activity in August 1972. This review covers briefly the unique direction-finding capability of the experiment, a detailed chronology of the low-frequency radio events, and, where possible, their association with both ground-based radio observations and solar flares. The attempted observation of solar bursts in the presence of intense magnetospheric noise may, as illustrated, lead to erroneous results in the absence of directional information. The problem of assigning an electron-density scale and its influence on determining burst trajectories is reviewed. However, for the disturbed conditions existing during the period in question, it is felt that such trajectories cannot be determined accurately by this method. The capabilities, limitations, and observing programs of present and future satellite experiments are briefly discussed.
    Keywords: SOLAR PHYSICS
    Type: Space Science Reviews; 19; Oct
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  • 13
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    Diamagnetic boundary layers - A kinetic theory (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: A kinetic theory is presented for boundary layers associated with MHD tangential 'discontinuities' in a collisionless magnetized plasma, such as those observed in the solar wind. The theory consists of finding self-consistent solutions of Vlasov's equation and Maxwell's equation for stationary one-dimensional boundary layers separating two Maxwellian plasma states. Layers in which the current is carried by electrons are found to have a thickness of the order of a few electron gyroradii, but the drift speed of the current-carrying electrons is found to exceed the Alfven speed, and accordingly such layers are not stable. Several types of layers in which the current is carried by protons are discussed; in particular, cases are considered in which the magnetic-field intensity, direction, or both, changed across the layer. In every case, the thickness was of the order of a few proton gyroradii, and the field changed smoothly, although the characteristics depended somewhat on the boundary conditions. The drift speed was always less than the Alfven speed, consistent with stability of such structures. These results are consistent with observations of boundary layers in the solar wind near 1 AU.
    Keywords: SOLAR PHYSICS
    Type: Astrophysics and Space Science; 45; Dec. 197
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  • 14
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    The solar physics Shuttle/Spacelab program and its relationship to studies of the flare build-up (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: The main phase of solar physics (including flare-buildup) research on Shuttle/Spacelab during the 1980s centers around the use of facility instruments for multiple-user, multiple flight operations. Three main facilities are being considered: a meter-class optical telescope for visible and near-UV wavelengths, an EUV/XUV/soft X-ray facility, and a hard X-ray imaging facility (including a full-sun 5-600 keV spectrometer, a nuclear gamma ray spectrometer, and an X-ray polarimeter for the 5-100 keV range). Smaller instruments designed for specific observations and other classes of instruments such as solar monitors that are not on the facility level are also being considered.
    Keywords: SOLAR PHYSICS
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  • 15
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    The 1976 Helios and Pioneer solar conjunctions-continuing corroboration of the link between Doppler noise and integrated signal path electron density (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Observed Doppler noise (rms phase jitter) from the 1976 solar conjunctions of the Helios 1 and 2 and the Pioneer 10 and 11 spacecraft was processed with a recently developed Doppler noise model ISEDB. Good agreement is obtained between the observed data and the model. Correlation is shown between deviations from the ISEDB model and sunspot activity, but it is insufficient to be modeled. Correlation is also shown between ISEDB model deviations for (spacecraft) signal paths on the same side of the sun.
    Keywords: SOLAR PHYSICS
    Type: The Deep Space Network; p 121-137
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  • 16
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    Interplanetary disturbances caused by the August 1972 solar flares as observed by Pioneer 9 (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Pioneer 9 plasma and field observations at 0.78 AU were used as the basis of the analysis of the dynamic behavior of the interplanetary medium during early August, 1972. The following investigations were carried out: (1) energy and mass estimates for the solar flares of Aug. 2, 4, and 7; (2) shock wave characteristics; and (3) a numerical simulation of the first two flare-generated disturbances on Aug. 2, 4, and 7.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Sept. 1
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  • 17
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    Structure of the extended solar magnetic field and the sunspot cycle variation in cosmic ray intensity (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: It is proposed that a relation exists between the extent of interplanetary-magnetic-field sectors and observed variations in cosmic-ray intensity at earth. Changes that take place in the sector magnetic fields and solar polar fields during a sunspot cycle are described. It is argued that a geometrical effect arising from changes in sector-field and polar-field extent during sunspot cycles may be the principal cause of the 11-yr modulation of cosmic-ray intensity observed at earth. The fraction of the heliosphere occupied by sector fields is estimated as a function of time through an average sunspot cycle, the solid angle of the heliosphere occupied by the extended solar polar fields is plotted through the same cycle, and monthly averages of observed absolute intensities of primary cosmic rays with a rigidity greater than 0.5 GV are compared with the plot of polar-field extent. It is found that the average sunspot-cycle variation of the solid angle of the extended polar fields is rather similar to the observed variation in the flux of the cosmic rays considered.
    Keywords: SOLAR PHYSICS
    Type: Nature; 262; Aug. 26
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  • 18
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    Coronal temperatures and temperature gradients from OSO-7 spectroheliograms (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Temperatures and temperature gradients for the outer corona are obtained from brightness gradients of EUV lines that were measured with the spectroheliograph on OSO-7. Brightness gradients show considerable deviations from isothermal model calculations that include collisional excitation and photoexcitation. A negative temperature gradient that gives both positive and negative ion-abundance gradients appears to be able to account for the discrepancy. For the 284-A of Fe XV, perhaps the strongest line from the outer corona, measurements during 1972 appear to be consistent with a temperature near 2.3 million K near the equator at about 1.3 solar radii from the solar center and with temperature-gradient values near -0.7 that extend from as low as 1.2 to about 1.8 solar radii. Temperatures from strong lines of Fe XIV and Fe XVI indicate that variations of about 200,000 K exist along lines of sight where emission is appreciable. There appears to be some agreement between these results and temperature measurements from ion abundances in the solar wind and the Doppler width of the 5303-A line.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 47; Apr. 197
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  • 19
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    Limb-brightening observations from the OSO-7 satellite. II - Comparison of Abel-inverted intensities of Fe XIV and Fe XIII EUV emission lines with predictions (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Intensities of Fe XIV and Fe XIII EUV emission lines obtained at coronal locations beyond the limb by the Goddard spectroheliograph on the OSO 7 satellite have been corrected for the wavelength dependence of the instrument's sensitivity and have been Abel-inverted to provide a valid comparison with theoretical predictions for each ion. Details of the Abel-inversion procedure are given, including explicit formulas for application of Bracewell's (1956) method. The intensity ratios of pairs of lines originating from a common level are compared with expected theoretical transition probability ratios over a range of heliocentric distance; deviations in some cases yield information about adjacent unclassified lines. Comparison of the observations with predictions for Fe XIV and Fe XIII shows generally good agreement, with a few interesting discrepancies that may imply a corresponding need for more accurate collisional excitation cross sections. The same comparison yields the variation of electron density with heliocentric radius for each ion separately; the two density functions are found to agree within a factor of three.
    Keywords: SOLAR PHYSICS
    Type: Astronomy and Astrophysics; 53; 2, De; Dec. 197
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  • 20
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    On the theory of the type III burst exciter (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: In situ satellite observations of type III burst exciters at 1 AU show that the beam does not evolve into a plateau in velocity space, contrary to the prediction of quasilinear theory. The observations can be explained by a theory that includes mode coupling effects due to excitation of the parametric oscillating two-stream instability and its saturation by anomalous resistivity. The time evolution of the beam velocity distribution is included in the analysis.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 46; Feb. 197
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  • 21
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    Directivity of low frequency solar type III radio bursts (1976)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: The occurrence rate of type III solar bursts in the frequency range 4.9 MHz to 30 kHz is analyzed as a function of burst intensity and burst arrival direction. We find that (1) the occurrence rate of bursts varies inversely with the 1.5 power of the flux, and (2) the distribution of burst arrival directions at each frequency shows a significantly larger number of bursts observed west of the earth-sun line than east of it. This western excess in occurrence rate appears to be correlated with the direction of the average interplanetary magnetic field, and is interpreted as beaming of the observed burst radiation along the magnetic field direction.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 46; Feb. 197
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  • 22
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    The quiet sun chromospheric network observed from Skylab (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The paper analyzes spectra of a supergranulation cell interior and cell boundary obtained near the solar center at wavelengths between 1200 and 1560 A with a normal-incidence spectrograph aboard Skylab. Absolute intensities, relative intensities, and profiles are given for selected optically thin and optically thick lines over the cell interior, the boundary, and intermediate positions; the results are compared with spectra obtained at the limb. Characteristic lengths along the line of sight are derived for the Si III emitting region, and these are compared with the predictions of Gabriel's (1975) model. It is concluded that the present data are representative of a fairly typical cell interior and boundary, that nonthermal motions are isotropic and the same for the interior and boundary, and that the electron-density ratio between the interior and the boundary is about a factor of two or less.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 209; Oct. 1
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  • 23
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    Doppler wavelength shifts of transition zone lines measured in Skylab solar spectra (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Wavelengths of lines of the transition-zone ions Si IV, C IV, O IV, N V, and O V are observed to be redshifted relative to the wavelengths of chromospheric lines in XUV spectra obtained from the normal-incidence spectrograph on Skylab. The spectra cover the wavelength range from 1200 to 1565 A and were obtained with the slit positioned over chromospheric network and cell regions, on coronal holes, and above the limb. The network-area and coronal-hole spectra were obtained near the disk center. Only some of the spectra show redshifted transition-zone lines. The observed shifts are between 0.03 and 0.08 A, implying velocities of 15 km/s or less. The amount of wavelength shift does not always appear to be the same for lines of different ions. The shifts imply that descending plasma in the solar atmosphere produces more emission than ascending plasma at temperatures between approximately 70,000 and 200,000 K.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 205; May 1
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  • 24
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    The emission-line spectrum above the limb of the quiet sun - 1175-1940 A (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Spectra of a quiet solar region obtained at positions within and above the solar white-light limb in the wavelength region from 1175 to 1940 A are discussed. The spectra were obtained by the slit spectrograph (SO82-B) on Skylab. The spectral resolution is 0.06 A, and the projected slit area on the sun was 2 x 60 arcsec (1450 x 43500 km). Relative line intensities are presented for lines formed in the temperature region of the solar atmosphere from about 8000 to 220,000 K. Representative line profiles of both optically thin and optically thick lines are shown as a function of height above the limb. Random mass-motion velocities are deduced from the optically thin lines, and the relative intensities and profiles of the lines are discussed in terms of current theoretical models. A wavelength list with identifications is given for the spectrum obtained at +4 arcsec above the white-light limb.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal Supplement Series; 31; July 197
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  • 25
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    Solar irradiance - Total and spectral and its possible variations (1976)
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    Publication Date: 2011-08-16
    Description: The present status of our knowledge of the total and spectral irradiance of the sun is briefly reviewed. The currently accepted NASA/ASTM standard values of the solar constant and the extraterrestrial solar spectral irradiance are presented. The uncertainties in these values are relatively high. Data on the variability of the solar constant are conflicting and inconclusive. The variability of solar spectral irradiance is almost totally unknown and unexplored. Some alleged sun-weather relationships are cited in support of the need to know more precisely the variations in total and spectral solar irradiance. An overview of the solar monitoring program of NASA is presented, with special emphasis on the Solar Energy Monitor in Space (SEMIS) experiment which has been proposed for several spacecraft missions. The monitor is a combination of a solar-constant detector and a prism monochromator.
    Keywords: SOLAR PHYSICS
    Type: Applied Optics; 15; Apr. 197
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  • 26
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    Solar gamma-ray lines as probes of accelerated particle directionalities in flares (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Anisotropies of charged particles accelerated in solar flares can be studied by observing Doppler shifts of selected gamma-ray lines. The spectral shape of the 6.1-MeV line of O-16 is calculated. If the accelerated particles are isotropic, the line remains centered at an emitting-nucleus rest-frame energy of 6129.4 keV, and its width (FWHM) is about 100 keV. However, for particle anisotropies that may be produced in solar flares, the line is shifted to lower energies by about 30 to 40 keV.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Feb. 1
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  • 27
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    The emission-line spectrum above the limb of a solar coronal hole - 1175-1940 A (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Emission-line spectra of a coronal hole that coincided with the north pole of the sun are discussed which were obtained with a slit spectrograph aboard Skylab at positions within and above the solar white-light limb in the wavelength range from 1175 to 1940 A. Relative line intensities, line profiles, and full widths at half-maximum are presented for selected chromospheric and transition-zone lines observed above the present polar coronal hole. Average mass motions in the transition zone are determined as a function of electron temperature from the widths of the optically thin lines by assuming ionization equilibrium. The line intensities and profiles are compared with corresponding results deduced from spectra obtained above a quiet solar region. The coronal-hole spectra are found to imply an angular dependence for the source function as well as a radial dependence such that the source function is the smallest at the south pole and increases with decreasing solar latitude.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal Supplement Series; 31; July 197
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  • 28
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    Electron parameter correlations in high-speed streams and heat flux instabilities (1976)
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    Publication Date: 2011-08-16
    Description: Statistical electron parameter correlations associated with high-speed streams are determined with the aim of identifying one or more locally active solar wind heat flux instabilities. Evidence that points toward local regulation of the heat flux at 1 AU is presented, and the results of a search for special signatures expected from the action of the Alfven, magnetosonic, and whistler flux instabilities are discussed. It is shown that under certain conditions, the whistler mode can be active in regulating the heat flux at 1 AU.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; May 1
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  • 29
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    Solar wind speed variations - 1962-1974 (1976)
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    Publication Date: 2011-08-17
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Oct. 1
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  • 30
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    Heating of the solar chromosphere and corona. I - Generalized inhomogeneous wave equation for magnetoacoustic motions (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The generalized inhomogeneous wave equation that governs magnetoacoustic, vortical, and thermal motions in compressible fluids and that is applicable to the problem of heating of the solar chromosphere and corona is obtained. The effects of kinematic and bulk viscosity, heat conduction, Joule dissipation, and magnetic diffusivity are included. Under the usual assumptions, the generalized wave equation reduces to the well-known equations of Lighthill, Kulsrud, Phillips, and others. The major problems encountered in applying Lighthill's (1952) mechanism to sound generation in turbulent media are reviewed for both the subsonic and supersonic cases.
    Keywords: SOLAR PHYSICS
    Type: Astrophysics and Space Science; 43; Aug. 197
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  • 31
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    Doppler noise considered as a function of the signal path integration of electron density (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The hypothesis is advanced that observed Doppler noise during solar conjunctions is proportional to total columnar electron content along the signal path. This assumption leads directly to a geometrical model (ISED) for observed Doppler noise which is shown to be in very good agreement with Doppler noise data accumulated during the 1975 Pioneer 10, Pioneer 11 and Helios 1 solar conjunctions. An augmented model is constructed which quantitatively indicates correlation between earth observed sunspot activity and systematic, cyclical deviations from the ISED model.
    Keywords: SOLAR PHYSICS
    Type: The Deep Space Network; p 159-193
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  • 32
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    The solar spectrum - Wavelengths and identifications from 160 to 770 angstroms (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Jan. 15
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  • 33
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    On the nonexistence of plane-polarized large amplitude Alfven waves (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: A theorem is presented which shows that purely Alfvenic plane-polarized large-amplitude disturbances in the solar wind are not possible and will never be observed. The theorem establishes that there is no nontrivial plane-polarized magnetic-field configuration in which the parameter B-squared is constant throughout all space. It is noted, however, that more general nonplanar Alfvenic disturbances may well exist.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Jan. 1
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  • 34
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    Microscale 'Alfven waves' in the solar wind at 1 AU (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Data obtained by IMP 1 about interplanetary plasma and magnetic-field fluctuations on a scale of one hour are analyzed. It is found that linearly and circularly polarized Alfven waves were rarely present. Fluctuations having most of the characteristics of large-amplitude 'Alfven waves' and which were observed to be moving away from the sun nearly along the magnetic-field direction are shown not to have been pure transverse Alfven waves since they were accompanied by nonzero fluctuations in the magnetic-field intensity. It is suggested that the fluctuations may have been nonlinear elliptically polarized Alfven waves coupled to the fast mode and moving through a magnetic field that is nonuniform on a scale not exceeding about 0.01 AU.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Jan. 1
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  • 35
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    A shock surface geometry - The February 15-16, 1967, event (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: An estimated shape is presented for the surface of the flare-associated interplanetary shock of February 15-16, 1967, as seen in the ecliptic-plane cross section. The estimate is based on observations by Explorer 33 and Pioneers 6 and 7. The estimated shock normal at the Explorer 33 position is obtained by a least-squares shock parameter-fitting procedure for that satellite's data; the shock normal at the Pioneer 7 position is found by using the magnetic coplanarity theorem and magnetic-field data. The average shock speed from the sun to each spacecraft is determined along with the local speed at Explorer 33 and the relations between these speeds and the position of the initiating solar flare. The Explorer 33 shock normal is found to be severely inclined and not typical of interplanetary shocks. It is shown that the curvature of the shock surface in the ecliptic plane near the earth-Pioneer 7 region is consistent with a radius of not more than 0.4 AU.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Jan. 1
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  • 36
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    Formation of iron sulphide in solar nebula (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Noting that the iron sulfide in the Orgueil carbonaceous meteorite is an Fe-deficient monosulfide (pyrrhotite), it is suggested that such mineral chemistry is inconsistent with equilibrium condensation of the solar nebula and that the course of condensation may have been modified by kinetic effects. The effect of Ni on the reaction between Fe and S to produce FeS is examined, and possible reasons are considered for the fact that the cited meteorite differs in both crystal structure and Ni content from the predictions of equilibrium condensation. It is proposed that sulfide formation in the solar nebula may have been inhibited by sluggish diffusion, so that sulfur began to react with previously condensed troilite to form pyrrhotite. On this basis, observations of the Orgueil sulfides are shown to suggest that the course of solar-system condensation was modified by kinetic effects below about 700 K and that equilibrium may not have been achieved.
    Keywords: SOLAR PHYSICS
    Type: Nature; 259; Jan. 22
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  • 37
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    Kitt Peak 60-cm vacuum telescope (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: A major new solar-research telescope conceived and built during a time of budget restraint is described. The observation of magnetic and velocity (circulation) field structure on a synoptic basis and with diffraction-limited resolution is the aim. New optical features include the use of oversize mirrors and windows to avoid thermal edge effects and the placement of the coelostat feed outside the vacuum, mainly for economy. The site selected has prevailing winds that clear thermals from these mirrors. Test data in the form of the system MTF and optical transmission, together with examples of full disk magnetograms and photoheliograms, show present performance capability. Measured MTF indicates a response of 0.2 at 1 sec of arc (whereas diffraction-limited response would be about 0.8). System transmission, including the accompanying spectrograph, is only 2-3% (wavelength 0.44-1.1 microns). Thus, both the optical quality and efficiency are subject to improvement.
    Keywords: SOLAR PHYSICS
    Type: Applied Optics; 15; Jan. 197
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  • 38
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    Solar cycle evolution of high-speed solar wind streams (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: Large amplitude high-speed solar wind streams and streams with maximum speeds in excess of 700 km/sec are far more common in years of declining and minimum solar activity than near solar maximum. Further, the broadest solar wind streams observed directly with space probes during the years 1962-1974 occurred near solar minimum in 1974. Changes in the frequency and nature of solar wind stream structures at the orbit of earth appear to be directly related to the long-term evolution of regions of low density in the solar corona.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 207; Aug. 1
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  • 39
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    Electromagnetic instabilities driven by unequal proton beams in the solar wind (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The paper sets forth a numerical investigation of the linear dispersion relation for typical solar wind conditions at 1 AU during those times (high-speed streams) when a secondary beam of protons drifting relative to the main proton component is present. Three beam-driven instabilities were found to occur as the beam drift velocity approaches the Alfven speed: (1) a pure, field-aligned magnetosonic wave that is most important at relatively high beta and/or high beam drift speeds; (2) an oblique magnetosonic wave having highest growth rates 15-30 deg from the magnetic field; and (3) an oblique Alfven wave having maximum growth rates at increasing angle to the magnetic field. The linear growth rates for the field-aligned magnetosonic and the Alfven oblique modes are investigated as a function of relative beam density, varying anisotropic pitch angle distributions for the various components, electron temperature, and electron heat flux.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; June 1
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  • 40
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    Low frequency radio observations of the solar wind near the moon (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The RAE-2 lunar orbiter often measures sporadic 20-40 dB intensity increases in the frequency range of 25-110 kHz. Numerous examples of the disappearance of this intense noise during occultations of the sun have been observed. The average position of these occultations coincides with the average location of the plasma cavity above the nightside of the moon. We suggest that the observed high noise levels may be generated near the spacecraft by a disturbed solar wind electron population in the vicinity of the moon.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 3; June 197
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  • 41
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    Timing of solar cycles by rigid internal rotations (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Description: The so-called 11-year cycle of solar activity is really more complex and contains many periods of greatly different lengths. Periods as long as 178 years and as short as 3.1 years are predicted by a theory based on beats between rigidly rotating, inertially oscillating g-modes inside the sun. Most of the beat periods are then confirmed to about 1 percent accuracy in sunspot observations. Since the agreement is of high statistical significance, one can conclude that approximate alignment of major solar oscillation modes contributes to high solar activity. The theory receives further support when tested against an independent class of observations - the large-scale magnetic sector structure. Predicted rotation rates of at least four solar oscillation modes are detected in the sector data with discrepancies all less than 0.3 percent. As a by-product of these successful fits to observation, the mean rotation of the entire solar mass becomes known. Its rotation frequency is 4.49 by 10 to the -7th power Hz, which is a sidereal period of 25.8 days. Magnetic fields have played no role in calculating the length of any of these solar cycles.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 205; Apr. 15
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  • 42
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    Comment on the paper 'Solution of one-fluid model equations with short range retarding magnetic forces for the quiet solar wind' by Cuperman and Harten (1976)
    In:  Other Sources
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    Publication Date: 2011-08-16
    Keywords: SOLAR PHYSICS
    Type: Astrophysics and Space Science; 40; Mar. 197
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  • 43
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    The large-scale magnetic field in the solar wind (1976)
    In:  CASI
    Details
    Publication Date: 2016-05-14
    Description: A literature review is presented of theoretical models of the interaction of the solar wind and interplanetary magnetic fields. Observations of interplanetary magnetic fields by the IMP and OSO spacecraft are discussed. The causes for cosmic ray variations (Forbush decreases) by the solar wind are examined. The model of Parker is emphasized. This model shows the three dimensional magnetic field lines of the solar wind to have the form of spirals wrapped on cones. It is concluded that an out-of-the-ecliptic solar probe mission would allow the testing and verification of the various theoretical models examined. Diagrams of the various models are shown.
    Keywords: SOLAR PHYSICS
    Type: Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 143-165
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  • 44
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    Numerical study of some solar-wind interaction models with space objects (1976)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: The considerable variety of atmospheric and magnetic field properties possessed by the planets results in a corresponding variety of flow details, and a remarkably rich field of comparative study of solar wind flow around major objects in the solar system. It is the purpose of this paper to present a review of the fluid aspects of these flows and how they are approximated to obtain tractable mathematical problems, and a commentary on possibilities for further improvements and on some misconceptions that have appeared in applications of the results.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Solar-Wind Interaction with the Planets Mercury, Venus, and Mars; p 121-133
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  • 45
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    On the nature of the solar-wind-Mars interaction (1976)
    In:  CASI
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    Publication Date: 2016-06-07
    Description: Plasma measurements near Mars on the U.S.S.R. Mars-2, -3, and -5 spacecraft are considered. The data are compared with simultaneous magnetic measurements. Strong evidence is obtained in favor of a direct interaction and mass exchange between the solar wind plasma and the gaseous envelope of Mars.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Solar-Wind Interaction with the Planets Mercury, Venus, and Mars; p 21-40
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  • 46
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    Coronal propagation: Variations with solar longitude and latitude (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Observational results on the East-West effect are summarized and discussed in the context of existing models of coronal propagation. The variation of the number of events with solar longitude is shown to be surprisingly similar for particles covering a large interval of rigidities. Also, over large longitudinal distances, time delays to the event onset and maximum intensity are independent of energy and velocity. This has important implications and will require probably a transport process which is determined by fundamental properties of solar magnetic fields, e.g. reconnection processes between open and closed field configurations. The relative role of open and closed field configurations is extensively discussed. Some evidence is presented that the acceleration of protons to higher (approximately 10 MeV) energies is related with a shock wave traveling in the solar atmosphere. The importance of measurements performed from spacecraft out-of-the-ecliptic plane is stressed.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 261-299
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  • 47
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    Latitudinal properties of the solar wind from studies of ionic comet tails (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: A statistical analysis is presented of the orientations of ionic comet tails in the solar wind. The analysis indicates that the radial solar wind speed is not necessarily higher near the solar poles than near the equator. The results refer to a long-term, global flow pattern and do not refer to short-term variations of solar wind speed.
    Keywords: SOLAR PHYSICS
    Type: Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 95-107
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  • 48
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    The 3-D solar radioastronomy and the structure of the corona and the solar wind (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: The mechanism causing solar radio bursts (1 and 111) is examined. It is proposed that a nonthermal energy source is responsible for the bursts; nonthermal energy is converted into electromagnetic energy. The advantages are examined for an out-of-the-ecliptic solar probe mission, which is proposed as a means of stereoscopically viewing solar radio bursts, solar magnetic fields, coronal structure, and the solar wind.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 65-83
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  • 49
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    Solar magnetic fields and the corona (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Results from a seminar on the role of solar magnetic fields in determining the structure of the corona and interplanetary medium are presented. Some topics considered are: (1) polar regions of the sun which have identical magnetic configurations but display a vastly different appearance in the corona, (2) the influence of latitude on coronal and interplanetary microstructure, and (3) the role of the corona in contributing to the solar wind. It is proposed that an out-of-the-ecliptic solar probe mission would provide needed information on the above topics, and the study of solar activity in general.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 59-64
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  • 50
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    Implications of Saito's coronal density model on the polar solar wind flow and heavy ion abundances (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: A comparison of polar solar wind proton flux upper limits derived using a coronal density model, with Lyman alpha measurements of the length of the neutral H tail of comet Bennet at high latitudes, shows that either extended heating beyond 2 solar radii is necessary some of the time or that the model's polar densities are too low. Whichever possibility is the case, the fact that the solar wind particle flux does not appear to decrease with increasing latitude indicates that the heavy element content of the high latitude wind may be similar to that observed in the ecliptic. It was then shown that solar wind heavy ion observations at high latitudes allow a determination of the electron temperature at heights which bracket the nominal location of the coronal temperature maximum thus providing information concerning the magnitude and extent of mechanical dissipation in the intermediate corona.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 108-142
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  • 51
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    Out-of-ecliptic studies of coronal holes and their relation to the solar wind (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: The advantages of observing coronal holes of the sun above the solar ecliptic plane by a solar probe are discussed. Also discussed are the size of coronal holes, their temperature, and magnetic fields associated with the holes. The role of coronal holes in contributing to the solar wind is examined. Data and observations on coronal holes from Skylab and OSO are treated. It is concluded that an out-of-the-ecliptic solar probe mission would greatly add to the understanding of coronal holes (at high latitudes) thus adding a new perspective to the observation of these phenomena. (Photographs of the sun taken by Skylab are shown).
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 48-58
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  • 52
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    High-temperature flare lines in the solar spectrum 171 A-630 A (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 205; Apr. 1
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  • 53
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    Solar-wind tritium limit and the mixing rate of the solar atmosphere (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Tritium has been measured, in Surveyor 3 samples, some of which were adjacent to those in which solar-wind-implanted He-4 had previously been measured. Little of the H-3 can be attributed to solar-wind implantation. The upper limit for the H-3/He-4 ratio in the solar wind is four times ten to the minus tenth power and corresponds to a H-3/H-1 limit of two times ten to the minus eleventh power. This limit imposes a requirement on the mixing rate in the solar atmosphere if the H-3 production rate in solar-surface nuclear reactions is greater than 160 sq cm/sec.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 205; Apr. 1
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  • 54
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    A.t.m. observations on the X u.v. emission from solar flares (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The paper summarizes observations of selected solar flares made with a far-UV spectroheliograph (190-465 A) and a UV spectrograph (900-1900 A) aboard Skylab. The emission lines used in the present analysis are identified, and three events are described in detail: the flare of June 15, 1973, a small subflare observed on August 9, 1973, and the flare of January 21, 1974. Ultraviolet images of two other events are also presented in an attempt to sketch a general picture of a flare as seen in this spectral region. It is found that a small kernel seems to be the source of the primary energy release of a flare. The size, electron density, and ion temperature of a typical kernel are estimated, and it is noted that hot clouds of coronal gas at 20 million K surrounded the observed kernels. It is speculated that flare kernels might be very thin channels through which high-energy particles, originating in deep layers, are ejected into the corona.
    Keywords: SOLAR PHYSICS
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  • 55
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    Depletion of solar wind plasma near a planetary boundary (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A mathematical model is presented that describes the squeezing of solar wind plasma out along interplanetary magnetic field lines in the region between the bow shock and the effective planetary boundary (in the case of the earth, the magnetopause). In the absence of local magnetic merging the squeezing process should create a 'depletion layer', a region of very low plasma density just outside the magnetopause. Numerical solutions are obtained for the dimensionless magnetohydrodynamic equations describing this depletion process for the case where the solar wind magnetic field is perpendicular to the solar wind flow direction. For the case of the earth, the theory predicts that the density should be reduced by a factor exceeding 2 in a layer about 700-1300 km thick if the Alfven Mach number in the solar wind, is equal to 8. Scaling of the model calculations to Venus and Mars suggests layer thicknesses about 1/10 and 1/15 those of the earth, respectively, neglecting diffusion and ionospheric effects.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Apr. 1
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  • 56
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    Radial variation of solar-wind parameters (1976)
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    Publication Date: 2019-06-27
    Description: It is demonstrated that since fluctuations in the solar wind are not small, they can have important effects on the observed average values of parameters in the solar wind and their radial variation. The effect is distinct from the dynamical effect of waves and turbulence, and results from the averaging process. It is concluded that, for example, the average density of the solar wind need not vary as the inverse square of distance, even if the average velocity is constant and radial. The effect on thermal anisotropies might also be important. The magnitudes of the effects depend on presently unknown correlations between fluctuations in the solar wind.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 3; Mar. 197
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  • 57
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    Observations of a high-energy ion shock spike in interplanetary space (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Observations are reported of a high-energy ion shock spike extending in energy to more than 25 MeV for protons, more than 4.3 MeV/nuc for alpha particles, and more than 1.6 MeV/nuc for medium nuclei with Z of at least 6. The measurements were obtained in the course of a solar-particle event on September 15, 1975, by the IMP-7 and IMP-8 spacecraft. It is shown that the observations can be reasonably accounted for by intensive acceleration of charged particles at an 'almost' perpendicular interplanetary shock wave. The data are inconsistent with a one-step d.c.-type acceleration process.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 3; Mar. 197
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  • 58
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    Multistream and Monte Carlo calculations of the sun's aureole (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The scattered UV intensities in the sun's aureole are calculated using both a multi-stream scattering method and a Monte Carlo approach. Angular distributions for both Rayleigh and aerosol scatterings are obtained with a realistic atmospheric model. Moderate- and sharply-forward-peaked phase functions of aerosol scattering, corresponding to realistic analytic size distributions, are incorporated. Results from the two independent calculations are in reasonable agreement for a realistic atmospheric model. The results indicate that the scattered UV intensity in the sun's aureole is about four orders smaller than the transmitted intensity while the scattered intensity for pure Rayleigh scattering is only 1-10 millionths times that of the transmitted sun. Based on these intensity ratios, we estimate that the integrated scattered contributions from the aureole to a well-collimated sun photometer of acceptance aperture 2-3 deg are below about 1% of the direct contribution.
    Keywords: SOLAR PHYSICS
    Type: Journal of the Atmospheric Sciences; 33; Mar. 197
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  • 59
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    Structure of the solar chromosphere. II - The underlying photosphere and temperature-minimum region (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The paper presents a non-LTE empirical model of the quiet solar photosphere and the temperature-minimum region. The continuous spectrum computed from this model is in good overall agreement with available disk-center observations throughout the wavelength range from 0.125 to 500 microns. It is found that (1) absolute-intensity measurements are needed in the range between 1 and 2 microns to establish the structure of the deepest observable layers; (2) absolute-intensity or flux measurements are needed in the range between 20 and 200 microns to determine whether the minimum solar temperature occurring between the photosphere and the chromosphere is as low as indicated by present observations or much higher, as recent theoretical predictions indicate; (3) studies of the far-ultraviolet spectrum based on the assumption of LTE can be substantially in error; and (4) line opacity seems to account for the 'missing opacity' in the ultraviolet.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal Supplement Series; 30; Jan. 197
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  • 60
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    Hydraulic concentration of magnetic fields in the solar photosphere. III - Fields of one or two kilogauss (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Detailed analysis of weak and strong lines suggests that the magnetic fields in isolated intense flux tubes in supergranule boundaries in the solar photosphere may be as large as 2000 gauss. This paper is a concise systematic review of hydrodynamic effects that might compress a magnetic field to great intensity. The properties of force-free fields are reviewed to show that they do not contribute to concentration of magnetic fields, in spite of the popular notion to the contrary. Of the seven effects considered, it is concluded that only cooling of the gas within the field can produce the high field densities inferred from observation. It is shown that inhibition of convection appears not to possess the necessary qualitative cooling features and that overstability, generating transverse hydromagnetic waves - essentially Alfven waves - is the only way to account for the cooling and field intensification.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 204; Feb. 15
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  • 61
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    Spectroscopic evidence for a higher rotation rate of magnetized plasma at the solar photosphere (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Feb. 1
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  • 62
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    A two-region model of the solar wind including azimuthal velocity (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The two-region model of the solar wind divides the interplanetary space into two regions: it assumes that the solar wind is one-fluid in an inner region within 0.4 AU and two-fluid in an outer region beyond 0.4 AU. This paper includes the angular motion of the solar wind in the two-region model. The flow in the one-fluid region is governed by the one-fluid magnetohydrodynamic equations. The second and third moment equations of the Vlasov equation together with other conservation equations are used to describe the solar-wind flow in the two-fluid region. The predicted azimuthal velocity at 1 AU is less than 2 km/s. All other macroscopic and microscopic properties from this model are in good agreement with experimental quiet-time observations at 1 AU. The numerical results also confirm that when the azimuthal velocity is included in the analysis, the amount of magnetic-field energy converted into kinetic energy in the solar wind is only a small fraction of the total expansion energy flux and has little effect upon the final radial expansion velocity.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Feb. 1
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    Spectroscopic studies of the solar corona at X-ray wavelengths (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The spatial distribution of emission in several X-ray lines is discussed with emphasis on temperature dependence and association with active regions. Results are presented for the trio of helium-like O VII lines which demonstrate (1) a spatial variation in the density-dependent forbidden-to-intersystem line ratio, and (2) a strong spatial variation in the intensity of the O VII resonance line relative to the optically forbidden transitions. The second effect appears to be caused by resonance scattering by material in the line of sight.
    Keywords: SOLAR PHYSICS
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    Evidence of a large-scale gradient in the solar wind velocity (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Measurements of the solar wind velocity are compared at two widely separated locations, using plasma data obtained by Mariner 5, en route to Venus, and with the near-earth satellites Explorer 33, 34, and 35. A previous study of the propagation of interplanetary sector boundaries between Mariner and the earth had implied the existence of large scale velocity gradient which was interpreted as a latitude gradient of approximately 13 km/sec per degree of latitude. The results of the present investigation in which the earlier results were extended to the overall solar wind, without regard to the presence of sector boundaries, suggests that a latitude dependence of the solar wind velocity is the most plausible interpretation of the large-scale velocity gradient.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; May 1
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    Solar limb brightening in submillimeter wavelengths (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Differential two-beam scans of the sun in submillimeter wavelengths (350 microns to 1 millimeter) indicate limb brightening approaching 1 percent when the cosine of the angle from the normal equals 0.60. The observations also show considerable chromospheric structure, both in active and quiet regions, but with less relative amplitude than at millimeter and centimeter wavelengths. The limited angular resolution of the observing system, together with photometric errors due to fluctuating atmospheric transparency, make the brightness profile of the extreme limb uncertain. The observed degree of limb brightening is considerably less than that consistent with spherically symmetric model atmospheres based on continuum brightness-temperature measurements. The suppression of limb brightening suggests the existence of irregular granular structure with both horizontal and vertical characteristic sizes of the order of 1500 km. High-resolution images in the wings of the K-line show granular structure of about this horizontal scale.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 203; Feb. 1
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  • 66
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    Non-LTE profiles of strong solar lines (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The complete linearization method is applied to the formation of strong lines in the solar atmosphere. Transitions in Na(I), Mg(I), Ca(I), Mg(II), and Ca(II) are computed with a standard atmosphere and microturbulent velocity model. The computed profiles are compared to observations at disk center.
    Keywords: SOLAR PHYSICS
    Type: Contrib. of the Observatory of N. Mex. State Univ., Vol. 1, No. 4,; p 110-122
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  • 67
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    Results of coronal hole research: An overview (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: An overview of the last 10 years of coronal hole research, in particular since 1970, is presented. The findings of the early investigations and the more recent results obtained with Skylab/Apollo Telescope Mount instrumentation are discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-73317
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    Observations of limb flares with a soft X-ray telescope (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The structure and evolution of 26 limb flares have been observed with a soft X-ray telescope flown on Skylab. The results are: (1) One or more well defined loops were the only structures of flare intensity observed during the rise phase and near flare maximum, except for knots which were close to the resolution of the telescope; (2) the flare core features were always sharply defined during rise phase; and (3) for the twenty events which contained loops, the geometry of the structure near maximum was that of a loop in ten cases, a loop with a spike at the top in four cases, a cusp or triangle in four cases, and a cusp combined with a spike in another two cases. Based on observation of the original film, it is suggested that flares which underwent large scale deformations had become unstable to MHD kinks. This implies that these flares occurred in magnetic flux tubes through which significant currents were flowing.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-144329 , ATR-76(7405)-2
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    A direct measurement of the charge states of energetic iron emitted by the sun (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The charge states of energetic iron have been measured directly for the first time in a solar particle event. In the energy interval 0.01 to 0.25 MeV per nucleon, iron is not fully stripped but has a mean ionization state of 11.6. This value is remarkably similar to the mean ionization state of iron in the quiet solar wind and suggests that the charge states were "frozen-in" at a coronal temperature of approximately 1,500,000 K.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-148144 , TR-76-113 , PUBL-76-259
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    Time dispersion of energetic solar particles, unexpected velocity and species dependence (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: The intensity-time behavior for protons and helium, as well as for carbon, oxygen and iron ions was measured following the 1974 September 19 solar flare for energies between 0.5 and approximately 5 MeV per nucleon. The profiles displayed a time dispersion which is inversely proportional to velocity for each individual species. In addition, at a given velocity the time dispersion also depended on the charge to mass ratio of the ion. Based on this latter dependence, it was concluded that while carbon and oxygen are essentially fully stripped, iron nuclei are not, having an effective charge Q = 10 + or - 5. The observed dispersion cannot be explained by purely rigidity dependent diffusive propagation.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-148143 , TR-76-114 , PHYSICS-PUB-76-260
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    A solar flare bibliography for 1973 through 1975 (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The open literature for 1973 through 1975 was searched for publications with flare information that might pertain to the analysis of the Skylab data. The resulting bibliography is divided into three sections: (1) results from Skylab, (2) results from ground-based data during the Skylab time period, (3) other pertinent publications.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-73312
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  • 72
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    Magnetohydrodynamic and gasdynamic aspects of solar-wind flow around terrestrial planets: A critical review (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Problems in space physics are discussed whose models, in simplified form, reduce to a supersonic flow scheme with a detached shock wave, namely: (1) solar wind interaction with an intrinsic planetary magnetic field; (2) solar wind interaction with the ionized component of the atmosphere of a comet; and (3) solar wind interaction with the ionosphere of a planet which does not possess its own magnetic field. The numerical study of the above problems is performed with the use of magnetogasdynamic equations for an ideal single fluid model. From the physical veiwpoint, the problems are solved in terms of as simple phenomena as possible; the principal objective is to make recently developed methods of numerical analysis of mixed flows applicable to space physics problems.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Solar-Wind Interaction with the Planets Mercury, Venus, and Mars; p 135-149
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  • 73
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    Magnetic holes in the solar wind (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: An analysis is presented of high resolution interplanetary magnetic field measurements from the magnetometer on Explorer 43 which showed that low magnetic field intensities in the solar wind at 1 AU occur as distinct depressions or 'holes'. These magnetic holes are new kinetic-scale phenomena, having a characteristic dimension on the order of 20,000 km. They occurred at a rate of 1.5/day in the 18-day time span (March 18 to April 6, 1971) that was analyzed. Most of the magnetic holes are characterized by both a depression in the absolute value of the magnetic field, and a change in the magnetic field direction; some of these are possibly the result of magnetic merging. However, in other cases the magnetic field direction does not change; such holes are not due to magnetic merging, but might be a diamagnetic effect due to localized plasma inhomogeneities.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-71109 , X-692-76-90
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  • 74
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    Three dimensional aspects of interplanetary shock waves (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: Most of the interplanetary shock waves observed with 1 AU of the sun originate from some short lived solar event, such as a solar flare, and then propagate out as a more-or-less spherical shock wave until they leave the solar system. Beyond 1 AU another class of interplanetary shock wave becomes common--the corotating shock pair formed by the interaction of long lived solar wind streams. The three dimensional geometry of these two classes of interplanetary shocks is discussed. Also discussed are how these geometries can be statistically studied with an out-of-the-ecliptic mission. Diagrams of shock wave propagation are shown. Also given are numerical examples of shock wave propagation.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 166-187
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    H alpha observations of the 12 August 1975 type 3-RS bursts (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: H alpha filtergram observations of a number of the Type III-RS (reverse slope) bursts that occurred on August 12, 1975 are presented. Solar radio emission was peculiar on that date in that a large number, and proportion, of the usually rare reverse slope bursts were observed. The radio bursts are shown to coincide in time with a homologous set of H alpha flares located at the limbward edge of spot group Mt. Wilson 19598. A model is proposed in which the reverse slope bursts are the downward branches of U bursts, whose upward branches are hidden behind the coronal density enhancement over the spot group.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-147098 , BBSO-0155
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  • 76
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    AE 6: A model environment of trapped electrons for solar maximum (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A projected inner zone electron model environment, AE 6, for the epoch 1980 is presented. It is intended to provide estimates of mission fluxes that spacecraft will encounter in the coming solar maximum years. AE 6 is presented by graphs of omnidirectional integral flux as a function of L shell, the ambient magnetic field B, and the energy E. Results of orbital integrations for altitudes from 150 n.m. to 18,000 n.m. are given for circular orbits with four different inclinations, using the AE 6 and the AE 4 solar maximum models for the inner and outer zones, respectively. The derivation of AE 6 is described, and a brief comparison is given of the radial profiles of equatorial fluxes from several related models. A short summary of the associated computer programs is included.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-72597 , NSSDC/WDC-A-R&S-76-04
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    Atlas of Skylab ATM/S056 super-long exposures and stepped-image frames (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A description is given of Skylab and exposure information regarding the S-L pictures is tabulated. Frames which display stepped images are identified.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-64992
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    Gamma-ray and microwave evidence for two phases of acceleration in solar flares (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Relativistic electrons in large solar flares produce gamma ray continuum by bremsstrahlung and microwave emission by gyrosynchrotron radiation. Using observations of the 1972, August 4 flare, the electron spectrum and the physical properties of the common emitting region of these radiations were evaluated. Information was also obtained on energetic protons in this flare by using gamma ray lines. From the electron spectrum, the proton-to-electron ratio, and the time dependences of the microwave emission, the 2.2 MeV line and the gamma ray continuum, it was concluded that in large solar flares relativistic electrons and energetic nuclei are accelerated by a mechanism which is different from the mechanism which accelerates approximately less than 100 keV electrons in flares.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-71083 , X-660-76-58
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    Atlas of Skylab ATM/S056 coronal hole observations (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: An atlas of coronal hole observations (Patrol Long and Single Frame Long Filter 3) recorded by the Skylab Apollo Telescope Mount/SO56 X-ray Telescope during the first two manned missions is presented. A total of 279 operations (excluding super long frames) were determined. Comparisons are made between coronal hole observations performed in the first manned mission and those in the second manned mission, and between a super long filter 3 image and a typical single frame (or Patrol) long image. Additional studies to enhance the S056 coronal hole observations and perhaps to extend coverage into the last manned mission are suggested. The data presented are in preliminary form.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-64994
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  • 80
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    Energies of backstreaming protons in the foreshock (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A predicted pattern of energy vs detector location in the cislunar region is displayed for protons of zero pitch angle traveling upstream away from the quasi-parallel bow shock. The pattern is implied by upstream wave boundary properties. In the solar ecliptic, protons are estimated to have a minimum of 1.1 times the solar wind bulk energy E sub SW when the wave boundary is in the early morning sector and a maximum of 8.2 E sub SW when the boundary is near the predawn flank.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-147981 , TRW-29506-6002-RU-00
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    Measures of the solar spectral irradiance between 1200 and 3000 A (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Tabulated data on solar flux measurements are presented. The measurements, taken from balloons, rockets and satellites, are not new data, but have been critically re-evaluated. The eleven year sunspot cycle is discussed. Also discussed is the brightness temperature. The effect of solar radiation at various wavelengths, on the photochemistry of stratospheric ozone is briefly discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-71172 , X-912-76-171
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    A mechanism for inducing climatic variations through ozone destruction: Screening of galactic cosmic rays by solar and terrestrial magnetic fields (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A perturbation analysis, allowing for temperature and opacity feedbacks, is developed to calculate depletions in the O3 abundance and reductions of stratospheric solar heating that result from increases in NOx concentration. A pair of perturbation coefficients give the reduction in O3 and temperature through the stratosphere for a specified NOx increase. This type of analysis illustrates the tendency for various levels to self-heal when a perturbation occurs. Physical arguments indicate that the expected sign of the climatic effect is correct, with colder surface temperatures produced by reduced magnetic shielding. In addition, four qualitative reasons are suggested for thinking that significant ozone reductions by cosmic ray influxes will lead to an increased terrestrial albedo from stratospheric condensation. In this view, long-term (approximately 10,000 years) climatic changes have resulted from secular geomagnetic variations while shorter (approximately 100 years) excursions are related to changes in solar activity.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-148695
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    Ionization effects due to solar flare on terrestrial ionosphere (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Sudden frequency deviation ionospheric disturbances related to the flares of May 18 and 19, 1973 were observed from the NASA/MSFC high frequency Doppler sounder array system in Huntsville, Alabama. The results are compared with those observed at Table Mountain near Boulder, Colorado and at the University of Hawaii.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-148476 , UAH-RR-188
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    History of solar-terrestrial relations as deduced from spacecraft and geomagnetic data: Solar M regions (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: This brief history is organized around the long problem of the solar M region, i.e. the structure on the sun that is responsible for recurrent geomagnetic disturbances.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-148565 , SU-IPR-665
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    Solar cosmic ray measurements at high heliocentric latitudes (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A brief review is presented of what might result from a program of solar cosmic ray observations on 'out-of-the-ecliptic' spacecraft. The following topics are discussed: (1) The magnetic fields of the sun at high latitudes, (2) propagation of fast charged particles in the solar corona and in interplanetary space at high latitudes, (3) origin of interplanetary particle populations and the solar wind, (4) other particle phenomena in interplanetary space (e.g., acceleration of shock waves), and (5) effect of spacecraft mission characteristics on solar cosmic ray studies at high latitudes. Maps of polar coronal magnetic fields are shown.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 231-260
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    IPS observations of the solar wind speed out of the ecliptic (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Interplanetary scintillation observations from 1971-1975 show that the average solar wind speed increases away from the solar equator, with a mean gradient of 2.1 km/s per degree. These results are compared with spacecraft observations over the + or - 7 deg attainable in the ecliptic and with those deduced from comet tails. The role of temporal variations, especially those caused by latitude dependent solar wind streams, is emphasized, and this points to the need for extensive ecliptic and ground-based observations during an out-of-the-ecliptic spacecraft mission.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 84-94
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    Experiments out of the solar system ecliptic plane: An introduction to the ecliptic mission (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: Mission planning by NASA and ESA for the 1980 timeframe to observe the sun from an angle other than the solar ecliptic plane is discussed. Such missions will aid in a more thorough understanding of the sun, interplanetary space, and their influence on the earth. Jupiter swing-by techniques (first achieved by Pioneer 10) are proposed as a means of achieving an out-of-the-ecliptic mission for solar studies. Spacecraft trajectories are illustrated for a dual Pioneer spacecraft mission to observe the sun.
    Keywords: SOLAR PHYSICS
    Type: NASA. Goddard Space Flight Center Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 10-36
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  • 88
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    Production of a short-lived filament by a surge (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: A large surge was observed on September 17, 1971 part of which, after travelling 200,000 km across the surface, returned to the surface to form a filament. The filament lasted about 30 minutes, then rose up and returned to the source of the surge. This was interpreted as the filling of a semi-stable magnetic trap. Analysis of the microwave radio burst showed it to have been produced by a source optically thick at 8,800 MHz, with area 4 (arc min)squared and T approximately 275,000 deg, N squared sub eV approximately 7 x 10 to the 48th power. The soft x-ray burst showed a component at 12 x 1,00.000 deg with N squared sub eV approximately 3 x 10 to the 48th power.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-147090 , BBSO-0154
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  • 89
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    The lifetime and evolution of fibrils (1976)
    In:  CASI
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    Publication Date: 2019-06-27
    Description: A detailed study was made of the lifetimes and evolution of fibrils in McMath 12417, using high resolution filtergrams in H alpha and CaII K made at Big Bear Solar Observatory. It was found that the lifetime of a fibril increases monotonically with its length. This relationship, together with the form of the variation of fibril lengths as a function of time, suggests that fibrils result from material being impulsively injected into magnetic field lines at approximately 30 km/sec, and returning under gravity. The lifetimes and apparent lengths of fibrils are then a function of the inclination of the field lines only. A study of wavelength scans through the H alpha line confirms that the apparent expansion and contraction of fibrils represents true mass motion.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-147103 , BBSO-0156
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  • 90
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    Formation of the 0.511.-MeV line in solar flares (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The gamma-ray line produced at 0.51-MeV was studied and is shown to be the result of either of free annihilation of positrons with electrons or of the decay of positronium by 2-photon emission. Positron annihilation from the bound state of positronium may also proceed by 3-photon emission, resulting in a continuum with energies up to 0.51-MeV. Accurate calculations of the rates of free annihilation and positronium formation in a solar-flare plasma are presented. Estimates of the positronium-formulation rates by charge exchange and the rates of dissociation and quenching are also considered. The temperature and density dependence of the ratio of 3-photon to 2-photon emission was obtained. It is shown that when the ratio of free electrons to neutral atoms in the plasma is approximately unity or greater, the Doppler width of the 0.51-MeV line is a function of the temperature of the annihilation region. For the small ion densities characteristics of the photosphere, the width is predominantly a function of the density.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-71066 , X-682-76-6
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  • 91
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    The relative abundance of neon and magnesium in the solar corona (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A technique is proposed for specifically determining the relative solar coronal abundance of neon and magnesium. The relative abundance is calculated directly from the relative intensity of the resonance lines of Ne X (12.134A) and Mg XI (9.169A) without the need for the development of a detailed model of the thermal structure of the corona. Moderate resolution Bragg crystal spectrometer results from the OVI-10 satellite were used to determine a coronal neon to magnesium relative abundance of 1.47 + or - 0.38. The application of this technique to a recent higher resolution rocket observation gave an abundance ratio of approximately 0.93 + or - 0.15.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-146394 , SU-IPR-650
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  • 92
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    The August 1972 solar-terrestrial events - Solar wind plasma observations (1976)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Solar-wind observations associated with the enhanced levels of solar activity in August 1972 are reviewed with emphasis on recent analyses which more unambiguously characterize the changes in the interplanetary medium. Observations from Pioneer 9 at about 0.8 AU, Pioneer 10 at 2.2 AU, and in the vicinity of earth are reviewed and reinterpreted in the light of new data. Recent calculations of local shock velocities are reviewed, and their implications are discussed. These results indicate that, contrary to previously published observations, there is no significant deceleration of the interplanetary shocks between 0.8 AU and 2.2 AU.
    Keywords: SOLAR PHYSICS
    Type: Space Science Reviews; 19; Oct
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  • 93
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    Influence of magnetic field structure on the conduction cooling of flare loops (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: A simple model facilitates calculation of the influence of magnetic-field configuration on the conduction cooling rate of a hot post-flare coronal plasma. The magnetic field is taken to be that produced by a line dipole or point dipole at an arbitrary depth below the chromosphere. For the high temperatures (at least 10 million K) produced by flares, the plasma may remain static and isobaric. The influence of the field is such as to increase the heat flux (per unit area) into the chromosphere, but to decrease the total conduction cooling of the flare plasma. This leads to a significant enhancement of the total energy radiated by the flare plasma.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 49; Aug. 197
    Format: text
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  • 94
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    The spatial structure of a solar flare in soft X-rays and centimetric wavelengths (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: High-resolution images of the decay phase of a soft X-ray flare observed by the S-054 experiment on Skylab are compared with interferometric scans of the radio burst obtained simultaneously at 2.8 cm. The spatial resolution of the radio instrument in one direction, although lower than the X-ray telescope resolution, is high enough for a detailed comparison. The comparison clarifies the relationship between the sources of soft X-ray and thermal radio emission in solar flares. The X-ray emission is localized in a looplike structure which appears spatially coincident with the rapidly varying component of the radio burst. The more stable components of the radio source, which do not appear to contribute substantially to X-ray emission, are found to be spatially associated with the extremes of the X-ray loop. A model of plasma-filled loops is suggested which accounts for the emissions in both spectral ranges and for their spatial location and temporal development.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 49; Aug. 197
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  • 95
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    The Hale solar sector boundary (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: A Hale solar-sector boundary is defined as that half (northern hemisphere or southern hemisphere) of a sector boundary in which the change of sector-magnetic-field polarity is the same as the change of polarity from a preceding spot to a following spot. Above a Hale sector boundary the green corona has maximum brightness, while above a non-Hale boundary the green corona has a minimum brightness. The Hale portion of a photospheric sector boundary tends to have maximum magnetic-field strength, while the non-Hale portion has minimum field strength.
    Keywords: SOLAR PHYSICS
    Type: AD-A086396 , Solar Physics; 49; July 197
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  • 96
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    Association of X-ray arches with chromospheric neutral lines (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Daily maps of magnetic neutral lines derived from H-alpha observations have been superimposed on solar X-ray images for the period from June 15 to 30, 1973. Nearly all X-ray-emitting structures consist of systems of arches covering chromospheric neutral lines. Areas of low emissivity, coronal holes, appear as the areas between arcades of arches. The presence of a coronal hole, therefore, is determined by the spacing between neutral lines and the scale of the arches over those neutral lines. X-ray emissivity on the solar disk extends from neutral lines in proportion to the vertical and horizontal scale of the arches over those neutral lines. Increasing scale of arches corresponds with increasing age of magnetic fields associated with the neutral line. All X-ray filament cavities coincided with neutral lines, but filaments appeared under cavities for only part of their length and for only a fraction of the disk passage.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 49; July 197
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  • 97
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    MHD solution of interplanetary disturbances generated by simulated velocity perturbations (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: An MHD time-dependent numerical simulation, restricted to the solar equatorial plane, is used to demonstrate the interplanetary disturbances caused by several simplified coronal holes. Each 'hole' is assumed to have a configuration such that the higher solar wind velocity produced within their longitudinal extent is Gaussian over a 7-day period at the inner boundary (0.3 AU) of the numerical simulation. A second, twin coronal hole is assumed to rotate on the solar disk behind its predecessor. It is shown that the first coronal hole-produced interplanetary shock ensemble is overtaken by the second ensemble because of the higher velocity, lower density environment into which the latter propagates. A number of features predicted by MHD similarity theory are confirmed by the numerical simulation. These features include (1) strong azimuthal magnetic and plasma density compression, accompanied with average temperature depression, at the contact surface between forward and reverse shock ensembles, and (2) increasing spatial separation distance between forward and reverse shocks.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 81; Nov. 1
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  • 98
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    Thermal instability in post-flare plasmas (1976)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The cooling of post-flare plasmas is discussed and the formation of loop prominences is explained as due to a thermal instability. A one-dimensional model was developed for active loop prominences. Only the motion and heat fluxes parallel to the existing magnetic fields are considered. The relevant size scales and time scales are such that single-fluid MHD equations are valid. The effects of gravity, the geometry of the field and conduction losses to the chromosphere are included. A computer code was constructed to solve the model equations. Basically, the system is treated as an initial value problem (with certain boundary conditions at the chromosphere-corona transition region), and a two-step time differencing scheme is used.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-149455 , SU-IPR-679
    Format: application/pdf
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  • 99
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    Further changes in the distribution of density and radio scattering in the solar corona in 1973 (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 209; Oct. 1
    Format: text
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  • 100
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    On the minimum variance direction of magnetic field fluctuations in the azimuthal velocity structure of the solar wind (1976)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The paper examines the properties of microscale magnetic field fluctuations for diverse classes of large-scale azimuthal velocity structures in the solar wind, with particular reference to the orientation of the wave normal vector for MHD waves in the interplanetary medium. It is shown that the direction of minimum variance does not exhibit any characteristic refraction pattern with respect to large-scale velocity structures in the solar wind. It is suggested that the direction of minimum variance is not indicative of the wave normal vector directions. The determination of the wave normal vector directions for the predominantly transverse MHD waves in the interplanetary medium is presently beyond the capability of single spacecraft observations.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 3; Sept
    Format: text
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