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  • SOLAR PHYSICS  (568)
  • 2000-2004
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  • 1980-1984  (310)
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  • 1
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    Some basic considerations of measurements involving collimated direct sunlight (1976)
    In:  CASI
    Details
    Publikationsdatum: 2006-08-09
    Beschreibung: For abstract, see N77-26622.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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
    Publikationsdatum: 2006-08-09
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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
    Publikationsdatum: 2006-08-09
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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
    Publikationsdatum: 2006-01-12
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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
    Publikationsdatum: 2006-01-12
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: The Deep Space Network; p 68-76
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  • 7
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    Report on the Workshop on Intercomparison of Solar UV Irradiance Measurements and Related Instrument Calibration (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-19
    Beschreibung: The knowledge of the absolute value of the solar ultraviolet irradiance did not improve very much during the rising phase of the solar cycle 21. The variations associated with the solar rotation period were observed by means of three satellites, namely, the Atmospheric Explorer E (AE-E), Nimbus 7 and the Solar Mesospheric Explorer (SME). Long-term variations related to the solar activity cycle are not well known. Values were deduced during the solar cycle 21 from the AE-E satellite and the rocket program performed by the Laboratory for Atmospheric and Space Physics leading to variations of about a factor of 2 around 150 nm but definitely less than 20 percent beyond 175 nm. Such low level of variation is still masked by the current uncertainties and reproducibility of the observations performed since 1976. The uncertainties of recent observations are reported with their discrepancies. The gaps between the current accuracy goals and the achievements are still very important. The challenge for the next three years is to improve both the accuracy and the precision of future observations at the level of the available irradiance standards and to measure quantitatively long-term variations of the order of a few percent. The main causes of these gaps are identified.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: International Council of Scientific Unions Middle Atmosphere Program. Handbook for MAP, Vol. 8; p 45-51
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  • 8
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    Electrodynamic coupling in magnetically confined stellar X-ray loops (1983)
    In:  Other Sources
    Details
    Publikationsdatum: 2011-08-18
    Beschreibung: The solar coronal complex X-ray structure is now known to involve radiation loops that coincide spatially with the magnetic loops confining the radiating plasma. An effort is presently made to identify primary submodels involved in the global coupling between a mechanical energy reservoir of beta value greater than 1 and a contiguous site of X-ray activity whose beta value is lower than 1. The 'dynamo' model invoked establishes a quantitative connection between mechanical driver properties and the dimensions, field strength, and number density distribution of elemental magnetic loops.
    Schlagwort(e): SOLAR PHYSICS
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  • 9
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    Interpretation of vector magnetograph data including magneto-optic effects. I - Azimuth angle of the transverse field (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: In this paper, the presence of Faraday rotation in measurements of the orientation of a sunspot's transverse magnetic field is investigated. Using observations obtained with the Marshall Space Flight Center's (MSFC) vector magnetograph, the derived vector magnetic field of a simple, symmetric sunspot is used to calculate the degree of Faraday rotation in the azimuth of the transverse field as a function of wavelength from analytical expressions for the Stokes parameters. These results are then compared with the observed rotation of the field's azimuth which is derived from observations at different wavelengths within the Fe I 5250 A spectral line. From these comparisons, it is found: the observed rotation of the azimuth is simulated to a reasonable degree by the theoretical formulations if the line-formation parameter is varied over the sunspot; these variations are substantiated by the line-intensity data; for the MSFC system, Faraday rotation can be neglected for field strengths less than 1800 G and field inclinations greater than 45 deg; to minimize the effects of Faraday rotation in sunspot umbrae, MSFC magnetograph measurements must be made in the far wings of the Zeeman-sensitive spectral line.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 88; 51-64
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  • 10
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    Dynamics of a surge observed in the C IV and H alpha lines (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Time sequences of a surge have been obtained in Active Region 2701 during a coordinated SMY program, on October 2nd, 1980, while the MSDP spectrograph operated in H-alpha at the Meudon Solar Tower and the UVSP spectrometer on SMM observed in the 1548 A C IV resonance line. The cold (H-alpha) and hot (C IV) material follow the same channel, and the event lasts about 10 min in both lines. A good correlation is found between H-alpha and C IV velocities; radial velocities along the surge are in the range 40-60 km/s in both cases. The observations are consistent with the hypothesis that a pressure gradient drives the surge. The H-alpha data seem to indicate the presence of a shock wave in the chromosphere, while the C IV quantities (velocities, accelerations) vary on a very short time scale. Their maxima occur at some locations which could be interpreted as 'pinched' zones.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astronomy and Astrophysics (ISSN 0004-6361); 127; 2, No; 337-344
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  • 11
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    Differences in the temporal variations of solar UV flux, 10.7-cm solar radio flux, sunspot number, and Ca-K plage data caused by solar rotation and active region evolution (1983)
    In:  Other Sources
    Details
    Publikationsdatum: 2011-08-18
    Beschreibung: Attention is given to two types of temporal variations in the solar UV spectral irradiance caused by solar rotation and active region evolution. It is noted that the first type of dissimilar temporal behavior occurs when concentrations of solar active regions evolve at solar longitudes nearly 180 deg apart. Both the UV observations and modeled UV fluxes based on Ca-K plage data then exhibit pronounced 13-day periodicity, whereas the 10.7-cm solar radio flux and sunspot number exhibit quite dissimilar temporal variations. This type of dissimilarity is related to the modeled UV flux and has a dependence on the solar central meridian distance that is narrower than that for the 10.7-cm radio flux or for sunspot numbers. A second case of marked dissimilarity is seen when major new solar active regions arise and dominate the full-disk fluxes for several rotations. It is found that the strongest peaks in 10.7 cm and sunspot numbers tend to occur on their first rotation, for example, during major dips in the total solar irradiance, whereas the Ca-K plages and UV enhancements peak on the next rotation and then decay more slowly on subsequent rotations.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 88; 9883-988
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  • 12
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    The stability of coronal loops - Finite-length and pressure-profile limits (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Results are described from a quickly converging, necessary-and-sufficient, MHD-stability test for coronal-loop models. The primary stabilizing influence arises from magnetic line tying at the photosphere, and this end conditions requires a series expansion of possible loop excitations. The stability boundary is shown to quickly approach a limit as the number of terms increases, providing a critical length for the loop in proportion to its transverse magnetic scale. Several models of force-free-field profiles are tested and the stability behavior of a localized current channel, embedded in an external current-free region, is shown to be superior to that of other, broader, current profiles. Pressure-gradient effects, leading to increased or decreased stability, are shown to be amplified by line tying. Long loops must either conduct low net current, or exhibit an axial-field reversal coexisting with a low-pressure core. The limits on stability depend on the magnetic aspect ratio, the plasma-to-magnetic pressure ratio, and the field orientation at the loop edge. Applications of these results to the structure of coronal loops are described.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 88; 163-177
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  • 13
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    Implications of high-energy neutron observations from solar flares (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The time-dependent flux of high-energy neutrons discovered from the solar flare of 1980 June 21 provides a new technique for determining the total number and energy spectrum of accelerated protons and nuclei at the sun. The implications of these observations on gamma-ray emission, relativistic electron spectrum and number, proton and electron energy contents, and the location of the interaction region are also examined.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X); 273; L41-L45
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  • 14
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    Fluid motions in the solar chromosphere-corona transition region. IV - Mass motions over sunspot umbrae (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 273; 374-380
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  • 15
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    Solar irradiance variations. II - Analysis of the extreme ultraviolet measurements onboard the Atmosphere Explorer E satellite (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Five of the extreme ultraviolet channels (L-alpha, L-beta, He I, He II, Fe XV) measuring irradiance fluctuations on board the AE-E satellite between 1977 and 1980 have been studied in detail. It is shown that the daily variations correspond very closely to the daily variations in solar radio emission (F10.7), but that the UV data are afflicted with serious and to date unrecognized calibration changes during the period of operation of the instruments. In order to correct for these changes, a statistical analysis is carried out, and a set of corrections to the raw data is suggested. The resulting, now uniform, data are then compared with rocket measurements (L-alpha) and data acquired onboard the AE-C satellite (L-beta). Finally the remaining discrepancies are discussed. After concluding that they are below the overall level of uncertainties, a first-order 10-year run of EUV irradiances derived from F10.7 data is proposed. This estimate includes the ratio of irradiance levels between the maxima of solar cycles 20 and 21 and the intervening minimum.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 88; 9037-905
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  • 16
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    Determining the solar wind speed above active regions using remote radio-wave observations (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: A new technique has made it possible to measure the velocity of portions of the solar wind during its flow outward from the sun. This analysis utilizes spacecraft (ISEE-3) observations of radio emission generated in regions of the solar wind associated with solar active regions. By tracking the source of these radio waves over periods of days, it is possible to measure the motion of the emission regions. Evidence of solar wind acceleration during this outward flow, consistent with theoretical models, has also been obtained.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Science (ISSN 0036-8075); 222; 506-508
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  • 17
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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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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
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  • 18
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    The solar brightness temperature at millimeter wavelengths (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics; 48; May 1976
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  • 19
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    Evidence for the regulation of solar wind heat flux at 1 AU (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Oct. 1
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  • 20
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    High-speed solar wind flow parameters at 1 AU (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Oct. 1
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  • 21
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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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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics; 46; Jan. 197
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  • 22
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    Hectometric and kilometric solar radio emission observed from satellites in August 1972 (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Space Science Reviews; 19; Oct
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  • 23
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    Diamagnetic boundary layers - A kinetic theory (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysics and Space Science; 45; Dec. 197
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  • 24
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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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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
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  • 25
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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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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: The Deep Space Network; p 121-137
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  • 26
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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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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Sept. 1
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  • 27
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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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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature; 262; Aug. 26
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  • 28
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    Coronal temperatures and temperature gradients from OSO-7 spectroheliograms (1976)
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics; 47; Apr. 197
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  • 29
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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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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astronomy and Astrophysics; 53; 2, De; Dec. 197
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  • 30
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    On the theory of the type III burst exciter (1976)
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics; 46; Feb. 197
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  • 31
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    Directivity of low frequency solar type III radio bursts (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics; 46; Feb. 197
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  • 32
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    The quiet sun chromospheric network observed from Skylab (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 209; Oct. 1
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  • 33
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    Doppler wavelength shifts of transition zone lines measured in Skylab solar spectra (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 205; May 1
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  • 34
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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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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal Supplement Series; 31; July 197
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  • 35
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    Solar irradiance - Total and spectral and its possible variations (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Applied Optics; 15; Apr. 197
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  • 36
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    Solar gamma-ray lines as probes of accelerated particle directionalities in flares (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 203; Feb. 1
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  • 37
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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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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal Supplement Series; 31; July 197
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  • 38
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    Electron parameter correlations in high-speed streams and heat flux instabilities (1976)
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; May 1
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  • 39
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    Hydromagnetic waves, turbulence, and collisionless processes in the interplanetary medium (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: An extended discussion is conducted concerning the origin and evolution of interplanetary hydromagnetic waves and turbulence, and their influence on the large scale dynamics of the solar wind. The solar wind is at present the preeminent medium for the study of hydromagnetic waves and turbulence, providing an opportunity for advancement of understanding of the most fundamental processes of the astrophysical plasmas. All interplanetary fluctuations whose time scale is observed to be greater than 1 sec can be regarded as hydromagnetic fluctuations. It has been found to be simplest, and generally very satisfactory, to model interplanetary variations as fluctuations in an MHD fluid. Attention is given to the classification of wave modes, geometrical hydromagnetics, Alfven wave pressure, rugged invariants, and the kinetic theory of collisionless processes.
    Schlagwort(e): SOLAR PHYSICS
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  • 40
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    Behavior of transition-region lines during impulsive solar flares (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: The emissions observed in lines originating in the transition-region plasma, particularly during impulsive flares, are investigated using data collected by the Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission. Data concerning lines from ions such as Si II, C IV, Si IV, O V, and Fe XXI are analyzed. Topics examined include the transition region away from sunspots, oscillatory motions above sunspots, the shape of the transition region, the transition region during flares, and O V and Fe XXI during flare flash phases.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0038-0938)
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  • 41
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    Gamma-ray lines and neutrons from solar flares (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The energy spectrum of accelerated protons and nuclei at the site of a limb flare was derived by a technique, using observations of the time dependent flux of high energy neutrons at the earth. This energy spectrum is very similar to the energy spectra of 7 disk flares for which the accelerated particle spectra was previously derived using observations of 4 to 7 MeV to 2.223 MeV fluence ratios. The implied spectra for all of these flares are too steep to produce any significant amount of radiation from pi meson decay. It is suggested that the observed 10 MeV gamma rays from the flare are bremsstrahlung of relativistic electrons. Previously announced in STAR as N83-19695
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0038-0938)
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  • 42
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    A comparison of coronal and interplanetary current sheet inclinations (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: The HAO white light K-coronameter observations show that the inclination of the heliospheric current sheet at the base of the corona can be both large (nearly vertical with respect to the solar equator) or small during Cararington rotations 1660 - 1666 and even on a single solar rotation. Voyager 1 and 2 magnetic field observations of crossing of the heliospheric current sheet at distances from the sun of 1.4 and 2.8 AU. Two cases are considered, one in which the corresponding coronameter data indicate a nearly vertical (north-south) current sheet and another in which a nearly horizontal, near equatorial current sheet is indicated. For the crossings of the vertical current sheet, a variance analysis based on hour averages of the magnetic field data gave a minimum variance direction consistent with a steep inclination. The horizontal current sheet was observed by Voyager as a region of mixed polarity and low speeds lasting several days, consistent with multiple crossings of a horizontal but irregular and fluctuating current sheet at 1.4 AU. However, variance analysis of individual current sheet crossings in this interval using 1.92 see averages did not give minimum variance directions consistent with a horizontal current sheet. Previously announced in STAR as N83-31566
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 88; Oct. 1
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  • 43
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    The solar O III spectrum. II - Longer wavelengths, line widths, and the He II Lyman alpha radiation field (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The solar O III spectrum above 900 A is analyzed, including several visible and infrared lines which are important in nebular studies. The dependence of the line intensities on the rate of photoexcitation by He Ly-alpha is determined, and the observability of these lines in the solar spectrum is studied. The impact approximation is employed to calculate the expected line widths of the stronger solar O III lines. The photoexciting field at 304 A calculated from the observed intensities of the O III lines below 900 A (Bhatia et al., 1982) is compared with the field predicted by a recent model (Avrett et al., 1976). It is shown that additional radiation trapping must be present beyond that given by this model.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal Supplement Series (ISSN 0067-0049); 53; Sept
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  • 44
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    Measurements on a shock wave generated by a solar flare (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: It is shown that path-integrated radio-scattering measurements of the solar wind velocity yield higher estimates than those of point measurements. The post-shock speed is determined from radio scattering measurements by selection of the maximum of the radio-scattering deduced from the velocity-time curve, whereas velocity points on the rising edge of the shock underestimate the post-shock gas velocity, and therefore the shock speed. However, it is suggested that large uncertainties reside in using radio techniques for measurements of parameters of the shock wave, and the uncertainties may be large enough to encompass the lower velocity values calculated by a point method of measurement.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature (ISSN 0028-0836); 304; Aug. 25
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  • 45
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    Solar radius change between 1925 and 1979 (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: From an analysis of numerous reports from different locations on the duration of totality of the solar eclipses on January 24, 1925, and February 26, 1979, it is found that the solar radius at the earlier date was 0.5 arcsec (or 375 km) larger than at the later date. The correction to the standard solar radius found for each eclipse is different when different subsets of the observations are used (for example, edge of path of totality timings compared with central timings). This is seen as suggesting the existence of systematic inaccuracies in our knowledge of the lunar figure. The differences between the corrections for both eclipses, however, are very similar for all subsets considered, indicating that changes of the solar size may be reliably inferred despite the existence of the lunar figure errors so long as there is proper consideration of the distribution of the observations. These results are regarded as strong evidence in support of the occurrence of solar radius changes on shorter than evolutionary time scales.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature (ISSN 0028-0836); 304; Aug. 11
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  • 46
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    Solar oscillations with 13-day period (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: Reference is made to the solar observations made by Claverie et al. (1982) over a three-month period in the summer of 1981 which show oscillatory velocity with a period of 13.1 days and amplitude of 6.6 m/s. These investigators reject the possibility that they see the Doppler shift from a radial oscillation, because the amplitude is implausibly large. They also do not believe that their signal was induced by solar magnetic fields, since typical mean solar fields are too small. Photo-electric drift-scan measurements of the solar diameter and full-disk magnetograms taken at Kitt Peak National Observatory are examined here for evidence of variations corresponding to the velocity oscillations of the 13.1-day period. An upper limit on radius variations is reported which is a factor of six below the amplitude needed to explain the velocity observations as a radial oscillation. Attention is also given to the possible role of the rotation of large-scale surface magnetic features.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature (ISSN 0028-0836); 304; Aug. 11
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  • 47
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    Formation of the Cl I line at 1351 A in the solar chromosphere (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: The formation of the multiplet containing the Cl I 1351 A line is investigated due to the unusual brightness of this line. It is determined that this line is formed via a fluorescence effect driven by the 1335 A line of C II. Non-LTE calculations including this effect are found to agree with the observed line intensity. It is shown that the 1347 and 1363 A lines of Cl I do not benefit from this effect and they are predicted to be approximately 100 times weaker.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 266
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  • 48
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    Observations of solar oscillations of low and intermediate degree (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: Measurements are presented of solar velocity oscillations with spherical harmonic degree 1-139 and angular order approximately 0. With an amplitude sensitivity of approximately 2 cm/s, trapped acoustic wave modes of radial orders 2-26 are observed at frequencies between 1.7 and 5.5 mHz. The radial order identifications of low-degree modes previously inferred from theory are confirmed. Only marginal evidence of long-period, gravity-mode oscillations is found.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature; 302; Mar. 3
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  • 49
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    Magnetic canopies in unipolar regions (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: Base-height statistics are presented for magnetic canopies in six unipolar magnetic regions which were observed near the limb with the Kitt Peak Vacuum Telescope and Diode Array Magnetograph during the period 25 April-3 July, 1980. As in earlier studies, extensive areas are found to be covered by low-lying canopies.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 87; Aug. 198
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  • 50
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    Corotating pressure waves without fast streams in the solar wind (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: Voyager 1 and 2 magnetic field and plasma data are presented which demonstrate the existence of large scale, corotating, non-linear pressure waves between 2 AU and 4 AU that are not accompanied by fast streams. The pressure waves are presumed to be generated by corotating streams near the sun. For two of the three pressure waves that are discussed, the absence of a stream is probably a real, physical effect, viz., a consequence of deceleration of the stream by the associated compression wave. For the third pressure wave, the apparent absence of a stream may be a geometrical effect; it is likely that the stream was at latitudes just above those of the spacecraft, while the associated shocks and compression wave extended over a broader range of latitudes so that they could be observed by the spacecraft. It is suggested that the development of large-scale non-linear pressure waves at the expense of the kinetic energy of streams produces a qualitative change in the solar wind in the outer heliosphere. Within a few AU the quasi-stationary solar wind structure is determined by corotating streams whose structure is determined by the boundary conditions near the sun. Previously announced in STAR as N83-19694
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 88; Aug. 1
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  • 51
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    Microwave and hard X-ray observations of a solar flare with a time resolution better than 100 ms (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Simultaneous microwave and X-ray observations are presented for a solar flare detected on 1980 May 8 starting at 1937 UT. The X-ray observations were made with the Hard X-ray Burst Spectrometer on the Solar Maximum Mission and covered the energy range from 28-490 keV with a time resolution of 10 ms. The microwave observations were made with the 5 and 45 foot antennas at the Itapetinga Radio Obervatory at frequencies of 7 and 22 GHz, with time resolutions of 100 ms and 1 ms respectively. Detailed correlation analysis of the different time profiles of the event show that the major impulsive in the X-ray flux preceded the corresponding microwave peaks at 22 GHz by about 240 ms. For this particular burst the 22 GHz peaks preceded the 7 GHz by about 1.5s. Observed delays of the microwave peaks are too large for a simple electron beam model but they can be reconciled with the speeds of shock waves in a thermal model. Previously announced in STAR as N82-30215
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 84; April 19
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  • 52
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    The isotopic composition of solar flare noble gases (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: The relative elemental and isotopic abundances of noble gases provide insights into a number of topics related to the solar system. Neon is in many ways the most diagnostic of the noble gases. The diagnostic character is mainly related to the variation in the relative abundance of the two most abundant neon isotopes, Ne-20 and Ne-22. The available evidence suggests that trapped neon found in meteorites and in lunar samples consists of as many as five isotopically distinct components, including neon A, B, C, D, and E. Neon B has been shown to be due to solar wind neon which has been directly implanted into the material found in a meteorite. It appears that neon E is extrasolar in origin. There exist ambiguities regarding the origins of the remaining three components. The present investigation is concerned with a reexamination of the existing data in an effort to eliminate or at least clarify these ambiguities. It is found that neon C is apparently due to directly implanted, low-energy solar flare neon nuclei.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 266
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  • 53
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    Solar wind speed variations - 1962-1974 (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-17
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Oct. 1
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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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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysics and Space Science; 43; Aug. 197
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    Doppler noise considered as a function of the signal path integration of electron density (1976)
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: The Deep Space Network; p 159-193
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    The solar spectrum - Wavelengths and identifications from 160 to 770 angstroms (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 203; Jan. 15
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    On the nonexistence of plane-polarized large amplitude Alfven waves (1976)
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Jan. 1
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    Microscale 'Alfven waves' in the solar wind at 1 AU (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Jan. 1
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    A shock surface geometry - The February 15-16, 1967, event (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; Jan. 1
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    Formation of iron sulphide in solar nebula (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature; 259; Jan. 22
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    Kitt Peak 60-cm vacuum telescope (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Applied Optics; 15; Jan. 197
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    Solar cycle evolution of high-speed solar wind streams (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 207; Aug. 1
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    Electromagnetic instabilities driven by unequal proton beams in the solar wind (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 81; June 1
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    Low frequency radio observations of the solar wind near the moon (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Geophysical Research Letters; 3; June 197
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    Timing of solar cycles by rigid internal rotations (1976)
    In:  Other Sources
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    Publikationsdatum: 2011-08-16
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; 205; Apr. 15
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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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    Publikationsdatum: 2011-08-16
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysics and Space Science; 40; Mar. 197
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    The rotational spectrum of g-modes in the sun (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Observations and calculations are presented which strongly suggest that the unique sequence of rotation rates due to g-modes is active in the sun. It is found that all angular harmonics from 1 = 2-11 appear to be resolved, while higher harmonics up to at least 1 = 20 also seem to be active. The extreme narrowness of many of the spectral lines indicates that the g-modes are locked in sets of constant 1 by a local mechanism which excites the modes and possibly regulates the long-term precision of their rotation. These sets act as a system of resonant, or nearly resonant, clocks which impose a degree of periodicity upon solar activity and measure the mean solar interior rotation
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 264
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    Observation of chromospheric evaporation during the Solar Maximum Mission (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: A study is presented of the upward motions of part of the soft X-ray emitting plasma using data for flares collected in 1980 by the Bent Crystal Spectrometer and the Hard X-ray Burst Spectrometer on the Solar Maximum Mission satellite. Results show that upward motions of the soft X-ray plasma are temporally associated with the build up of the thermal phase of flares and with the period of energy deposition as indicated by the hard X-ray emission. In addition, it is found that the hardness of the hard X-ray spectrum, the evaporation velocity, and the rate of increase of the gradual phase are correlated. It is also possible that the total electron energy deposited in the chromosphere, the peak emission measure of the evaporating plasma, and the peak emission measure of the thermal coronal plasma may also be correlated.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0038-0938)
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    Conductive flux in the chromosphere derived from line linear polarization observation (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: It is shown that quantitative information on the mechanisms of energy transport which take place in solar flares can be obtained by measurement of impact line polarization. Linear polarization in two chromospheric lines (H-alpha and SI 1437 A) observed in the gradual phase of solar flares was investigated. The polarized electric vector is shown to be directed towards the center of the disk. The relationship between conductive heat flux and linear line polarization is determined using a function which represents the velocity distribution of electrons carrying heat flux. The relationship between linear polarization and heat flux is applied to the observed degree of polarization, which yields the conductive heat flux in the high chromosphere. It is determined that this conductive flux is of the order of magnitude of the total radiation loss in the chromosphere and below, which is also of the order of magnitude of the conductive flux in the transition zone.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0038-0938)
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    Radio blips and hard X-rays in solar flares (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The properties of short, narrow-band spikes occurring in groups at decimetric wavelengths have been extensively analyzed. The bursts, termed blips in the literature, have been found to appear in the impulsive phase of flares. They are associated with hard X-ray emission in 40 percent of all cases with simultaneous coverage. The correspondence between blips and X-ray spikes is generally not one-to-one, blips being more numerous than X-ray spikes. In some cases, however, close correlations between single events have been found. Blips have been discovered to drift in frequency and to decay in time similarly to type III bursts at lower frequency. They also resemble type III bursts in polarization. An analysis of starting frequencies, however, clearly shows that blips and type III bursts belong to different statistical populations. The narrow bandwidth of blips, the major qualitative difference with respect to type III bursts, suggests that blips are the signature of electron beams which either decay rapidly or have a locally enhanced emission due to the presence of some low-frequency wave. Blips have been shown to be an impulsive phase phenomenon occurring at densities of one to three billion per cu cm in the low corona.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 271; Aug. 1
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    Physical conditions in a quiescent prominence derived from UV spectra obtained with the UVSP instrument on the SMM (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: A quiescent prominence observed above the north-west limb on November 20, 1980, is analyzed using data obtained with the UV spectrometer and polarimeter (UVSP) on the Solar Maximum Mission (SMM). The spectral data include the lines 1215 A of H1, 1401 A of OIV, 1402 A of SIIV, 1548 A of CIV, 1640 A of HeI, and 1655 A of CI. From an analysis of these lines and their emission patterns, the physical characteristics of the prominence plasma are deduced, and it is suggested that the prominence consisted of flux tubes at various temperatures. In the hotter parts of the plasma the number density reached values of about 3 x 10 to the 11th/cu cm.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 84; April 19
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    Vertical gradients of sunspot magnetic fields (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The results of a Solar Maximum Mission (SMM) guest investigation to determine the vertical gradients of sunspot magnetic fields for the first time from coordinated observations of photospheric and transition-region fields are described. Descriptions are given of both the photospheric vector field of a sunspot, derived from observations using the NASA Marshall Space Flight Center vector magnetograph, and of the line-of-sight component in the transition region, obtained from the SMM Ultraviolet Spectrometer and Polarimeter instrument. On the basis of these data, vertical gradients of the line-of-sight magnetic field component are calculated using three methods. It is found that the vertical gradient of Bz is lower than values from previous studies and that the transition-region field occurs at a height of approximately 4000-6000 km above the photosphere.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 84; April 19
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    Dynamics and spectroscopy of asymmetrically heated coronal loops (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Numerical models of steady flows along coronal magnetic flux tubes of varying cross sectional areas are investigated. The flows are induced by altering the spatial symmetry of the heating. In two cases the flux tube geometry is symmetric about the top of the loop, but the spatial dependence of the heating rate is changed from a symmetric deposition which supports a stationary equilibrium to a time-independent asymmetric deposition. In a third case the volumetric heating rate is uniform, but one half of the loop is larger in volume than the other. The resulting velocity structure varies significantly with changes in the flux tube geometry. Calculations of the ionization balance and line emission for a number of ionization stages of oxygen suggest that heating induced flows may be responsible for the redshifts seen in spectral lines formed in the network at transition region temperatures.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 267
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    Microwave signatures from a reconnecting plasma pinch, with application to loop flares (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: A calculation is made of microwave signature of a cylindrical plasma pinch undergoing magnetic reconnection, a process which occurs in many astrophysical situations, such as solar flares. Depending on the viewing angle and the average energy of the accelerated electrons, the microwaves from this betatron-like source show various amounts of circular polarization. The degree of polarization is shown to be frequency dependent, and the sense of polarization is sometimes reversed. The power spectrum is predicted to have several interesting properties, which can be compared with high-resolution measurements.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 275; 901-915
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    Effects of core perturbations on the structure of the sun (1983)
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    Publikationsdatum: 2011-08-18
    Beschreibung: The effects of perturbing the inner part of the solar core where the hydrogen abundance has been partially depleted by nuclear burning are investigated. Small regions are mixed within the core and the evolution of the resulting luminosity and radius perturbations is followed. The sensitivity of the solar luminosity and radius to mixing events of different sizes and at different locations in the core is determined and several relationships between the luminosity and radius perturbations are examined to see if the value of one of these perturbations can be inferred from a measurement of the other. It is found that any core perturbation which alters the hydrostatic structures will immediately affect the solar luminosity and radius. The behavior of these perturbations depends on the location of the mixing event within the core. Mixing events cannot produce the decrease in the solar radius without leading to a homogeneous evolution of the solar core and/or to a prohibitively large change in the solar luminosity.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 273; 795-804
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    Si III line ratios in the sun (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: New atomic data for Si III have been used to predict level populations and emission-line intensity ratios for electron densities and temperatures appropriate to the solar transition region. The electron impact collision rates used here are substantially larger than those previously published owing to delineation of the complex resonance structures in the low-energy collision strengths. This together with small changes in the spontaneous radiative rates produces significant changes in the calculated intensity ratios. Generally good agreement is found with observations obtained using the Naval Research Laboratory slit spectrograph aboard Skylab, electron densities from three Si III ratios and from other methods normally agreeing to 0.2 dex or better for a wide variety of solar features. For a fourth ratio, incorporating lines with a wide wavelength separation, the agreement is less satisfactory, possibly owing to uncertainties in the observational data.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 274; 420-428
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    Lines of Fe XII sensitive to coronal electron density (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Lines of Fe XII sensitive to coronal electron density are discussed. The lines appear in solar spectra obtained by the Naval Research Laboratory (NRL) slit spectograph flown on Skylab. These lines are due to transitions between levels of the 3s 2 3p 3 configuration and fall at the wavelengths 1242.03 A, 1349.38 A, 2169.03 A, 2405.71 A, and 2565.99 A. It is shown that the line at 2169.03 A is severely blended by a line of Ni II at heights less than 12 arcsec outside the solar limb. Above 12 arcsec the lines at 2169.03 and 2405.71 A are apparently unblended and can be used to derive electron densities. An average coronal electron pressure of 6 x 10 to the 14th/cu cm K is obtained. However, the emitting path lengths of the Fe XII lines, deduced using the electron densities and absolute intensities, are unrealistically large. The reason for this difficulty is unclear.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 273; 822-828
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    Determination of solar wind elemental abundances from M/Q observations during three periods in 1980 (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Mass spectra in the M/Q range from 2 to 3, provided by a high-resolution mode of the ISEE-3 Plasma Composition Experiment, were evaluated for three selected periods during early 1980. The observed Ne/O ratios are compatible with estimated solar abundance ratios. In two of the three periods, the He/Ne-ratios agree with the Apollo foil results. Freezing-in temperatures for oxygen are similar to those obtained by other groups. Possible reasons for an unexpectedly high flux at M/Q = 2.4 are discussed.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 88; 359-376
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    Solar flare X-ray spectra from the P78-1 spacecraft (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Results from the high resolution solar X-ray spectrometer experiments on the P78-1 spacecraft are discussed. These results concern physical quantities such as electron temperature and density, turbulence, mass motions, and state of ionization equilibrium, characteristic of the thermal soft X-ray emitting flare plasma, and the time behavior of these quantities during flares. In addition, a brief description of the instruments is given, the plasma diagnostics used in interpreting the spectra are summarized, and the origin of the thermal soft X-ray emitting plasma is discussed in light of the P78-1 results, earlier data, and numerical simulations of magnetic flux tubes heated to solar flare temperatures.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0038-0938)
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    Purely coronal flare-like variations (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Quasiperiodic X-ray, UV, microwave, and metric-wave variations after a solar flare on November 6, 1980 are reported and analyzed, based on observational data from SMM (HXRBS, UVSP, HXIS), GOES-2, the 100-m radiotelescope at Bonn, and the Nancay radioheliograph. The maxima of the 13 brightenings observed are listed and characterized; a comparison is made with a 'normal' flare at 17:26 UT on the same day. The HXIS and UVSP data are discussed in terms of the physical properties, X-ray flux, O V flux, and H-alpha flux. The variations are found to be mainly thermal and purely coronal, with no chromospheric (H-alpha) participation (in contrast to the 17:26 flare). Since strong X-ray emissions were observed which should have involved the chromosphere through magnetic-field-line heat conduction, it is proposed that the variations wre produced ina coronal plasmoid magnetically separate from the chromosphere. A mechanism for the evolution of such a plasmoid from the upper loops of a giant X-ray arch is discussed. An iterative HXIS-image-deconvolution process is presented in an appendix.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 85; June 198
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  • 81
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    Expected intensities of solar forbidden lines emitted from 2p(k) (k = 2, 3, 4) configurations (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Predicted intensities of all significant transitions within the ground configurations of six-, seven-, and eight-electron ions are tabulated for solar conditions, on a common scale. Some applications of the table entries to line identification and emission measure analysis are presented, including proposed Mg VI classifications for the coronal lines 3488.5 A and 3502.5 A.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 85; May 1983
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  • 82
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    Heliospheric magnetic fields and plasmas (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: A survey of the existing literature on heliospheric physics, covering the period 1972-1982, is presented. Attention is given to observations and theories germane to the examination of the heliosphere as a large-scale astrophysical system that is part of the earth's environment. The literature includes data and models for magnetic sectors and the large-scale magnetic field, the large-scale plasma structure, and models and observed variations in the solar wind. Consideration is also devoted to the transient and corotating streams and shocks, the composition of the solar wind, and to MHD turbulence, waves, and discontinuities. More intensive investigations of the region near 1 AU are recommended, particularly to characterize the coronal source of the solar wind. The solar polar mission will be the first to provide radial measurements for comparisons with previous exclusively ecliptic measurements of solar activities.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: (ISSN 0034-6853)
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  • 83
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    Evidence for inhomogeneous thermal sources of two similar solar spike events of 1978 May 5 and December 4 (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Two short duration single spike solar events of 1978 May 5 and December 4 exhibit similar time profiles in the microwave and hard X-ray ranges, indicating emission from compact sources. Microwave spectral observations exhibit inhomogeneities present in the source parameters. The existence of fine time structures in the microwave time profiles at 10.4 GHz from Berne are interpreted as a signature of the dynamics of a disturbance traveling through the source at the ion-sound speed. Stereoscopic observations with the hard X-ray detector on the solar orbiter, Helios-2, and the Berne microwave antenna do not indicate any time lag or differences in the time profiles during the impulsive phase. This is taken as evidence for the absence of directionality of emission making beam models unlikely for short duration single spike events. Previously announced in STAR as N83-13047
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 270; July 1
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  • 84
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    Fluid motions in the solar chromosphere-corona transition region. III - Active region flows from wide slit Dopplergrams (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Large-scale velocity patterns observed in C IV in active regions show close correspondence with photospheric magnetic field patterns. In a large majority of cases, magnetic neutral lines show blueshift on their sun center side and redshift on their limbward side. The large-scale flow is consistent with widespread loop structure having downflow in both legs of the loops. Studies of individual bright loops, confirm that the flow is downward in most cases. However, an important subset of loops show flow from one end of the loop to the other.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 269; June 15
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  • 85
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    Atomic calculations for the Fe XX X-ray lines (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The atomic data presented here and in Bhatia and Mason (1980) allow the calculation of theoretical intensity ratios for all the EUV, UV, and X-ray lines from Fe XX. Tabulations are presently given for the transitions between levels in the 2s2 2p3, 2s2 2p2 3s, and 2s2 2p2 3d configurations of Fe(19+), and electron collision strengths are calculated by means of the 'distorted wave' approximation. In addition to the theoretical X-ray line intensity ratios, new spectral line identifications from a solar flare are presented.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astronomy and Astrophysics Supplement Series (ISSN 0365-0138); 52; April 19
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  • 86
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    Atomic calculations for Ca XVII - UV and X-ray lines (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Doschek et al. (1977) have pointed out the importance of the Ca XVII UV lines as an electron density diagnostic. Energy levels, transition probabilities, and collision strengths, are presently obtained for the 2s2, 2s 2p, 2p2, 2s 3s, 2s 3p, and 2s 3d configurations of Ca XVII, and the theoretical intensity ratios for the UV and X-ray lines are compared with observed intensities in solar flare spectra. Inconsistencies are indicated in the analysis of UV data, and discrepancies between observed and theoretical intensity ratios indicate that further studies are required. New identifications are suggested in the X-ray wavelength region.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astronomy and Astrophysics Supplement Series (ISSN 0365-0138); 52; April 19
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  • 87
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    Conductive flux in flaring solar chromospheres deduced from the linear polarization observations (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astronomy and Astrophysics; 119; 2, Ma; Mar. 198
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  • 88
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    Models of the formation of the solar nebula (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: Protostellar cloud collapse and solar nebula formation models indicate that the size of the nebula produced will be larger in terms of both gas centrifugal balance R(CF) and collapse time diffusion length R(V). From this, it can be deduced that low mass nebulas are produced if (R(V)/R(CF))-squared is much greater than unity, while nebulas result for values lower than approximately unity. The total angular momentum value distinguishes most current models of the solar nebula. Analytic expressions for the surface density, nebular mass flux and photospheric temperature distributions during the formation stage are presented for simple modes illustrating and general properties of growing protostellar disks.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Icarus; 53; Jan. 198
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  • 89
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    Multiple transonic solutions with a new class of shock transitions in steady isothermal solar and stellar winds (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: It is shown that a new class of shock transitions arises in the transonic solutions of the steady isothermal solar wind equations when momentum deposition and/or nonradial flow tube divergence give rise to multiple critical points in the flow. These shock transitions between critical solutions occur for a certain range of the parameters which characterize the momentum deposition function. The isothermal wind equations allow multiple transonic solutions in the presence of such shock transitions, yielding a continuous solution passing through an inner critical point and solutions involving a shock transition between critical solutions. It is determined that these multiple transonic solutions have the same flow speed at the base but different supersonic flow speeds at infinity. It is found that the nonradial flow tube divergence and momentum addition are equivalent, which gives rise to multiple critical points and hence to multiple transonic solutions with shock transitions. In addition, the physical relevance of these properties are examined for astrophysical systems such as the inner solar wind, flows in extragalactic jets, and accretion discs.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Journal of Geophysical Research; 88; Mar. 1
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  • 90
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    Facular influences on the apparent solar shape (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The problem of the influence of faculae on apparent solar shape is examined in light of general facular contrast models. The diagonal components of the oblateness signal from the faculae observed are calculated, and it is found that the faculae can contribute a signal whose time dependence is similar to that of the Dicke and Goldenberg (1967) oblateness signal, allowing an acceptable fit to the oblateness measurements for a facular contrast within the range of acceptable values.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Nature; 301; Jan. 13
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  • 91
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    Numerical simulations of loops heated to solar flare temperatures. I - Gasdynamics. II - X-ray and UV spectroscopy (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The NRL's Dynamic Flux Tube Model is used to numerically simulate the dynamic response of a coronal magnetic loop to an energy input of the order encountered in solar flares. The coronal plasma is heated by the deposition of flare energy at the top of the loop to more than 10 million K, yielding a conduction front that moves toward the chromosphere, where the plasma is heated by the large downward conductive flux and ablates upward to the coronal part of the loop at velocities of a few hundred km/sec. The conduction front simultaneously produces chromospheric ablation and compresses the material ahead of it. With the aid of compressional instabilities, the compressed plasma grows throughout the flare heating phase, presenting a possible source of the flare optical continuum emission which is correlated with soft X-ray radiation. The observational consequences of rapidly heated loop gas dynamic processes are discussed. In the second part of this presentation, the dynamical calculation results previously obtained are used to predict the spectral line intensities, profiles and wavelengths of several X-ray lines and the UV line of Fe XXI at 1354.1 A. Three different viewing orientations of the loop are considered.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 265
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  • 92
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    Impact linear polarization observed in a UV chromospheric line during a solar flare (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 265
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  • 93
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    Simultaneous ultraviolet line and hard X-ray bursts in the impulsive phase of solar flares (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Astrophysical Journal; vol. 265
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  • 94
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    Fluid motions in the solar chromosphere-corona transition region. I - Line widths and Doppler shifts for C IV (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Schlagwort(e): SOLAR PHYSICS
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  • 95
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    Progress and problems in the theory of type III solar radio emission (1983)
    In:  Other Sources
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    Publikationsdatum: 2011-08-18
    Beschreibung: The experimental and theoretical status of type III solar radio emission is considered in detail. Very recent developments which are relevant to the underlying plasma physics are emphasized. In particular, the identity of the submegahertz emissions as fundamental, or second harmonic, the degree of correlation between emissivities, electron streams, and plasma (Langmuir) waves, paradoxes concerned with the time-ordering of these phenomena, and the role of background density irregularities and ion-acoustic turbulence in the solar wind, are discussed. From the theoretical point of view, the current picture of the underlying Langmuir turbulence, including such effects as the interaction between Langmuir waves and stream electrons, induced scatter off ions, and strong turbulence effects such as modulational instability and soliton collapse, is discussed.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Solar Physics (ISSN 0038-0938); 89; 403-442
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  • 96
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    The large-scale magnetic field in the solar wind (1976)
    In:  CASI
    Details
    Publikationsdatum: 2016-05-14
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 143-165
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  • 97
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    Numerical study of some solar-wind interaction models with space objects (1976)
    In:  CASI
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    Publikationsdatum: 2016-06-07
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: NASA. Goddard Space Flight Center Solar-Wind Interaction with the Planets Mercury, Venus, and Mars; p 121-133
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  • 98
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    On the nature of the solar-wind-Mars interaction (1976)
    In:  CASI
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    Publikationsdatum: 2016-06-07
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: NASA. Goddard Space Flight Center Solar-Wind Interaction with the Planets Mercury, Venus, and Mars; p 21-40
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  • 99
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    Coronal propagation: Variations with solar longitude and latitude (1976)
    In:  CASI
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    Publikationsdatum: 2016-06-07
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: 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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  • 100
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    Latitudinal properties of the solar wind from studies of ionic comet tails (1976)
    In:  CASI
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    Publikationsdatum: 2016-06-07
    Beschreibung: 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.
    Schlagwort(e): SOLAR PHYSICS
    Materialart: Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 95-107
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