the nature and effects of space environments on man. For N79-34119*# National Aeronautics and Space Administration, INTRODUCTION TO SKYLAB c18 Avail: NTIS MF A01; SOD HC CSCL 22B The general characteristics of the Skylab space station are In its Skylab's Astron. and Space Sci. 1979 p 7-26 (For Avail: NTIS MF A01; SOD HC CSCL 03A The importance of the ultraviolet region to astrophysics is In its Skylab's Astron. and Space Sci. 1979 p 27-42 (For Avail: NTIS MF A01; SOD HC CSCL 03B The micrometeoroid collection experiment (S149) mounted In its Skylab's Astron. and Space Sci. 1979 p 43-64 (For Comet Kohoutek (1973 XII) was discovered by Lubos G.Y In its Skylab's Astron. and Space Sci. 1979 p 65-78 (For primary document see N79-34118 24-88) Avail: NTIS MF A01; SOD HC CSCL 03B The particles within the magnetosphere have various origins and some have complex histories. Among those observed by instruments on Skylab were galactic cosmic rays, trapped particles probably originating in the solar wind, and neutrons formed by the reaction of high-energy particles with the atmosphere. In addition, there were secondary particles produced by high-energy particles striking the structure of Skylab itself. Skylab's orbit was entirely within the magnetosphere. G.Y. In its Skylab's Astron. and Space Sci. 1979 p 79-92 (For primary document see N79-34118 24-88) Avail: NTIS MF A01; SOD HC CSCL 04A The earth's atmosphere was studied from the ground and from various vehicles. Skylab's position above the atmosphere and the long duration of the mission enabled the crews to gather information about the atmosphere that could hardly be obtained in any other way. Photographic observations of the sunrise, the moonrise, the horizon, the ionosphere, the earth's limb in ultraviolet and the aurora are presented. Data obtained from spectral line absorption analysis is also presented. G.Y. N79-34127 California Inst. of Tech., Pasadena. The detection by HEAO-1 of pulsed soft X-rays (0.1 0.5 keV) with a period of 9 s and a pulsed fraction that varies between 0 and 100% from SS Cygni at the peak of an optical outburst confirms for the first time the supposed high-energy origin of the optical pulsations seen from dwarf novae. The pulse shape is remarkably sinusoidal for such a large amplitude oscillation. A soft X-ray pulsation detected from U Geminorum on the declining portion of an optical outburst is quasi-periodic with periods ranging from 20 to 30 s, and present throughout all binary phases with an average amplitude of approximately 15%. A preliminary survey of the soft X-ray emission from approximately 65 dwarf novae during quiescence was also made. Thus far, soft X-rays were detected only at positions coincident with those of AY Lyrae and EX Hydrae. The quiescent state spectra of dwarf novae are compared with their outburst spectra. It is concluded that variations in the mass accretion rate may account for the variety of X-ray behavior observed. Dissert. Abstr. N79-34128 Texas Univ. at Austin. Continuous spectrum scans were applied to the problem of galaxy population analysis. Synthetic spectra were matched objectively to observed spectra by a modified least squares technique with linear side constraints. The spectrum scans which are sampled uniformly every 10 A, without recourse to a fictitious continuum against which to measure equivalent widths. Observations of the nuclear regions of M31 and M32 indicate that the light is dominated by late-type, evolved stars with strong lines. Since the scans yield accurate line strength measures, the main sequence turnoff and the average metallicity can be determined with some precision. The model building technique is the sensitivity of the solutions to small perturbations is discussed. Extension of the observations to the 1 micron region should allow the determination of the slope of the mass function which is essential for galaxy evolution studies. Dissert. Abstr. The X-ray spectral observations of two low luminosity clusters of galaxies, Centaurus and A1060, are presented. An emission feature of the Centaurus cluster at 7.9 keV is detected at about one third of the strength of the 6.7 keV line. This higher energy line represents K sub beta emission from highly ionized iron. An isothermal model with an Fe emission line is discussed and it is shown that the model cannot fit the data of the Centaurus or the A1060 clusters. The implications of the two component nature of the continuum on the Fe abundance and the X-ray surface brightness distribution are discussed. A.W.H. The solid state spectrometer on the HEAO-2 X-ray observatory observed the X-ray spectrum of Tycho's SNR. The observations show a relative excess of line emission from Si, S, and Ar by > or = 6 compared to that expected from a plasma of solar composition in collisional equilibrium and by a factor of > or 3 compared to Cas A. Similar excesses are not found for line emission from Mg and Fe. The data suggest that the SN observed by Tycho in 1572 produced significant amounts of Si group elements but did not eject large amounts of Fe as predicted by some models of Type I SN events. Author = Eighteen interplanetary sector boundary crossings observed at 1 AU by the magnetometer on the IMP-6 spacecraft are discussed. The events were examined on many different time scales ranging from days on either side of the boundary to high resolution measurements of 12.5 vectors per second. Two categories of boundaries were found, one group being relatively thin and the other being thick. In many cases the field vector rotated in a plane from one polarity to the other. Only two of the transitions were null sheets. Using the minimum variance analysis to determine the normals to the plane of rotation, and assuming that this is the same as the normal to the sector boundary surface, it was found that the normals were close to the ecliptic plane. An analysis of tangential discontinuities contained in 4-day periods about the events showed that their orientations were generally not related to the orientations of the sector boundary surface, but rather their characteristics were about the same as those for discontinuities outside the sector boundaries. Author N79-34134*# National Aeronautics and Space Administration. Steven H. Pravdo (Maryland Univ.) and Barham W. Smith 03C The A-2 spectroscopy experiment on HEAO 1 detected X-ray emission up to 25 keV from the supernova remnants Cas A and Tycho. The spectra must include continuum components with effective temperature equivalent or > 10 to the 8th power K which could arise from optically thin plasmas in the collisionless shock fronts. This is the first indication of electron-ion temperature equilibrium in the expanding shell of young remnants. Measurements of the equivalent widths of the K alpha and K beta iron line blends in Cas A, show that their ratio is not compatible with the measured X-ray temperature in the collisional ionization N79-34135*# National Aeronautics and Space Administration, Washington, D. C. GENERAL PROPERTIES OF HII REGIONS IN GALAXIES M. A. Smirnov and B. V. Komberg Oct. 1979 33 p refs Transl. into ENGLISH of Obshchiye Svoystva zon HII v Galaktikakh (Moscow), report PR-315, 1977 p 1-38 Transl. by Kanner (Leo) Associates, Redwood City, Calif. Original document prepared by Academy of Sciences (USSR), Moscow (Contract NASW-3199) (NASA-TM-75700) Avail: NTIS HC A03/MF A01 CSCL 03B The structure, electron density, and dimensions of HIl regions in galaxies are discussed. These parameters are correlated to the chemical composition gradient along the galactic radius, the dimensions of the three largest HII regions in the galaxy, and the amount of hydrogen in the galaxy, as well as the mass, dimensions, and total optical luminosity of the galaxy. The relationships of HIl regions to star formation and galactic nucleus activity are discussed and the kinematic properties of the SB and Sab galaxies are related to the size of HIl regions. THE PRODUCTION AND SPATIAL DISTRIBUTION OF Michael Raymond Combi 1979 167 p The brightness profiles of ions and neutrals were constructed from spectrograms of Comets Bennett and West. A re-evaluation of photochemical models of the cometary coma was done. Monte Carlo simulations of realistic photochemical models showed that Haser's model can adequately describe the spatial distribution of neutral species, but that the 'measured' scale lengths are only lower limits to the actual scale lengths found from the velocity of a species and its lifetime against photodissociation by the solar ultraviolet. The apparently short parent scale lengths found to date are in fact consistent with theoretical photodissociation lifetimes. Dissert. Abstr. N79-34137*# National Aeronautics and Space Administration Goddard Space Flight Center, Greenbelt, Md. A CATALOG OF JOVIAN DECAMETER-WAVE RADIO OBSERVATIONS FROM 1957 - 1978 J. R. Thieman Aug. 1979 37 prefs (NASA-TM-80308) Avail: NTIS HC A03/MF A01 CSCL 03B Data from over 200.000 hours of observation of Jupiter radio emission in the decameter-wavelength band, were collected from 13 observing sites and are available on magnetic tape Observations were made at 14 fixed frequencies from 5 to 30 MHz. The characteristics of the tape recording technique and the data format are described. The combination of overlapping data from observing sites scattered world-wide lessens the effect of the earth's daily interruption of the ground-received signal. A power spectral analysis of the data shows no evidence of The Voyager 2 magnetic field experiment is described and compared to the Voyager 1 experiment and data. The magnetosphere, the bow shock, the magnetopause, and the extended magnetic tail of Jupiter are discussed. Two crossings of the near equatorial current sheet were observed in the magnetosphere and its tail every 10 hour rotation period of the planet. A definitive mapping of the geometry and character of these enhanced plasma and depressed magnetic field regions is discussed. The interaction of the satellite Ganymede with the Jovian magnetosphere, which leads to disturbances as the Jovian magnetosphere corotates with the planet past the satellite is analyzed. A.W.H. N79-34122*# National Aeronautics and Space Administration, Washington, D. C. OBSERVATIONS OF COMET KOHOUTEK In its Skylab's Astron. and Space Sci. 1979 p 43-64 (For primary document see N79-34118 24-88) Avail: NTIS MF A01; SOD HC CSCL 03B 92 SOLAR PHYSICS Includes solar activity, solar flares, solar radiation and sunspots. N79-34139 Indiana Univ., Bloomington. THE LARGE-SCALE INTERACTION OF THE SOLAR WIND Comet Kohoutek 1973f was monitored extensively in late-1973 and early-1974, and exhibited a broad range of plasma tail behavior. On 1974 January 20, the tail was in a highly disturbed condition. The IMP 8 satellite in earth orbit was taking measurements of the solar wind and interplanetary magnetic field. Comparison of the observed tail geometry on January 20 with the theoretical position angles generated from the wind sock theory of plasma tails and the corotated satellite observations shows that the tail disturbance was probably caused by large gradients of the polar component of the solar-wind velocity. The study provides perhaps the first conclusive case of an association between a comet tail and a solar-wind event, and it suggests that the wind sock model gives a valid description of the large scale orientation of plasma tails. Dissert. Abstr. The microstructure of solar wind stream interaction regions is considered theoretically with emphasis on the role of several electrostatic kinetic instabilities which may be important within the stream interface and the compression region. Inside of 1 AU, the interface is likely to be stable against the electrostatic streaming instabilities considered. Between 1 and 2 AU, the interface will excite the magnetized ion-ion instability. The compression region is also found to be unstable beyond 1 AU where the modified two-stream instability, beam-cyclotron instability, and ion-acoustic instability are important in determining the structure of the compressive pulses as they evolve into forward and reverse shocks. It is concluded that the modified two-stream instability and beam-cyclotron instability predominately play a role in heating the electrons to the threshold for the ion-acoustic instability. Various electrostatic plasma waves, ranging in frequency from the lower-hybrid to harmonics of the electron cyclotron frequency, would be produced by these instabilities. Their signature should also be seen by high time resolution measurements of the temperature of the various plasma species. A.R.H. The primary scientific objective of the spectrometer is to provide a greater understanding of the role of energetic electrons in solar flares. This will be achieved by observations of high energy X-rays in the energy range from 20 to 200 keV with time resolution of 0.128s on a continuous basis and as short as 1 ms for limited intervals. The X-ray detector is an actively shielded CsI(Na) crystal with a thickness of 0.635 cm and a sensitive area of 71 sq cm. In the first year after launch, it is expected that approximately 1000 flares above the sensitivity threshold of 0.2 photons/(sq cm s) lasting for one second, will be detected. A.R.H. N79-34144*# Colorado Univ., Boulder. Optical, radio and X-ray evidence of violent mass motions in the corona has existed for some years but only recently have the form, nature, frequency and implication of the transients become obvious. The observed properties of coronal transients concentrating on the white-light and radio manifestations. The possible mechanisims involved in the radio bursts are discussed. The estimates of various forms of energy are reviewed. It appears that the magnetic energy transported from the Sun by the transient exceeds that of any other form, and that magnetic forces dominate in the dynamics of the motions. The conversion of magnetic energy into mechanical energy, by expansion of the fields, provides a possible driving force for the coronal and interplanetary shock waves. G.Y. N79-34145# National Geophysical and Solar-Terrestrial Data Center, Boulder, Colo. SOLAR-GEOPHYSICAL DATA NUMBER 416, APRIL 1979. PART 1: PROMPT REPORTS, DATA FOR MARCH 1979, FEBRUARY 1979 Apr. 1979 169 p 2 Vol. (PB-297218/0; SGD-416-Pt-1; NOAA-79051502-Pt-1) Avail: NTIS HC A08/MF A01 CSCL 03B Data is provided for March 1979 on: alert periods, daily solar indices, solar flares, solar radio emission, spacecraft observations, coronal holes, solar wind measurements, inferred interplanetary magnetic field polarities, mean solar magnetic field and Boulder geomagnetic substorm log. It also provides data for February 1979 on: daily solar activity center, sudden ionospheric disturbances, solar X-ray radiation, solar radio emission, cosmic rays, geomagnetic indices, and radio propagation indices. GRA N79-34147# National Geophysical and Solar-Terrestrial Data Center, Boulder, Colo. SOLAR-GEOPHYSICAL DATA NUMBER 417, MAY 1979. PART 1, (PROMPT REPORTS): DATA FOR APRIL 1979-MARCH 1979 Helen E. Coffey May 1979 166 p (PB-297447/5; SGD-417-Pt-1; NOAA-79061402) Avail: NTIS HC A08/MF A01 CSCL 03B Data is provided for April 1979 on: alert periods, daily solar indices, solar flares, solar radio emission, spacecraft observations, coronal holes, inferred interplanetary magnetic field polarities, mean solar magnetic field, solar wind measurements, and Boulder Geomagnetic Substorm Log. It also provides data for March 1979 on: daily solar activity center, sudden ionospheric disturbances, solar X-ray radiation, solar radio emission, cosmic rays, geomagnetic indices and radio propagation indices. GRA N79-34148# National Geophysical and Solar-Terrestrial Data Center, Boulder, Colo. SOLAR-GEOPHYSICAL DATA NUMBER 415, MARCH 1979. PART 2 (COMPREHENSIVE REPORTS): DATA FOR SEPTEMBER 1978, AUGUST 1978 AND MISCELLANEA Helen E. Coffey May 1978 84 p (PB-296276/9; SGD-415-Pt-2; NOAA-79041606) Avail: NTIS HC A05/MF A01 CSCL 03B The data on active regions, synoptic solar maps, solar flares, solar radio emission, and energetic solar particles and plasma are presented from September, 1978. A synoptic chart, abbrevi ated calendar record, and regional flare index for August 1978 are provided. The miscellaneous data includes: solar radio emission. cosmic rays for December 1978, and solar-terrestrial activity 1977. GRA N79-34149# National Oceanic and Atmospheric Administration, Patrick S. McIntosh Feb. 1979 326 p refs (PB-296477/2; UAG-70) Avail: NTIS HC A15/MF A01 CSCL 03B A record of large-scale solar magnetic fields and solar activity during 130 solar rotations, from November 1964 through July 1974 in the form of H-alpha synoptic charts and accompanying descriptive notes is presented. A perspective on large-scale magnetic fields is provided by the inference of lines of polarity reversal from the systems of structures visible in H-alpha patrol filtergrams. These structures map the neutral lines in the radial component of solar magnetic fields, thereby revealing details of the boundaries to large-scale magnetic fields that are not recorded in magnetograms sensitive to the longitudinal (line-of-sight component of the fields. This atlas testifies that neutral lines are of themselves important physical features in solar activity They are associated directly with systems of physical structures. They form continuous lines that often encircle the entire sun. N79-34151 Indiana Univ., Bloomington. Jack ONeal Burns, Jr. 1979 353 p Extended radio galaxies which lie in rich and poor clusters were studied through observations with the NRAO 300 ft single dish telescope, the Green Bank interferometer and the VLA. Detailed total intensity and polarization observations for a more restricted sample of two classical double sources and nine head-tail galaxies were also performed with the NRAO interferometer. The rich and poor radio cluster samples are combined to investigate the relationship between source morphology and the scale sizes of clustering. Potentially fruitful areas of future cluster research of X-ray, optical, and radio frequencies are discussed In particular, the probability of detecting poorer clusters with future X-ray satellites is addressed. Dissert. Abstr N79-34152# Instituto de Pesquisas Espaciais. Sao Jose dos Campos (Brazil). OBSERVATIONS OF EXTRATERRESTRIAL GAMMA RAY BEAMS USING A HIGH ANGULAR RESOLUTION TELESCOPE [OBSERVACOES DE FONTES DE RAIOS GAMA EXTRATERRESTRES COM UM TELESCOPIO DE ALTA RESOLUCAO ANGULAR] J. O. D. Jardim, K. R. Rao, O. D. deAguiar, and I. M. Martin Jun. 1979 10 p refs In PORTUGUESE Presented at the 6th Reuniao Anual da Soc. Astron. Brasil. SAB, 4-6 Jul. 1979 |