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  • Other Sources  (22)
  • 1980-1984  (16)
  • 1970-1974  (6)
  • 1
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    Predelivery cell and battery summary for SMM 20A h batteries (1981)
    In:  Other Sources
    Details
    Publication Date: 2016-06-07
    Description: Nickel cadmium batteries were performance tested and found to be compatible with the demands and goals of the Solar Maximum Mission flights.
    Keywords: ENERGY PRODUCTION AND CONVERSION
    Type: NASA. Goddard Space Flight Center The 1980 Goddard Space Flight Center Battery Workshop; p 343-347
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    NASA TECHNICAL REPORTS
  • 2
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    Parallel 50 ampere hour nickel cadmium battery performance in the Modular Power Subsystems (MPS) (1980)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: The thermal performance of 50-ampere-hour, nickel cadmium batteries for use in a modular spacecraft is examined in near-Earth orbit simulation. Battery voltage and temperature profiles for temperature extreme cycles are given and discussed.
    Keywords: ENERGY PRODUCTION AND CONVERSION
    Type: NASA. Goddard Space Flight Center The 1979 Goddard Space Flight Center Battery Workshop; p 261-268
    Format: application/pdf
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  • 3
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    X-ray and microwave observations of active regions (1983)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Coordinated high-resolution (1-3 arcsec) observations of two active solar regions (H 421 and H 419) on November 16, 1979, are reported: soft-X-ray filtergrams from a sounding rocket flight, VLA total-intensity and circular-polarization microwave (6-cm) radio maps, KPNO full-disk photospheric magnetograms, and BBSO H-alpha data. The images were converted to 4.8-arcsec/mm-scale transparencies and coaligned on the basis of sunspot positions for comparison. The two active regions are characterized in detail, and intensity, size, and polarization data for the brightest microwave components (BMC) are listed. It is found that 19 of the 32 BMC are farther than 5 arcsec from any sunspot, and that X-ray-emitting structures only rarely correspond to sunspots, or BMC. About one third of the BMC are located at the feet or legs of coronal loops smaller than about 50,000 km. The limitations implied by these obervations for proposed thermal-bremsstrahlung, thermal-gyro-resonance, and nonthermal microwave-emission mechanisms are discussed.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 85; June 198
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  • 4
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    X-ray and H-alpha observations of a filament-disappearance flare - An empirical analysis of the magnetic field configuration (1981)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: On August, 29, 1973, a flare event occurred that involved the disappearance of a filament near central meridian. The event, well-observed in X-rays on Skylab and in H-alpha, was a four-ribbon flare involving both new and old magnetic inversion lines which were roughly parallel. The H-alpha, X-ray, and magnetic field data are used to deduce the magnetic polarities of the H-alpha brightening at the footpoints of the brightest X-ray loops. It is suggested that the event involved a reconnection of magnetic field lines rather than a brightening in place of preexisting loops. The simultaneity of the H-alpha brightening onsets in the four ribbons and the apparent lack of an eruption of the filament are consistent with this interpretation.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 70; Apr. 198
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  • 5
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    Kinematical analysis of flare spray ejecta observed in the corona (1981)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Observations in H-alpha, soft X-ray, white light and radio wavelengths are used to track cool and hot material from limb de-occultation to the extent of six solar radii. The kinematics and thermodynamics of the internal material are determined, along with the overall mass and energy budget of the event. It is found that the majority of the mass and energy is linked with the coronal material, but at least 20% of the ejected mass originated as near-surface prominence material, leading to the conclusions that the upper part of the prominence was being heated to coronal temperatures as it rose through the corona. Evidence was found that a moving type IV burst, indicative of strong magnetic fields, was associated with the upper part of the prominence, and the observations are judged to be most consistent with magnetic propulsion models of coronal transients.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 73; Oct. 198
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  • 6
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    Coronal loops and active region structure (1981)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: Synoptic H-alpha Ca K, magnetograph and Skylab soft X-ray and EUV data were compared for the purpose of identifying the basic coronal magnetic structure of loops in a 'typical' active region and studying its evolution. A complex of activity in July 1973, especially McMath 12417, was emphasized. The principal results are: (1) most of the brightest loops connected the bright f plage to either the sunspot penumbra or to p satellite spots; no non-flaring X-ray loops end in umbrae; (2) short, bright loops had one or both ends in regions of emergent flux, strong field or high field gradients; (3) stable, strongly sheared loop arcades formed over filaments; (4) EFRs were always associated with compact X-ray arcades; and (5) loops connecting to other active regions had their bases in outlying plage of weak field strength in McM 417 where H-alpha fibrils marked the direction of the loops
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 69; Jan. 198
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  • 7
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    The 50 AMP-hour nickel cadmium battery manual (1981)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The battery is designed with a minimum battery to cell weight ratio consistent with adequate containment for operating conditions and dynamic environments and minimized weight. The battery is fully qualified and the environments to which it was successfully subjected were selected by NASA Goddard to cover a wide range of probable uses. The battery is suitable for either near-Earth geosynchronous missions, is compatible with passive or active thermal control systems and may be electrically controlled by a variety of changing routines. The initial application of the 50 A.H. Battery is a near-Earth mission aboard the LANDSAT D Satellite.
    Keywords: ENERGY PRODUCTION AND CONVERSION
    Type: NASA-CR-166701
    Format: application/pdf
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  • 8
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    Mechanical energy output of the 5 September 1973 flare (1980)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The mechanical energy flux of observed macroscopic mass plasma motions in the solar flare of Sept. 5, 1973, is estimated. Consideration is given to the cool eruptive material in the eruptive filament and large surge as revealed by H alpha observations, the moving emission front seen in Ca II as well as H alpha, the piston-driven shock and mass ejection coronal transient observed in radio spectra and flare core motions, and mechanical energy estimates of 5.6 x 10 to the 29th to 8.9 x 10 to the 30th, 9.0 x 10 to the 29th, 2 x 10 to the 30th (thermal) and 10 to the 31st (magnetic), and 9 x 10 to the 24th erg are obtained, respectively, in agreement with previous estimates. It is concluded that the mechanical energy of large-scale mass motions dominates the radiative output of the flare by more than two orders of magnitude, and that a significant portion of the mechanical energy is in the form of magnetic flux delivered to interplanetary space.
    Keywords: SOLAR PHYSICS
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  • 9
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    Results from OSO-IV - The long term behavior of X-ray emitting regions. (1972)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Analysis of images of the sun obtained with the aid of a grazing incidence X-ray telescope on board the OSO IV spacecraft in the 2.5 to 12-A waveband nearly continuously from Oct. 27, 1967, to May 12, 1968. The instrument had sufficient spatial resolution (one and four arc minutes) and temporal resolution (5 to 20 min) to estimate the spatial characteristics of X-ray emitting regions and to monitor the temporal behavior of individual active regions. Variations in the absence of flares of as much as a factor of 10 in the X-ray output of individual regions were observed, with typical durations ranging from several hours to several days. The X-ray time variations are related to observations at optical and radio wavelengths. The results are interpreted under the assumption that the X-ray time variations are caused by temperature changes in the coronal portions of active regions. The contribution of radiative losses to the energy budget of the coronal active region is estimated.
    Keywords: SPACE RADIATION
    Type: Solar Physics; 22; Jan. 197
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    NASA TECHNICAL REPORTS
  • 10
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    Observations of the reappearance of polar coronal holes and the reversal of the polar magnetic field (1984)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Observational data relating to the evolution of the polar magnetic field around sunspot maximum is examined. Particular emphasis is given to coronal hole observations performed during the last two solar maxima. Long-term averages of the latitudinal dependence of the photospheric magnetic field and the evolutionary pattern of the polar crown filaments are used to trace the poleward motion of the reversal of the large-scale field and are compared to the redevelopment of polar holes. Within the context of phenomenological models of the solar cycle, it is concluded that: (1) the process of polarity reversal and redevelopment of polar holes is discontinuous, with surges of flux of old-cycle polarity interrupting the poleward migration of new-cycle flux; (2) contrary to the Babcock (1961) hypothesis, the polar crown disappears months after the magnetic pole reversal; and (3) the observations support suggestions of a poleward meridional flow around solar maximum that cannot be accounted for by Leighton-type (1964) diffusion.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 92; 109-132
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