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  • 1
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    Trapped-proton energy spectrum determination (M0002-1) (1984)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: The objective of this experiment is to measure the flux and energy spectrum of protons with energies of 1 to MeV. These protons are trapped on the Earth's magnetic field lines as part of the inner radiation belt, or Van Allen zone. The proton will be encountered predominantly in the South Atlantic anomaly at a 90 deg pitch angle.
    Keywords: SPACE RADIATION
    Type: NASA. Langley Research Center Long Duration Exposure Facility (LDEF); p 109-112
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  • 2
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    The diffuse X-ray background spectrum from 3 to 50 keV (1980)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: The spectrum of the extragalactic diffuse X-ray background has been measured with the GSFC Cosmic X-ray Experiment on HEAO 1 for regions of the sky away from known point sources and more than 20 deg from the galactic plane. A total exposure of 80 sq m-s-sr is available at present. Free-free emission from an optically thin plasma of 40 plus or minus 5 keV provides an excellent description of the observed spectrum from 3 to 50 keV. This spectral shape is confirmed by measurements from five separate layers of three independent detectors. With an estimated absolute precision of about 10%, the intensity of the emission at 10keV is 3.2 keV/keV/sq cm/s/sr, a value consistent with the average of previously reported spectra. A uniform hot intergalactic medium of approximately 36% of the closure density of the universe would produce such a flux, although nonuniform models indicating less total matter are probably more realistic.
    Keywords: SPACE RADIATION
    Type: Astrophysical Journal; vol. 235
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  • 3
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    Observations of the 1980 April 30 limb flare by the ultraviolet spectrometer and polarimeter on the Solar Maximum Mission (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Observations of the M2 limb flare of 1980 April 30 by the ultraviolet spectrometer and polarimeter in the C IV 1548 A line are described and compared with observations from other SMM instruments and with ground-based H-alpha data. Events observed during the 18 minutes leading up to the flare impulsive phase include the filling of a small loop with material moving at about 20 km/s, followed by a rapid brightening in C IV, H-alpha, and hard X-rays, with a subsequent brightening of a higher set of loops. The rapid brightening appears to be at the junction of the small loop with the overlying magnetic structures, which suggests the flare may be caused by their interaction.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; vol. 244
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  • 4
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    Spatial and temporal structures of impulsive bursts from solar flares observed in UV and hard X-rays (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: New observations are presented of impulsive UV and hard X-rays bursts in two solar flares obtained with instruments on Solar Maximum Mission. The UV bursts were observed in the Si IV and O IV emission lines, whose intensity ratio is density-sensitive. By comparing the spatially resolved Si IV/O IV observations with the corresponding hard X-ray observations, it is possible to study their spatial and temporal relationships. For one flare, the individual component spikes in the multiply peaked hard X-ray burst can be identified with different discrete Si IV/O IV flaring kernels of size 4 arcsec x 4 arcsec or smaller, which brighten up sequentially in time. For the other, many Si IV/O kernels, widely distributed over a large area, show impulsive bursts at the same time, which correlate with the main peak of the impulsive hard X-ray burst. The density of the flaring Si IV/O IV kernels is in the range from 5 x 10 to the 12th-13th/cu cm.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; vol. 248
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  • 5
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    Observations of solar flare transition zone plasmas from the Solar Maximum Mission (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The spatial and temporal evolution of the Si IV and O IV intensity, density and mass motions in preflare and flare transition zone plasmas are studied for the case of the April 8, 1980 flare. It is found that: (1) the UV flare observed in the Si IV and O IV lines is unambiguously identified as occurring in a low-lying, preexisting transition zone loop which spanned the magnetic neutral line separating a larger leader spot and a newly emerged, isolated spot of opposite polarity; (2) at the onset of the flare, the easternmost footpoint, which was anchored in an isolated spot region of high longitudinal magnetic field gradient, showed sudden, impulsive brightening with large intensity increases; and (3) the release flare energy was transported by way of large-scale connecting field lines to other parts of the active region, producing the hot plasma and H-alpha kernels observed near the trailing spot.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; vol. 253
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  • 6
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    The development and cooling of a solar limb-flare (1984)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: Observations of a flare that began in soft X-rays at 20:37 UT on April 12, 1980 at the west limb of the sun are discussed. The observations of the flare and postflare loops are first described, and the Solar Maximum Mission data are interpreted in terms of the temperature, density, and geometry of the emitting regions. The observed postflare cooling time is compared with that expected from radiation, conduction, and enthalpy flux. The loop model is discussed, and the observed events are compared with other proposed models.
    Keywords: SOLAR PHYSICS
    Type: Royal Astronomical Society, Monthly Notices (ISSN 0035-8711); 210; 443-462
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  • 7
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    The analysis of solar models: Neutrinos and oscillations (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Tests of solar neutrino flux and solar oscillation frequencies were used to assess standard stellar structure theory. Standard and non-standard solar models are enumerated and discussed. The field of solar seismology, wherein the solar interior is studied from the measurement of solar oscillations, is introduced.
    Keywords: SOLAR PHYSICS
    Type: NASA-CR-173628 , NAS 1.26:173628 , PREPRINT-153
    Format: application/pdf
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  • 8
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    A 5.57 hour modulation of the X-ray flux of 4U1822-37: A new model for CYG X-3 (1981)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The X-ray flux of 4U1822-37 is shown to be modulated with the 5.57 hour period of its optical counterpart. The X-ray light curve is two component with a smooth sinusoidal like 25 percent semiamplitude modulation and a 30 minute dip approximately 0.2 in phase following the other minimum. The X-ray spectrum is a relatively flat power law up to 17 keV, above which its steepens. Iron emission is detected at 6.7 keV with a 4 keV FWHM and an equivalent width of 1100 eV. There is an excee below 2 keV that is consistent with either a 0.25 keV thermal component or 350 eV equivalent width iron L emission. A slight softening of the spectrum is seen during both X-ray minima. The dip is interpreted as the partial occultation of an extended cloud of optically thick highly ionized material surrounding the central X-ray source. Modeling the eclipse gives a system inclination of 70-79 deg and a spherical cloud radius of 0.2-0.3 solar radius. Models for the long term modulation are considered. The properties of this source are compared to those of Cyg X-3. It is concluded that they are similar systems.
    Keywords: SPACE RADIATION
    Type: NASA-TM-82079
    Format: application/pdf
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  • 9
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    Super-alfvenic propagation of cosmic rays: The role of streaming modes (1980)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Numerous cosmic ray propagation and acceleration problems require knowledge of the propagation speed of relativistic particles through an ambient plasma. Previous calculations indicated that self-generated turbulence scatters relativistic particles and reduces their bulk streaming velocity to the Alfven speed. This result was incorporated into all currently prominent theories of cosmic ray acceleration and propagation. It is demonstrated that super-Alfvenic propagation is indeed possible for a wide range of physical parameters. This fact dramatically affects the predictions of these models.
    Keywords: SPACE RADIATION
    Type: NASA-TM-82032
    Format: application/pdf
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  • 10
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    The X-ray spectrum of QSO 0241+622 (1980)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Proportional counters on the OsO-8 spacecraft measured the X-ray spectrum of QSR 0241+622 in the range 2-50 keV. The best power law fit has a proton spectral index and 90 percent errors gamma = 1.93 (+0.5, -0.3) and low energy absorption consistent with reported gas column densities, but a thermal bremsstrahlung form with temperature 13.1 keV cannot be excluded. No indication of spectral variability is found in three observations of the source with HEAO-A2, although a possible 15-30 percent intensity change over a period of 6 months was observed. The quasar is similar to 3C 273 in the proportion of energy emitted in various bands, excluding the radio, if reported radiation above 50 keV from its direction is indeed associated with QSO 0241+622. The two quasars are compared and possible energy generation scenarios are discussed. Implications concerning quasar contributions to the diffuse background are discussed.
    Keywords: SPACE RADIATION
    Type: NASA-TM-80645
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