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  • 1
    Electronic Resource
    Electronic Resource
    The solar maximum mission (1983)
    Springer
    Solar physics 86 (1983), S. 7-7 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157169
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  • 2
    Electronic Resource
    Electronic Resource
    The 78.4-day period of Cygnus XR-1 (1979)
    [s.l.] : Nature Publishing Group
    Nature 280 (1979), S. 126-127 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Analysis of the power spectrum of the U-band polarisation of HDE226868 on 225 nights between 1974 and 1977 led to the original detection by Kemp et al.2 of a 39.2-d modulation in the magnitude of polarisation with peak-to-peak amplitude of 0.25% (or 0.0054 mag). A modulation with a 78.4-d period ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/280126a0
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  • 3
    Electronic Resource
    Electronic Resource
    X-ray observations of AM Herculis from OSO 8 (1979)
    [s.l.] : Nature Publishing Group
    Nature 279 (1979), S. 509-510 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The OSO 8 instruments used to observe AM Her consist of a proportional counter7 covering the photon energy range 2-40 keV, and a high energy scintillation spectrometer8 covering the range 20-250 keV. The source was observed during the period 1-10 October 1977. The results presented here from the ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/279509a0
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  • 4
    Electronic Resource
    Electronic Resource
    High energy X-ray spectrum of Her X-1 (1978)
    [s.l.] : Nature Publishing Group
    Nature 275 (1978), S. 195-197 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The discovery by Triimper et al.5,6 of two strong lines in the pulsed X-ray spectrum of Her X-1 has inspired many other groups to search for this phenomenon. The stronger of the two lines, at 5 8 ± 5 keV, has now been observed by Trumper et al. on two separate balloon flights, one in May ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/275195a0
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  • 5
    Electronic Resource
    Electronic Resource
    Intensity transitions in Cyg XR-1 observed at high energies from OSO 8 (1977)
    [s.l.] : Nature Publishing Group
    Nature 267 (1977), S. 813-815 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Cyg XR-1 was observed with the high energy X-ray spectrometer on board the OSO-8 satellite from 11 to 19 November, 1975, and from 27 October to 15 November, 1976 (excluding the period from 1 November to 7 November, 1976). The CsI(Na) scintillation spectrometer is sensitive to radiation in the 20 ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/267813a0
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  • 6
    Electronic Resource
    Electronic Resource
    The Hard X-Ray Burst Spectrometer on the Solar Maximum Mission (1980)
    Springer
    Solar physics 65 (1980), S. 25-37 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The primary scientific objectives of the Hard X-Ray Burst Spectrometer (HXRBS) to be flown on the Solar Maximum Mission are as follows: (1) To determine the nature of the mechanisms which accelerate electrons to 20–100 keV in the first stage of a solar flare and to 〉 1 MeV in the second stage of many flares; and (2) to characterize the spatial and temporal relation between electron acceleration, storage and energy loss throughout a solar flare. Measurements of the spectrum of solar X-rays will be made in the energy range from 20 to 260 keV using an actively-shielded CsI(Na) scintillator with a thickness of 0.635 cm and a sensitive area of 71 cm2. Continuous measurements with a time resolution of 0.128 s will be made of the 15-channel energy-loss spectrum of events in this scintillator in anticoincidence with events in the CsI(Na) shield. Counting-rate data with a time resolution as short as 1 ms will also be available from a limited period each orbit using a 32K-word circulating memory triggered by a high event rate. In the first year after launch, it is expected that approximately 1000 flares will be observed above the instrument sensitivity threshold, which corresponds to a 20–200 keV X-ray flux of 2 × 10−1 photons (cm2 s)−1 lasting for at least one second.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151382
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  • 7
    Electronic Resource
    Electronic Resource
    Microwave and hard X-Ray observations of a solar flare with a time resolution better than 100 ms (1983)
    Springer
    Solar physics 84 (1983), S. 311-319 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Simultaneous microwave and X-ray observations are presented for a solar flare detected on May 8, 1980 starting at 19:37 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 Observatory 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 peaks 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 1.5 s. 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.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157464
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  • 8
    Electronic Resource
    Electronic Resource
    Fast transients in hard X-ray solar flares (1983)
    Springer
    Solar physics 86 (1983), S. 239-240 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present the results of a search for fast spikes in 5483 hard X-ray solar flares as observed with the Hard X-Ray Burst Spectrometer on the Solar Maximum Mission (SMM). Hundreds of fast spikes with durations of less than 1 second have been detected at time resolutions of 128 ms and 10 ms. Fast spikes have been detected with rise and decay times as short as 20 ms and with widths as short at 45 ms that represent the fastest hard X-ray variations yet seen from the Sun. The observations of such fast variations place new constraints on the physical nature of the source.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157195
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  • 9
    Electronic Resource
    Electronic Resource
    Characteristics of gamma-ray line flares as observed in hard X-ray emissions and other phenomena (1983)
    Springer
    Solar physics 86 (1983), S. 409-419 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Observations of gamma-ray lines from solar flares by SMM demonstrated that energetic protons and heavy ions are accelerated during the impulsive phase. In order to understand the acceleration mechanism for gamma-ray producing protons and heavy ions, we have studied the characteristics of the flares from which gamma-ray lines were observed by SMM In order to identify the characteristics unique to the gamma-ray line flares, we have also studied intense hard X-ray flares with no gamma-ray line emissions. We have found the following characteristics: 1) Most of the gamma-ray line flares produced intense radio bursts of types II and IV. 2) For most of the gamma-ray line flares, the time profiles of high-energy (≳ 300 keV) hard X-rays are delayed by order of several seconds with respect to those of low-energy hard X-rays. The delay times seem to be correlated with the spatial sizes of the flares. 3) In Hα importance, the gamma-ray line flares range from sub-flares to importance-3 flares. 4) The hard X-ray spectra of the gamma-ray line flares are generally flatter (harder) than those of flares with no gamma-ray line emission. From these characteristics, we conclude that the first-order Fermi acceleration operating in a flare loop is likely to be the acceleration mechanism for energetic protons and heavy ions as well as relativistic electrons.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00157214
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  • 10
    Electronic Resource
    Electronic Resource
    The impulsive and gradual phases of a solar limb flare as observed from the solar maximum mission satellite (1982)
    Springer
    Solar physics 78 (1982), S. 201-213 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Simultaneous observations of a solar limb flare in the X-ray and ultraviolet regions of the spectrum are presented. Temporal and spectral X-ray observations were obtained for the 25–300 keV range while temporal, spectral, and spatial X-ray observations were obtained for the 30–0.3 keV range. The ultraviolet observations were images with a 10″ spatial resolution in the lines of O v (T e ∼ 2.5 × 105 K) and Fe xxi (T e ∼ 1.1 × 107 K). The hard X-ray and O v data indicate that the impulsive phase began in the photosphere or chromosphere and continued for several minutes as material was ejected into the corona. Impulsive excitation was observed up to 30 000 km above the solar surface at specific points in the flare loop. The Fe xxi observations indicate a preheating before the impulsive phase and showed the formation of hot post-flare loops. This later formation was confirmed by soft X-ray observations. These observations provide limitations for current flare models and will provide the data needed for initial conditions in modeling the concurrent coronal transient.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151603
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