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  • 1
    Electronic Resource
    Electronic Resource
    X-ray emission from γ -ray sources in the galactic anticentre region (1979)
    [s.l.] : Nature Publishing Group
    Nature 282 (1979), S. 692-695 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Following the detection of 13 localised sources of high-energy ?-radiation2, attempts have been made to correlate them with a variety of astrophysical objects. These include X-ray sources3"6, optical counterparts7, Hll regions8, supernova remnants9"11, highly variable galactic radio sources12, ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/282692a0
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  • 2
    Electronic Resource
    Electronic Resource
    GX339–4: a new black hole candidate (1979)
    [s.l.] : Nature Publishing Group
    Nature 278 (1979), S. 434-436 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The HEAO observations were made on 10-14 September 1977, 8-12 March 1978 and 10-14 September 1978. The average intensities in the 1-20 keV range of GX339-4 during these observations were -0.25, -0.01, and -0.8 ctcm2s1, respectively (1 HEAO ct cm'2 s"1 = 200 Uhuru flux units). These values are ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/278434a0
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  • 3
    Electronic Resource
    Electronic Resource
    BATSE/OSSE rapid burst response (1995)
    Springer
    Astrophysics and space science 231 (1995), S. 127-130 
    Details
    ISSN: 1572-946X
    Keywords: Gamma-ray bursts ; Counterparts ; Instrumentation
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The BATSE and OSSE instrument teams have modified flight software to promptly (within 2 min of trigger) slew the OSSE detectors to burst locations determined on-board by BATSE. This enables OSSE to make sensitive searches for prompt and delayed post-burst line and continuum emission above 50 keV. In the best cases our sensitivity will be more than an order of magnitude better than any other search in this energy range. We expect to slew to 1–2 bursts per month, based on the OSSE FOV and BATSE event rate. Detections or limits from continued operation of this system may provide significant constraints on burst models. As an example of the observations made using this system, we present preliminary limits for post-burst emission from GRB 950223 on several time scales.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00658601
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  • 4
    Electronic Resource
    Electronic Resource
    Discovery of two cosmic X-ray bursts in 1970 (1976)
    Springer
    Astrophysics and space science 42 (1976), S. 29-33 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Two bursts of high-energy photons have been discovered during analysis of 2 1/2 years of data from NRL's solar X-ray detector on OSO-6. Both bursts were simultaneously observed by the OGO-5 hard X-ray spectrometer (Kane, 1975). The bursts occurred at about 18 087 s UT on 25 January, 1970, and about 56 532 s UT on 1 October, 1970. The October event was also observed by Vela 5A; however, none of the Vela detectors observed the January event which had an intensity of about 2×10−5 ergs cm−2. Based on these new data, the number of bursts with intensities above about 10−5 ergs cm−2 appears to be about 50% higher than the Vela data alone would indicate.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00645520
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  • 5
    Electronic Resource
    Electronic Resource
    The gamma ray spectrometer for the Solar Maximum Mission (1980)
    Springer
    Solar physics 65 (1980), S. 15-23 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The Solar Maximum Mission Gamma Ray Experiment (SMM GRE) utilizes an actively shielded, multicrystal scintillation spectrometer to measure the flux of solar gamma rays. The instrument provides a 476-channel pulse height spectrum (with energy resolution of ∼7% at 662 keV) every 16.38 s over the energy range 0.3–9 MeV. Higher time resolution (2 s) is available in three windows between 3.5 and 6.5 MeV to study prompt gamma ray line emission at 4.4 and 6.1 MeV. Gamma ray spectral analysis can be extended to ≳15 MeV on command. Photons in the energy band from 300–350 keV are recorded with a time resolution of 64 ms. A high energy configuration also gives the spectrum of photons in the energy range from 10–100 MeV and the flux of neutrons ≳20 MeV. Both have a time resolution of 2 s. Auxiliary X-ray detectors will provide spectra with 1-sec time resolution over the energy range of 10–140 keV. The instrument is designed to measure the intensity, energy, and Doppler shift of narrow gamma ray lines as well as the intensity of extremely broadened lines and the photon continuum. The main objective is to use this time and spectral information from both nuclear gamma ray lines and the photon continuum in a direct study of the dynamics of the solar flare/particle acceleration phenomena.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151381
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  • 6
    Electronic Resource
    Electronic Resource
    Upper limit on the steady emission of the 2.223 MeV neutron capture γ-ray line from the Sun (1992)
    Springer
    Solar physics 142 (1992), S. 171-185 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Data accumulated by the Solar Maximum Mission Gamma Ray Spectrometer (GRS) have been searched for evidence of the 2.223 MeV neutron capture line from the Sun, outside the times of γ-ray-emitting solar flares. Background-corrected spectra accumulated over 3-day intervals between 1980 and 1989 show no evidence of the line. Upper limits are reported separately for periods of high and low solar activity. A conservative 3σ upper limit of 5.7 × 10−5 γ (cm2 s)−1 is placed on the steady flux in the 2.223 MeV line during inactive periods, which is nearly two orders of magnitude lower than previously published results. After correction for limb darkening of the line emission from off-center positions, this upper limit becomes 7.1 × 10−5 γ (cm2s)−1. Our 3σ upper limit on the steady flux in the line during periods of high solar activity is 6.9 × 10−5 γ (cm2 s)−1, or 8.6 × 10−5 γ (cm2 s)−1 after correction for limb darkening. Our results imply that the quiescent solar corona cannot be heated by ions accelerated above 1 MeV in microflares (or a continuous acceleration process), so long as the ion energy spectrum is similar to that measured in large flares. We also use our results to derive the rate of tritium production at the solar surface; our upper limit of 9 nuclei (cm2 s)−1 is about a factor of 9 below the upper limit from searches for 3H in the solar wind. We place upper limits of the order 1033 on the number of energetic (〉 30 MeV) protons which can be stored in active regions prior to being released in solar flares, which imply that the strongest observed flares cannot be produced by such a mechanism.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00156640
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  • 7
    Electronic Resource
    Electronic Resource
    Spectral feature of 31 December 1981 γ -ray burst not confirmed (1984)
    [s.l.] : Nature Publishing Group
    Nature 311 (1984), S. 360-362 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Annihilation lines have been reported in 5% of the bursts observed by the Konus instruments from 1978 to 19821'3. The typical emission features observed by Konus are centred at 400-450 keV and have widths of -200 keV (FWHM). The strong feature in the 5 March 1979 burst2 fits this description; ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/311360a0
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  • 8
    Electronic Resource
    Electronic Resource
    Experiment to detect Pulsed γ-Rays from the Crab Nebula (1971)
    [s.l.] : Nature Publishing Group
    Nature 229 (1971), S. 187-189 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The telescope is shown in Fig. 1. y-Rays are detected when they interact in a nuclear emulsion stack (650 cm2, 0.6 radiation length) producing electron pairs or Compton recoil electrons which traverse a multi-wire proportional counter and a pair of plastic scintillation counters. An upper energy ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/229187a0
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  • 9
    Electronic Resource
    Electronic Resource
    A 154-day periodicity in the occurrence of hard solar flares? (1984)
    [s.l.] : Nature Publishing Group
    Nature 312 (1984), S. 623-625 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] The SMM satellite was launched into a near-circular orbit with an inclination of 28.5 and an altitude of 570 km. The orbit processes, relative to the Earth-Sun line, with a period of -48 days. Because of the decay of the orbit, the period of revolution has decreased. In November 1980, the ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/312623a0
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  • 10
    Electronic Resource
    Electronic Resource
    Osse limits on pre- and post-burst emission (1995)
    Springer
    Astrophysics and space science 231 (1995), S. 123-126 
    Details
    ISSN: 1572-946X
    Keywords: Gamma-ray bursts ; Counterparts
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The existence of either pre- or post-burst emission can provide substantial new information about the burst source and its local environment. We have data from serveral events serendipitously in or near the OSSE field of view at the time of the burst. We present pre- and post-burst flux limits from one such event, GRB 940301. The OSSE data for other periods when scheduled observations have included burst locations will enable us to search for pre- and post- burst emission on many time scales.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00658600
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