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  • 1
    Electronic Resource
    Electronic Resource
    Gamma-Ray Evidence for a Stellar-Mass Black Hole near the Galactic Center (1989)
    Oxford, UK : Blackwell Publishing Ltd
    Annals of the New York Academy of Sciences 571 (1989), S. 0 
    Details
    ISSN: 1749-6632
    Source: Blackwell Publishing Journal Backfiles 1879-2005
    Topics: Natural Sciences in General
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1111/j.1749-6632.1989.tb50532.x
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  • 2
    Electronic Resource
    Electronic Resource
    Anomalous Temporal Behaviour of NP 0532 (1969)
    [s.l.] : Nature Publishing Group
    Nature 224 (1969), S. 1003-1004 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] If the rate of change of the period P or the frequency v is characterized by dP/dt=Kp/px-2 or dv/dt=-KvVn (1) where n = 5 for the gravitational radiation model3, n = 3 for the magnetic dipole model3, and n=l for the relativistic solar wind model4, only the first and second derivatives of the ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/2241003a0
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  • 3
    Electronic Resource
    Electronic Resource
    Polarization Reversal of Solar Microwave Bursts (1970)
    [s.l.] : Nature Publishing Group
    Nature 226 (1970), S. 68-69 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Table 1. EVENT 01 ! JANUARY 18, 1969 Frequency Polari; sation Max. flux density (MHz) R! R2 10-22 W m-2 Hz-1 9,400 B 0 190 3,750 o L 108 2,000 L L 178 1,000 L R 135 The various theories that may give rise to a reversal of polarization1 may be classified as those which ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/226068a0
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  • 4
    Electronic Resource
    Electronic Resource
    PREFACE (1981)
    Oxford, UK : Blackwell Publishing Ltd
    Annals of the New York Academy of Sciences 375 (1981), S. 0 
    Details
    ISSN: 1749-6632
    Source: Blackwell Publishing Journal Backfiles 1879-2005
    Topics: Natural Sciences in General
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1111/j.1749-6632.1981.tb33685.x
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  • 5
    Electronic Resource
    Electronic Resource
    Ion and relativistic electron acceleration by Alfven and whistler turbulence in solar flares (1982)
    Springer
    Solar physics 113 (1982), S. 195-201 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We show that protons can be accelerated to several GeV in ≲10 s by Alfven turbulence whose energy density is greater than a few erg/cm3. We also show that electrons can be accelerated to tens of MeV on similar time scales by whistler and Alfven turbulence.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00147698
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  • 6
    Electronic Resource
    Electronic Resource
    Determination of the coronal magnetic field and the radio-emitting electron energy from a Type IV solar radio burst (1968)
    Springer
    Solar physics 5 (1968), S. 531-545 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The intensity and frequency spectrum of gyro-synchrotron emission from energetic solar electrons radiating in coronal magnetic fields are calculated. These calculations, based on a recent study of the generation of gyro-synchrotron emission in a magnetoactive plasma, are applied to a Type IV radio burst originating at a high altitude in the solar corona. It is shown that the observed frequency spectrum of the burst, which exhibits very sharp low and high frequency cutoffs, can be best understood in terms of gyro-synchrotron emission in an ionized medium and that from the observed frequency spectrum and the ambient coronal density it is possible to deduce both the magnetic field at the site of the emission and the range of electron energies responsible for the burst.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00147018
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  • 7
    Electronic Resource
    Electronic Resource
    Microwave and hard X-ray bursts from solar flares (1969)
    Springer
    Solar physics 8 (1969), S. 119-141 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We have applied detailed theories of gyro-synchrotron emission and absorption in a magnetoactive plasma, X-ray production by the bremsstrahlung of non-thermal electrons on ambient hydrogen, and electron relaxation in a partially ionized and magnetized gas to the solar flare burst phenomenon. The hard X-ray and microwave bursts are shown to be consistent with a single source of non-thermal electrons, where both emissions arise from electrons with energies 〈 mc 2. Further-more, the experimental X-ray and microwave data allow us to deduce the properties of the electron distribution, and the values of the ambient magnetic field, the hydrogen density, and the size of the emitting region. The proposed model, although derived mostly from observations of the 7 July 1966 flare, is shown to be representative of this type of event.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00150663
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  • 8
    Electronic Resource
    Electronic Resource
    Evolution of energetic protons in twisted magnetic loops (1995)
    Springer
    Solar physics 160 (1995), S. 343-352 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We study the evolution of an ensemble of energetic (1 GeV) protons in a twisted force-free magnetic loop. The protons are followed with a bounce-average method and they are subjected to collisions with ambient gas and pitch-angle scattering by plasrma turbulence in the loop. The proton loss is initially by drift and later by scattering into the loss cone. Gamma rays are produced by pion decays resulting from nuclear reactions of these lost protons. It is found that in order to have long-lasting protons, one of the following scenarios should hold: (1) For small loops (of length ∼ 2 × 109 cm), the twist angle should be about 2π and the turbulence level below 10−8 erg cm−3. (2) For large loops (≳ 1010 cm), the turbulence level should be below 10−6 erg cm−3. These set the conditions for testing the trapping picture as a viable explanation for the observed eight-hour gamma-ray emission.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00732812
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  • 9
    Electronic Resource
    Electronic Resource
    More of the unseen Universe (1985)
    [s.l.] : Nature Publishing Group
    Nature 315 (1985), S. 780-780 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] IN THIS rather brief volume, Dr Hillier has attempted to present the theoretical concepts, the principal observational results and the detection techniques of gamma-ray astronomy. After an introductory chapter and an account of astrophysical gamma-ray production, five chapters are devoted to ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/315780b0
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  • 10
    Electronic Resource
    Electronic Resource
    Li Be B Energetics and Cosmic Ray Origin (1999)
    Springer
    Astrophysics and space science 265 (1999), S. 71-76 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Three different models have been proposed for LiBeB production bycosmic rays: the CRI model in which the cosmic rays areaccelerated out of an ISM of solar composition scaled withmetallicity; the CRS model in which cosmic rays with compositionsimilar to that of the current epoch cosmic rays are acceleratedout of fresh supernova ejecta; and the LECR model in which adistinct low energy component coexists with the postulated cosmicrays of the CRI model. These models are usually distinguished bytheir predictions concerning the evolution of the Be and Babundances. Here we emphasize the energetics which favor the CRSmodel. This model is also favored by observations showing that thebulk (80 to 90%) of all supernovae occur in hot, low densitysuperbubbles, where supernova shocks can accelerate the cosmicrays from supernova ejecta enriched matter.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1002185328791
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