Journal ArticleDOI
Observation of a Rapidly Pulsating Radio Source
TLDR
In this article, the first report of a curious class of astronomical radio sources, distinguished by their rapid and extremely regular pulsations, was made by Hewish et al. They are now understood to be rapidly rotating, magnetized neutron stars, or pulsars.Abstract:
Unusual signals from pulsating radio sources have been recorded at the Mullard Radio Astronomy Observatory The radiation seems to come from local objects within the galaxy, and may be associated with oscillations of white dwarf or neutron stars 1968 saw the first report of a curious class of astronomical radio sources, distinguished by their rapid and extremely regular pulsations Hewish et al associated them with unusually stable oscillations in compact stars They are now understood to be rapidly rotating, magnetized neutron stars, or pulsarsread more
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Magnetic Dipole Radiation from Pulsars
Abstract: RADIO astronomers1–3 have recently discovered pulsars in Vela and near the Crab nebula which seem to be associated with supernova remnants and have repetition periods (0.0892 s and 0.0331 s) considerably shorter than those previously found. The very wide range (60-fold) of periods at present observed is difficult to understand if pulsars are in fact pulsating objects of a single class, because in general (period) ∝ (density)−1/2 and an extremely wide range of density would be required. Of the remaining clock mechanisms proposed, rotation4,5 seems most consistent with the observations. The extremely short periods exclude white dwarfs and make the suggestion of neutron stars more likely.
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Amplitude Variations in Pulsed Radio Sources
TL;DR: In this paper, the long period fluctuations in the amplitudes of radio signals from the pulsed sources from the interstellar medium have been investigated, and it was shown that these fluctuations may be caused by irregularities in the medium.
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Time-dependent pair cascades in magnetospheres of neutron stars - I. Dynamics of the polar cap cascade with no particle supply from the neutron star surface
Andrey Timokhin,Andrey Timokhin +1 more
TL;DR: In this article, a general numerical algorithm for doing self-consistent kinetic simulations of electron-positron cascades is presented, where particle acceleration, pair creation and screening of the electric field are simultaneously calculated.
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Strange stars in Krori-Barua space-time
TL;DR: The singularity free space-time metric obtained by Krori and Barua (J. Phys. A, Math. Gen. 8:508, 1975) satisfies the physical requirements of a realistic star as discussed by the authors.
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Hydrodynamic Approaches in Relativistic Heavy Ion Reactions
TL;DR: In this paper, the authors review several facets of the hydrodynamic description of the relativistic heavy ion collisions, starting from the historical motivation to the present understandings of the observed collective aspects of experimental data, especially those of the most recent RHIC and LHC results.
References
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Journal ArticleDOI
Interplanetary Scintillation of Small Diameter Radio Sources
TL;DR: In this article, the authors used the black-body equations to calculate the increased radiation appropriate to the observed brightness increase in the star over a 1,000 A.u. band-width at 5,400 A.U.
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Normal modes of radial pulsation of stars at the end point of thermonuclear evolution
David W. Meltzer,Kip S. Thorne +1 more
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Energetic Particles from the Sun
C. E. Fichtel,F. B. Mcdonald +1 more
TL;DR: In this article, the authors discuss the association of solar cosmic rays with flare association, solar particle acceleration, recurrence and low energy solar particle events, and discuss the effects of solar particle particle acceleration.
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Possible magnetospheric phenomena associated with neutron stars
TL;DR: In this paper, it was shown that the importance of the early cooling by emission of neutrinos from the Urca process has been underestimated in the foregoing investigations, and the calculations of Miss Tsuruta indicate that a neutron star will rapidly cool to 3 or 4 × 106 °K, but that after 105 years its surface temperature will still be about 2 × 106°K.