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
Citations
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Why the braking indices of young pulsars are less than 3
Wen-Cong Chen,Xiang-Dong Li +1 more
TL;DR: In this paper, the authors discuss two possible reasons which cause the observed braking indices n of young radio pulsars to be smaller than 3: (a) the evolving spin-down model of the magnetic field component $B_{\perp}$ increases with time; and (b) the extrinsic braking torque model in which the tidal torques exerted on the pulsar by the fallback disk, and carries away the spin angular momentum from a pulsar.
Journal ArticleDOI
realfast: Real-time, Commensal Fast Transient Surveys with the Very Large Array
Casey J. Law,Geoffrey C. Bower,Sarah Burke-Spolaor,Bryan J. Butler,Paul Demorest,A. Halle,Shakeh E. Khudikyan,T. J. W. Lazio,Martin Pokorny,James Robnett,Michael P. Rupen +10 more
TL;DR: Realfast as discussed by the authors is a commensal, fast transient search system at the Jansky Very Large Array (JVL) that uses a novel architecture to distribute fast-sampled interferometric data to a 32-node, 64-GPU cluster for real-time imaging and transient detection.
Journal ArticleDOI
Pulsating Radio Source at α = 19 h 19 m , δ = +22°
TL;DR: In this article, it was decided to search for radio pulses from this source at these receiver frequencies, which were above that of the original observation at 81 MHz, the first observation being on February 24, 1968.
Journal ArticleDOI
Properties of matter in ultrahigh magnetic fields and the structure of the surface of neutron stars
TL;DR: The physical properties of atoms, molecules, and solids in ultrahigh magnetic fields B 109 G that are believed to exist on the surface of neutron stars are discussed in this article, where a scenario for magnetosphere evolution is proposed which suggests free emission for a young pulsar and strong binding of the matter to the surface at a later stage.
Journal ArticleDOI
The exploration of the unknown
TL;DR: The Square Kilometre Array (SKA) as discussed by the authors was conceived as a telescope which will both test fundamental physical laws and transform our current picture of the Universe. But, the scientific challenges outlined in this book are today's problems, not the old questions which are answered, but the new questions that will be raised by the new types of observations it will permit.
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.