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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The effect of HII regions on rotation measure of pulsars
TL;DR: In this article, the authors obtained new rotation measures for 11 pulsars observed with the Effelsberg 100-m radio telescope, in the direction of the Perseus arm, in order to study the magnetic field structure towards the PSR J2337+6151 and found that two pulsars towards I ∼ 149° (Region 1) and four pulsars toward l ∼ 113° (region 2) lie behind HII regions which seriously affect the pulsar rotation measures.
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Mission Overview and Initial Observation Results of the X-Ray Pulsar Navigation-I Satellite
TL;DR: In this article, the authors presented the initial observation results and aimed to recover the Crab pulsar's pulse profile to verify the X-ray instrument's capability of observing pulsars in space.
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Evidence for three-dimensional spin-velocity alignment in a pulsar
Jumei Yao,Weiwei Zhu,Richard N. Manchester,William A. Coles,Di Li,Di Li,Na Wang,Michael Kramer,Michael Kramer,Daniel R. Stinebring,Yi Feng,W. M. Yan,Chenchen Miao,Mao Yuan,Pei Wang,Jiguang Lu +15 more
TL;DR: In this paper, the authors reported evidence for three-dimensional alignment between the spin and velocity vectors, largely based on observations made with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST) of the pulsar PSR J0538+2817 and its associated supernova remnant S147.
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Millisecond radio pulsars with known masses: Parameter values and equation of state models
Sudip Bhattacharyya,Ignazio Bombaci,Debades Bandyopadhyay,Arun V. Thampan,Arun V. Thampan,Domenico Logoteta +5 more
TL;DR: In this article, a detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS.
Journal ArticleDOI
Evidence for magnetospheric effects on the radiation of radio pulsars
TL;DR: In this paper, the authors conducted the largest investigation to date into the origin of phase resolved, apparent RM variations in the polarized signals of radio pulsars, and they concluded that scattering cannot be the only cause of RM variations, and showed clear examples where magnetospheric effects dominate.
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.