The acceleration of cosmic rays in shock fronts – I
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This article is published in Monthly Notices of the Royal Astronomical Society.The article was published on 1978-02-01 and is currently open access. It has received 2613 citations till now. The article focuses on the topics: Shock waves in astrophysics & Fermi acceleration.read more
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Two-stream-like instability in dilute hot relativistic beams and astrophysical relativistic shocks
TL;DR: In this paper, the authors explore the linear growth of kinetic modes appearing in the precursor-upstream interaction in relativistic shocks propagating in non-and weakly magnetized plasmas: electrostatic two-stream parallel mode and electrostatic oblique modes.
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XMM-Newton and INTEGRAL analysis of the Ophiuchus cluster of galaxies
TL;DR: In this paper, the authors investigated the non-thermal hard X-ray emission in the Ophiuchus cluster of galaxies and found that this component produces approximately 10% of the total flux in the 1-10 keV band.
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Modelling the multi-wavelength emission of flat-spectrum radio quasar 3C 279
Y. G. Zheng,Chuyuan Yang +1 more
TL;DR: In this paper, the authors employed a length-dependent conical jet model for the jet structure and emission properties of flat-spectrum radio quasar 3C 279 in the steady state.
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Testing the theory of colliding winds: the periastron passage of 9 Sagittarii - I. X-ray and optical spectroscopy
Gregor Rauw,R. Blomme,Yaël Nazé,M. Spano,Laurent Mahy,Eric Gosset,D. Volpi,H. Van Winckel,Gert Raskin,C. Waelkens +9 more
TL;DR: In this article, a multi-wavelength monitoring campaign of the O-star binary 9 Sgr around the 2013 periastron was conducted, where X-ray observations and optical spectroscopy were used to test the predictions of colliding stellar winds over a broad range of wavelengths.
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Search for Diffuse X-rays from the Bow Shock Region of Runaway Star BD+43$^\circ$3654 with Suzaku
TL;DR: In this article, the maximum energy of accelerated particles from measurements of possible non-thermal emissions in the X-ray band was constrained with an exposure of 99 k s. This result leads to three conclusions: (1) a shock-heating process is inefficient on this system; (2) the energy of electrons does not exceed 10 TeV, corresponding to a Lorentz factor of less than $10^7$; and (3) the magnetic field in the shock acceleration site might not be as turbulent as those in pulsar wind nebulae