scholarly journals X-ray hotspot flares and implications for cosmic ray acceleration and magnetic field amplification in supernova remnants

2008 ◽  
Vol 386 (1) ◽  
pp. L20-L22 ◽  
Author(s):  
Yousaf M. Butt ◽  
Troy A. Porter ◽  
Boaz Katz ◽  
Eli Waxman
Keyword(s):  
Magnetic Field ◽  
Supernova Remnants ◽  
Cosmic Ray ◽  
X Ray ◽  
Field Amplification ◽  
Cosmic Ray Acceleration

A mechanism for X-ray production in Sco X-1

1969 ◽  
Vol 313 (1514) ◽  
pp. 395-402 ◽  
Keyword(s):  
Magnetic Field ◽  
Particle Acceleration ◽  
Magnetoactive Plasma ◽  
Cosmic Ray ◽  
Field Energy ◽  
Close Collaboration ◽  
Ionized Gas ◽  
X Ray ◽  
Magnetic Field Energy ◽  
Cosmic Ray Acceleration

In this brief talk I should like to present a summary of some recent results on the mechanism of X -ray production in extars, with special emphasis on Sco X-1. These results are an outcome of a close collaboration between Professor S. Olbert of M.I.T. and me. As mentioned by Professor Burbidge earlier today, we hypothesize that galactic X-ray sources are in fact entities wherein ‘frozen in’, compressed magnetic field rapidly relaxes by transferring magnetic field energy to ultrarelativistic (u.r.) electrons. Consider a volume of space filled with magnetoactive plasma. For reasons elaborated on elsewhere (Manley & Olbert 1968, 1969) we do not expect the ionized gas to be homogeneous. Rather we expect it to consist of an aggregate of long thin plasmoids acting almost independently of one another. We now postulate the presence of random Alfvén waves (m.h.d. noise) propagating back and forth, along the plasmoids, and inquire into the possibility of charged particle acceleration by interaction with these noisy plasmoids. This is akin to the cosmic ray acceleration mechanism proposed by Fermi, who however, considered only interactions with large, approximately spherical plasmoids.

scholarly journals Search for Nonthermal X-Rays from Supernova Remnant Shells

1998 ◽  
Vol 188 ◽  
pp. 117-120
Author(s):  
R. Petre ◽  
J. Keohane ◽  
U. Hwang ◽  
G. Allen ◽  
E. Gotthelf
Keyword(s):  
Radio Emission ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Cosmic Ray ◽  
High Energy ◽  
X Rays ◽  
X Ray ◽  
Nonthermal Radio ◽  
Cosmic Ray Acceleration ◽  
Nonthermal Radio Emission

The suggestion that the shocks of supernova remnants (SNR's) are cosmic ray acceleration sites dates back more than 40 years. While observations of nonthermal radio emission from SNR shells indicate the ubiquity of GeV cosmic ray production, there is still theoretical debate about whether SNR shocks accelerate particles up to the well-known “knee” in the primary cosmic ray spectrum at ~3,000 TeV. Recent X-ray observations of SN1006 and other SNR's may have provided the missing observational link between SNR shocks and high energy cosmic ray acceleration. We discuss these observations and their interpretation, and summarize our ongoing efforts to find evidence from X-ray observations of cosmic ray acceleration in the shells of other SNR's.

scholarly journals Cosmic ray acceleration by shocks: spectral steepening due to turbulent magnetic field amplification

2019 ◽  
Vol 488 (2) ◽  
pp. 2466-2472 ◽  
Author(s):  
A R Bell ◽  
J H Matthews ◽  
K M Blundell
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Ray ◽  
Field Amplification ◽  
Cosmic Ray Acceleration

Abstract We show that the energy required to turbulently amplify magnetic field during cosmic ray (CR) acceleration by shocks extracts energy from the CR and steepens the CR energy spectrum.

Particle acceleration at forward and reverse shocks in SNRs

2018 ◽  
Vol 27 (10) ◽  
pp. 1844023 ◽  
Author(s):  
Vladimir Zirakashvili
Keyword(s):  
Supernova Remnants ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Field Amplification ◽  
Streaming Instability ◽  
Cosmic Ray Acceleration ◽  
Astrophysical Neutrinos ◽  
Astrophysical Shocks ◽  
Accelerated Particles

Cosmic ray acceleration by astrophysical shocks in supernova remnants is briefly reviewed. Results of numerical modeling taking into account the magnetic field amplification by streaming instability and the shock modification are presented. Nonthermal emission produced by accelerated particles in old supernova remnants is compared with available data of modern radio, X-ray and gamma-ray astronomies. It is also shown that high-energy neutrinos produced in young supernova remnants of Type IIn extragalactic supernova can explain the recent IceCube detection of astrophysical neutrinos.

scholarly journals X-ray Emission as an Indicator of Cosmic ray Acceleration in Supernova Remnants

2000 ◽  
Vol 195 ◽  
pp. 69-76
Author(s):  
R. Petre ◽  
G. E. Allen ◽  
U. Hwang ◽  
J. W. Keohane ◽  
E. V. Gotthelf
Keyword(s):  
Supernova Remnants ◽  
Cosmic Ray ◽  
Systematic Investigation ◽  
Shock Acceleration ◽  
Acceleration Process ◽  
X Ray ◽  
Cosmic Ray Acceleration ◽  
The Status ◽  
Tev Gamma Rays ◽  
Cas A

X-ray observations over the past several years have led to the discovery of nonthermal X-ray emission arising in the shells of many young supernova remnants, including SN 1006, Cas A, and Tycho. This emission is thought to be synchrotron emission from electrons that have been shock accelerated to hundreds of TeV, and thus represents strong evidence that cosmic rays are accelerated in SNR shocks. The X-ray observations are corroborated by detection of TeV gamma rays from two of these remnants. A systematic investigation of young, shell-like remnants suggests that the nonthermal X-ray emission from shock-accelerated electrons is a common, if not ubiquitous, feature. We review the status of the X-ray observations and describe how they can be used to provide insight into the shock acceleration process.

Sign in / Sign up

Export Citation Format

Share Document