scholarly journals Nonthermal X-rays from supernova remnants

2013 ◽  
Vol 9 (S296) ◽  
pp. 245-252
Author(s):  
Anne Decourchelle
Keyword(s):  
Particle Acceleration ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
X Rays ◽  
Significant Progress ◽  
Small Spatial Scale ◽  
Spatially Resolved ◽  
Nonthermal Emission ◽  
Spatially Resolved Spectroscopy

AbstractSince the discovery of nonthermal X-rays in the shell-type supernova remnant SN1006 almost 20 years ago, the field has developed considerably, owing significant progress to our understanding of particle acceleration. Key to the characterization of the nonthermal emission is the ability of current satellites, XMM-Newton and Chandra, to perform spatially resolved spectroscopy at a relatively small spatial scale.In this review, I intend to present the main contributions of the study of nonthermal X-rays from supernova remnants to the understanding of particle acceleration.

scholarly journals GALACTIC AND EXTRAGALACTIC SUPERNOVA REMNANTS AS SITES OF PARTICLE ACCELERATION

2013 ◽  
Vol 53 (A) ◽  
pp. 612-616
Author(s):  
Manami Sasaki
Keyword(s):  
Particle Acceleration ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Strong Shock ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
X Rays ◽  
Basic Physics ◽  
Nearby Galaxies ◽  
Radiation Processes

Supernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into the acceleration of particles to high energies. This paper reviews the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implications for Galactic cosmic ray distribution are discussed.

scholarly journals Probing the effects of hadronic acceleration at the SN 1006 shock front

2013 ◽  
Vol 9 (S296) ◽  
pp. 315-319
Author(s):  
Marco Miceli ◽  
F. Bocchino ◽  
A. Decourchelle ◽  
G. Maurin ◽  
J. Vink ◽  
...  
Keyword(s):  
Particle Acceleration ◽  
Spectral Analysis ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Cosmic Ray ◽  
X Ray ◽  
Spatially Resolved ◽  
Large Program ◽  
Post Shock

AbstractSupernova remnant shocks are strong candidates for being the source of energetic cosmic rays and hadron acceleration is expected to increase the shock compression ratio, providing higher post-shock densities. We exploited the deep observations of the XMM-Newton Large Program on SN 1006 to verify this prediction. Spatially resolved spectral analysis led us to detect X-ray emission from the shocked ambient medium in SN 1006 and to find that its density significantly increases in regions where particle acceleration is efficient. Our results provide evidence for the effects of acceleration of cosmic ray hadrons on the post-shock plasma in supernova remnants.

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 Historical Supernovae and Supernova Remnants

1996 ◽  
Vol 145 ◽  
pp. 323-331 ◽  
Author(s):  
Zhenru Wang
Keyword(s):  
Tang Dynasty ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
High Energy ◽  
X Rays ◽  
Supernovae And Supernova Remnants ◽  
X Ray ◽  
The Tang Dynasty ◽  
High Energy Emission ◽  
The Relationship

The oldest historical supernova (SN), recorded by ancient Chinese in 14th Century B.C. on pieces of tortoise shells or bones, is identified with the aid of modern space γ-ray observations. Hard X-rays with energy up to 20 keV were observed from IC 443 by the X-ray satellite Ginga. We infer from these observations the age of IC 443 is ∼ 1000 — 1400 yrs. The result supports the hypothesis that IC 443 is the remnant of the historical SN 837 that occurred during the Tang Dynasty. The association between the supernova remnant (SNR) CTB 80 and SN 1408 has been hotly debated for about ten years and is briefly reviewed and discussed here. A new picture is presented to explain this association. High energy emission from historical SNRs can persist in a multiphase interstellar medium (ISM). As a result, the study of the relationship between SNRs and ancient guest stars has gained new vitality.

scholarly journals Possible Contributions of Supernova Remnants to the Soft X-ray Diffuse Background (0.1 - 1 keV)

1983 ◽  
Vol 101 ◽  
pp. 361-365
Author(s):  
W. T. Sanders ◽  
D. N. Burrows ◽  
D. McCammon ◽  
W. L. Kraushaar
Keyword(s):  
Supernova Remnants ◽  
Large Scale ◽  
Supernova Remnant ◽  
Galactic Halo ◽  
Galactic Plane ◽  
X Rays ◽  
X Ray ◽  
Band Emission ◽  
Diffuse Background ◽  
Almost All

Almost all of the B band (0.10–0.19 keV) and C band (0.15–0.28 keV) X-rays probably originate in a hot region surrounding the Sun, which Cox and Anderson have modeled as a supernova remnant. This same region may account for a significant fraction of the M band (0.5–1 keV) X-rays if the nonequilibrium models of Cox and Anderson are applicable. A population of distant SNR similar to the local region, with center-to-center spacing of about 300 pc, could provide enough galactic M band emission to fill in the dip in the count rate in the galactic plane that would otherwise be present due to absorption of both the extra-galactic power law flux and any large-scale-height stellar (or galactic halo) emission.

scholarly journals Separating Thermal and Nonthermal X‐Rays in Supernova Remnants. II. Spatially Resolved Fits to SN 1006 AD

2004 ◽  
Vol 600 (2) ◽  
pp. 752-768 ◽  
Author(s):  
K. K. Dyer ◽  
S. P. Reynolds ◽  
K. J. Borkowski
Keyword(s):  
Supernova Remnants ◽  
X Rays ◽  
Spatially Resolved

scholarly journals XMM-Newton observations of the non-thermal supernova remnant HESS J1731−347 (G353.6-0.7)

2017 ◽  
Vol 608 ◽  
pp. A23 ◽  
Author(s):  
V. Doroshenko ◽  
G. Pühlhofer ◽  
A. Bamba ◽  
F. Acero ◽  
W. W. Tian ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Galactic Plane ◽  
Thermal Power ◽  
X Rays ◽  
Absorption Column ◽  
X Ray ◽  
Spatially Resolved ◽  
Absorbing Material ◽  
First Time ◽  
X Ray Absorption

We report on the analysis of XMM-Newton observations of the non-thermal shell-type supernova remnant HESS J1731−347 (G353.6-0.7). For the first time the complete remnant shell has been covered in X-rays, which allowed direct comparison with radio and TeV observations. We carried out a spatially resolved spectral analysis of XMM-Newton data and confirmed the previously reported non-thermal power-law X-ray spectrum of the source with negligible variations of spectral index across the shell. On the other hand, the X-ray absorption column is strongly variable and correlates with the CO emission thus confirming that the absorbing material must be in the foreground and reinforcing the previously suggested lower limit on distance. Finally, we find that the X-ray emission of the remnant is suppressed towards the Galactic plane, which points to lower shock velocities in this region, likely due to the interaction of the shock with the nearby molecular cloud.

scholarly journals Origin of nonthermal emission from the Fermi bubbles and mechanisms of particle acceleration there

2013 ◽  
Vol 9 (S303) ◽  
pp. 399-402
Author(s):  
V. A. Dogiel ◽  
K.-S. Cheng ◽  
D. O. Chernyshov ◽  
C.-M. Ko
Keyword(s):  
Particle Acceleration ◽  
Radio Frequency ◽  
Galactic Center ◽  
Common Origin ◽  
Microwave Range ◽  
X Rays ◽  
Frequency Range ◽  
Nonthermal Emission ◽  
The Common ◽  
Γ Ray

The discovery of the two giant γ-ray lobes (Fermi bubbles) in the Galactic center (see Dobler et al. 2010 and Su et al. 2010) was one of the most impressive events of the last few years in astrophysics. However, some indications on giant structures in the Galactic center (GC) were observed several years before by WMAP in the radio frequency range between 23 and 33 MHz (Finkbeiner 2004), and by ROSAT in hard X-rays (Bland-Hawthorn & Cohen 2003). Recent observations performed by the Planck Collaboration (Ade et al. 2012) found also lobes in the microwave range which spatially coincided the Fermi bubbles that indicated on the common origin of these phenomena.

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