scholarly journals X-ray Spectroscopy of the Southwest Cygnus Loop

2004 ◽  
Vol 218 ◽  
pp. 81-82
Author(s):  
D. A. Leahy
Keyword(s):  
Supernova Remnants ◽  
The South ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved ◽  
Analysis Of The Images ◽  
The Right ◽  
Western Limb

The Cygnus Loop is one of the nearest supernova remnants (440 pc) and has been studied extensively in radio through X-ray wavelengths. An unusual bright “V”-shaped region on the south-western limb (near RA 20h46m and Decl. +30°) was revealed in ROSAT PSPC observations of the Cygnus Loop. The left side of the “V” has one of the highest hardness ratios (0.9–2 keV / 0.1–0.4 keV) in the Cygnus Loop whereas the right side has one of the lowest. Images and spatially resolved spectra were obtained using Chandra ACIS observations. Some results of analysis of the images and spectra are presented here.

scholarly journals Chandra Studies of Supernova Remnants and Pulsars

2001 ◽  
Vol 205 ◽  
pp. 358-365
Author(s):  
Patrick Slane ◽  
John P. Hughes ◽  
Cara E. Rakowski ◽  
David N. Burrows ◽  
John A. Nousek ◽  
...  
Keyword(s):  
Time Resolution ◽  
Supernova Remnants ◽  
Angular Resolution ◽  
Fast Time ◽  
X Ray ◽  
Spatially Resolved ◽  
Unique Capability

With sub-arcsecond angular resolution accompanied by fast time resolution and spatially resolved spectral capabilities, the Chandra X-ray Observatory provides a unique capability for the study of supernova remnants (SNRs) and pulsars. Though in its relative infancy, Chandra has already returned stunning images of SNRs which reveal the distribution of ejecta synthesized in the stellar explosions, the distinct properties of the forward and reverse shocks, and the presence of faint shells surrounding compact remnants. Pulsar observations have uncovered jet features as well as small-scaled structures in synchrotron nebulae. In this brief review we discuss results from early Chandra studies of pulsars and SNRs.

scholarly journals High Resolution X-ray Spectra of Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 205-211
Author(s):  
C. R. Canizares ◽  
P. F. Winkler ◽  
T. H. Markert ◽  
C. Berg
Keyword(s):  
Supernova Remnants ◽  
Abundance Ratio ◽  
Ionization Equilibrium ◽  
X Ray ◽  
Cygnus Loop ◽  
Doppler Shifts ◽  
Wide Range ◽  
Cas A ◽  
Einstein Observatory ◽  
Tycho’S Snr

We review results obtained with the Focal Plane Crystal Spectrometer (FPCS) on the Einstein Observatory. Clear evidence is found for departures from ionization equilibrium in the interior of Puppis A. This comes from the observed weakness of the forbidden lines relative to the resonance lines for the He - like triplets of O VII and Ne IX. However, it is shown that this departure from equilibrium does not alter our conclusion, based on previous FPCS results, that O and Ne are overabundant relative to Fe. The spectrum of N132D shows strong O VIII emission and very weak Fe emission, suggesting an even greater O/Fe abundance enhancement than in Puppis A. In the Cygnus Loop, the O to Ne abundance ratio is approximately solar; we have no information about Fe. The O VII triplet shows clear evidence for departures from ionization equilibrium in the Cygnus Loop. The spectrum of Tycho's SNR contains lines from ionization stages of Fe XVII through Fe XXIII and XXIV, indicating that a wide range of ionization conditions are present. Cas A and Kepler's SNR show relatively less emission from the higher ionization stages. For Tycho, we measured the strength of the strong Si XIII lines, and we find that a many-fold overabundance of Si relative to Fe is required regardless of the equilibrium state of the emitting plasma (confirming the Solid State Spectrometer results). On a separate topic, the completed analysis of X-ray Doppler shifts in Cas A suggests that the emitting material is concentrated in a ring that is inclined to the line of sight and is expanding at ~5000 km s−1.

scholarly journals Detailed X-ray Observations of the Cygnus Loop

1983 ◽  
Vol 101 ◽  
pp. 253-260
Author(s):  
W. H.-M. Ku ◽  
K. Long ◽  
R. Pisarski ◽  
M. Vartanian
Keyword(s):  
High Resolution ◽  
Proportional Counter ◽  
Supernova Remnant ◽  
Sounding Rocket ◽  
Loop Structure ◽  
High Quality ◽  
Radio Structure ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved

High quality X-ray spectral and imaging observations of the Cygnus Loop have been obtained with three different instruments. The High Resolution Imager (HRI) on the Einstein Observatory was used to obtain arcsecond resolution images of select bright regions in the Cygnus Loop which permit detailed comparisons between the X-ray, optical, and radio structure of the Loop. The Imaging Proportional Counter (IPC) on the Einstein Observatory was used to obtain an arcminute resolution map of essentially the full Loop structure. Finally, an Imaging Gas Scintillation Proportional Counter (IGSPC), carried aloft by a sounding rocket last fall, obtained modest resolution, spatially resolved spectrophotometry of the Cygnus Loop. An X-ray map of the Loop in the energy of the 0 VIII line was obtained. These data combine to yield a very powerful probe of the abundance, temperature, and density distribution of material in the supernova remnant, and in the interstellar medium.

scholarly journals X-ray spectral variations over the Cygnus Loop and Puppis A supernova remnants

1980 ◽  
Vol 191 (4) ◽  
pp. 729-737 ◽  
Author(s):  
M. A. Kayat ◽  
D. P. Rolf ◽  
G. C. Smith ◽  
R. Willingale
Keyword(s):  
Supernova Remnants ◽  
X Ray ◽  
Cygnus Loop

scholarly journals Shell Shock and Cloud Shock: Results from Spatially Resolved X‐Ray Spectroscopy withChandrain the Cygnus Loop

2002 ◽  
Vol 576 (2) ◽  
pp. 798-805 ◽  
Author(s):  
N. A. Levenson ◽  
James R. Graham ◽  
Julie L. Walters
Keyword(s):  
Shell Shock ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved

scholarly journals New Results on Supernova Remnants

1974 ◽  
Vol 60 ◽  
pp. 373-374 ◽  
Author(s):  
I. S. Shklovskii
Keyword(s):  
Supernova Remnants ◽  
X Ray ◽  
Cygnus Loop ◽  
Supernova Explosions ◽  
The Masses

Estimates of the masses and energies of the supernova explosions that resulted in the Cygnus Loop and similar remnants are revised downward on the basis of recent soft X-ray observations.

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 Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant

2018 ◽  
Vol 618 ◽  
pp. A155 ◽  
Author(s):  
Iurii Sushch ◽  
Robert Brose ◽  
Martin Pohl
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Supernova Remnants ◽  
High Energy ◽  
Radial Dependence ◽  
Electromagnetic Spectrum ◽  
X Ray ◽  
Spatially Resolved ◽  
Magnetic Field Profile ◽  
Broadband Emission

Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source, making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution one-dimensional (1D) hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field, which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.

Studies of the X-ray emission from supernova remnants

1974 ◽  
Vol 340 (1623) ◽  
pp. 423-437
Keyword(s):  
Supernova Remnants ◽  
Column Density ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Lower Intensity ◽  
X Ray ◽  
Cassiopeia A ◽  
Cygnus Loop ◽  
A Value ◽  
The Crab Nebula

Supernova remnants are now recognized as a class of soft X-ray emitting-objects. The evolution of a remnant’s X-ray emission is discussed and a number of possible X-ray emission mechanisms are described. The spectrum of the Crab Nebula has been studied with Copernicus. The data have been used to derive a value of the gas column density of the interstellar medium. The X-ray structure and spectrum of the remnant Cassiopeia. A have been investigated and the results are presented. A high resolution X-ray map of the Puppis A supernova remnant has been obtained and the interpretation of the X-ray structure is discussed. X-ray emission has been detected from the pulsar PSR 08 33-45. This observation is compared with data obtained from the Uhuru satellite in order to derive the gas column density to the source. Weak soft X-ray emission has been detected from the Cygnus Loop in the regions expected but a t a lower intensity – a search for regions of higher intensity is continuing. A programme to identify known radio remnants as X-ray emitters is in progress and the results obtained so far are reported.

scholarly journals G107.0+9.0: a new large optically bright, radio, and X-Ray faint galactic supernova remnant in Cepheus

2020 ◽  
Vol 498 (4) ◽  
pp. 5194-5206 ◽  
Author(s):  
Robert A Fesen ◽  
Kathryn E Weil ◽  
John C Raymond ◽  
Laurent Huet ◽  
Martin Rusterholz ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Galactic Plane ◽  
Line Emission ◽  
Wide Field ◽  
X Ray ◽  
Spatially Resolved ◽  
Sky Survey ◽  
Line Survey ◽  
Low Dispersion ◽  
Western Limb

ABSTRACT Wide-field H α images of the Galactic plane have revealed a new supernova remnant (SNR) nearly 3 deg in diameter centred at l = 107.0, b = +9.0. Deep and higher resolution H α and [O iii] 5007 Å images show dozens of H α filaments along the remnant’s northern, western, and southwestern limbs, but few [O iii] bright filaments. The nebula is well detected in the H α Virginia Tech Spectral-Line Survey images, with many of its brighter filaments even visible on Digital Sky Survey images. Low-dispersion spectra of several filaments show either Balmer dominated, non-radiative filaments, or the more common SNR radiative filaments with [S II]/H α ratios above 0.5, consistent with shock-heated line emission. Emission line ratios suggest shock velocities ranging from ≤70 km s−1 along its western limb to ≃ 100 km s−1 along its northwestern boundary. While no associated X-ray emission is seen in ROSAT images, faint 1420 MHz radio emission appears coincident with its western and northern limbs. Based on an analysis of the remnant’s spatially resolved H α and [O iii] emissions, we estimate the remnant’s distance at ∼1.5−2.0 kpc implying a physically large (dia. = 75−100 pc) and old (90−110 × 103 yr) SNR in its post-Sedov radiative phase of evolution expanding into a low-density interstellar medium (n0 = 0.05−0.2 cm−3) and lying some 250−300 pc above the Galactic plane.

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