scholarly journals Soft X-Ray Observations of Supernova Remnants

1974 ◽  
Vol 3 ◽  
pp. 565-572
Author(s):  
J. C. Zarnecki ◽  
J. L. Culhane ◽  
A. C. Fabian ◽  
C. G. Rapley ◽  
R.L.F. Boyd ◽  
...  
Keyword(s):  
Satellite Data ◽  
Supernova Remnants ◽  
Low Energy ◽  
X Ray ◽  
Cassiopeia A ◽  
Upper Limits

AbstractObservations of a number of supernova remnants have been carried out with the low energy X-ray telescope on the Copernicus satellite. Data are presented on the X-ray structure of the remnants Cassiopeia A and Puppis-A. Marginal detections or new upper limits are reported for the remnants IC443, DR4, MSH15-52A, Downes 83, Downes 84 and 3C392.

Study of Delayed States in 94Nb, 108Ag, and 110Ag

1971 ◽  
Vol 49 (6) ◽  
pp. 747-755 ◽  
Author(s):  
S. C. Gujrathi ◽  
J. M. d'Auria ◽  
R. G. Korteling
Keyword(s):  
High Resolution ◽  
Level Scheme ◽  
Half Life ◽  
Gamma Transition ◽  
Low Energy ◽  
X Ray ◽  
Upper Limits ◽  
Energy Gamma ◽  
Gamma Transitions ◽  
First Time

The lifetimes and energies associated with low-energy gamma transitions from the 93Nb(n,γ)94Nb, 107Ag(n,γ)108Ag, and 109Ag(n,γ)110Ag reactions have been studied using a high-resolution Ge(Li) X-ray spectrometer. New weak transitions are observed in the decay of 110Ag at 30.84, 38.19, 41.78, and 136.65 keV, while intense gamma transitions at 105.6, 235.8, and 266.95 keV are resolved into doublets. The half-life of the state involving the intense 117.47 keV transition in 110Ag and the 215 keV transition in 108Ag is confirmed as 36.5 ± 2.0 ns and 54 ± 8 ns, respectively, while a new delayed state associated with the gamma transition of 99.404 keV (T1/2 = 30 ± 5 ns) in 94Nb is observed for the first time. The upper limits for the half-lives involving most of the intense transitions in all the three isotopes are also reported. A level scheme is proposed and discussed for 108Ag.

X-ray spectra of the Cassiopeia A and TYCHO supernova remnants and their element abundances

1986 ◽  
Vol 306 ◽  
pp. 248 ◽  
Author(s):  
H. Tsunemi ◽  
K. Yamashita ◽  
K. Masai ◽  
S. Hayakawa ◽  
K. Koyama
Keyword(s):  
Supernova Remnants ◽  
X Ray ◽  
Cassiopeia A ◽  
Element Abundances

scholarly journals The X-ray structure of supernova remnants - I. Cassiopeia A

1977 ◽  
Vol 178 (3) ◽  
pp. 307-323 ◽  
Author(s):  
P. A. Charles ◽  
J. L. Culhane ◽  
A. C. Fabian
Keyword(s):  
Supernova Remnants ◽  
X Ray ◽  
Cassiopeia A

scholarly journals Deep XMM-Newton observations of the northern disc of M 31

2018 ◽  
Vol 620 ◽  
pp. A28 ◽  
Author(s):  
Manami Sasaki ◽  
Frank Haberl ◽  
Martin Henze ◽  
Sara Saeedi ◽  
Benjamin F. Williams ◽  
...  
Keyword(s):  
Spectral Properties ◽  
Supernova Remnants ◽  
X Ray ◽  
Star Forming ◽  
Transient Source ◽  
Upper Limits ◽  
Low Mass ◽  
Higher Temperature ◽  
M 31 ◽  
X Ray Binaries

Context. We carried out new observations of two fields in the star-forming northern ring of M 31 with XMM-Newton with each one of them consisting of two exposures of about 100 ks each. A previous XMM-Newton survey of the entire M 31 galaxy revealed extended diffuse X-ray emission in these regions. Aims. We study the population of X-ray sources in the northern disc of M 31 by compiling a complete list of X-ray sources down to a sensitivity limit of ∼7 × 1034 erg s−1 (0.5–2.0 keV) and improve the identification of the X-ray sources. The major objective of the observing programme was the study of the hot phase of the interstellar medium (ISM) in M 31. The analysis of the diffuse emission and the study of the ISM is presented in a separate paper. Methods. We analysed the spectral properties of all detected sources using hardness ratios and spectra if the statistics were high enough. We also checked for variability. In order to classify the sources detected in the new deep XMM-Newton observations, we cross-correlated the source list with the source catalogue of a new survey of the northern disc of M 31 carried out with the Chandra X-ray Observatory and the Hubble Space Telescope (Panchromatic Hubble Andromeda Treasury, PHAT) as well as with other existing catalogues. Results. We detected a total of 389 sources in the two fields of the northern disc of M 31 observed with XMM-Newton. We identified 43 foreground stars and candidates and 50 background sources. Based on a comparison with the results of the Chandra/PHAT survey, we classify 24 hard X-ray sources as new candidates for X-ray binaries. In total, we identified 34 X-ray binaries and candidates and 18 supernova remnants (SNRs) and candidates. We studied the spectral properties of the four brightest SNRs and confirmed five new X-ray SNRs. Three of the four SNRs, for which a spectral analysis was performed, show emission mainly below 2 keV, which is consistent with shocked ISM. The spectra of two of them also require an additional component with a higher temperature. The SNR [SPH11] 1535 has a harder spectrum and might suggest that there is a pulsar-wind nebula inside the SNR. For all SNRs in the observed fields, we measured the X-ray flux or calculated upper limits. We also carried out short-term and long-term variability studies of the X-ray sources and found five new sources showing clear variability. In addition, we studied the spectral properties of the transient source SWIFT J004420.1+413702, which shows significant variation in flux over a period of seven months (June 2015 to January 2016) and associated change in absorption. Based on the likely optical counterpart detected in the Chandra/PHAT survey, the source is classified as a low-mass X-ray binary.

scholarly journals X-Radiation from Supernova Remnants

1973 ◽  
Vol 55 ◽  
pp. 105-117
Author(s):  
K. A. Pounds
Keyword(s):  
Supernova Remnants ◽  
Crab Nebula ◽  
Low Energy ◽  
Radiation Mechanism ◽  
X Ray ◽  
The Crab Nebula

Available X-ray observations of supernova remnants are reviewed. The number of SNR seen above 2 keV remains small after inclusion of the UHURU results and for only the Crab Nebula is the data adequate to clearly indicate the radiation mechanism. The increasing importance of low energy X-ray studies (below 1 keV) of older and relatively nearby remnants is noted. Brief discussion is given of the relation of the X-ray data to current ideas of the evolution of SNR.

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 The Evolution of Young Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 119-124
Author(s):  
A. C. Fabian ◽  
W. Brinkmann ◽  
G. C. Stewart
Keyword(s):  
Density Distribution ◽  
Stellar Wind ◽  
Supernova Remnants ◽  
Initial Conditions ◽  
Numerical Models ◽  
Variable Mass ◽  
Initial Density ◽  
X Ray ◽  
Cassiopeia A ◽  
Initial Density Distribution

Einstein X-ray observations of the young supernova remnants Cassiopeia A (Murray et al. 1980) and Tycho (Seward, Gorenstein and Tucker 1982) indicate that the swept-up mass does not much exceed that of the observed ejecta. The initial density distribution of the ejecta and surrounding material is then important in determining the X-ray structure and evolution. Some aspects of this behaviour have been dealt with in previous numerical (e.g. Gull 1973; Itoh 1977; Jones, Smith and Straka 1981) and analytical (e.g. Chevalier 1982a,b) studies. We present here results obtained from numerical models covering a wider range of initial conditions. In particular, we consider the effect of a constant stellar wind from the progenitor star on the expansion of the remnant. We have previously suggested that variable mass loss from SN1006 may explain its warm filled interior (Fabian, Stewart and Brinkmann 1982).

scholarly journals Stellar binaries that survive supernovae

2019 ◽  
Vol 485 (4) ◽  
pp. 5394-5410 ◽  
Author(s):  
C S Kochanek ◽  
K Auchettl ◽  
K Belczynski
Keyword(s):  
Supernova Remnants ◽  
Reasonable Agreement ◽  
Main Sequence ◽  
High Mass ◽  
Core Collapse ◽  
Population Synthesis ◽  
X Ray ◽  
Upper Limits ◽  
Model Finding ◽  
X Ray Binaries

Abstract The number of binaries containing black holes (BH) or neutron stars (NS) depends critically on the fraction of binaries that survive supernova (SN) explosions. We searched for surviving star plus remnant binaries in a sample of 49 supernova remnants (SNR) containing 23 previously identified compact remnants and three high-mass X-ray binaries (HMXB), finding no new interacting or non-interacting binaries. The upper limits on any main-sequence stellar companion are typically $\lesssim 0.2\, \mathrm{M}_\odot$ and are at worst $\lesssim 3\, \mathrm{M}_\odot$. This implies that f < 0.1 of core-collapse SNRs contain a non-interacting binary, and f = 0.083 (0.032 < f < 0.17) contain an interacting binary at 90 per cent confidence. We also find that the transverse velocities of HMXBs are low, with a median of only 12 km s−1 for field HMXBs, so surviving binaries will generally be found very close to the explosion centre. We compare the results to a ‘standard’ StarTrack binary population synthesis (BPS) model, finding reasonable agreement with the observations. In particular, the BPS models predict that 6 per cent of initial binaries leave a star plus remnant binary, or 5 per cent of SNRs assuming an 84 per cent binary fraction.

scholarly journals Hard Cosmic X-Ray Sources

1973 ◽  
Vol 55 ◽  
pp. 51-73 ◽  
Author(s):  
L. E. Peterson
Keyword(s):  
Supernova Remnants ◽  
Galactic Center ◽  
Galactic Plane ◽  
Crab Nebula ◽  
X Rays ◽  
X Ray ◽  
Sky Survey ◽  
Upper Limits ◽  
Observational Status ◽  
The Crab Nebula

A review of the observational status of X-ray sources detected in the 20 ⋍ 500 keV range is presented. Of the approximately 115 sources listed in the March 1972 edition of the UHURU 2–6 keV sky survey catalog, about 15 sources have been studied in hard X-rays. Most of the data have been obtained from balloons, although the OSO-3, and more recently the OSO-7, have contributed. With the exception of CEN A, the SMC, and possibly M-87, all the sources detected at higher energies are galactic and heavily concentrated in the galactic plane. The Crab Nebula has been measured to about 500 keV in continuous emission and a component at the ⋍ 33 ms pulsar period comprising about 20% of the total emission has been detected to ∼10 MeV. Objects such as SCO-1 and CYG-2 are characterized by an exponential spectrum, which varies over a 10 min. time scale about a factor of two, and a flatter spectrum extending to above 40 keV which exhibits independent variability. Objects such as CYG-1 and possibly CYG-3 have a multi-component power law spectrum extending to over 100 keV, and may vary many factors over a period of weeks. Other sources generally not yet identified with optical or radio candidates, located in the Galactic Center and the Centaurus/Crux region also show considerable variability, and in one case may have been detected to nearly 500 keV. Only upper limits at about 2 × 10−4 photon (cm2 s keV)−1 in the 20–50 keV range exist for most supernova remnants and extragalactic sources.

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