[ITAL]Chandra[/ITAL] Observation of Supernova Remnant G54.1+0.3: A Close Cousin of the Crab Nebula

2002 ◽  
Vol 568 (1) ◽  
pp. L49-L52 ◽  
Author(s):  
F. J. Lu ◽  
Q. D. Wang ◽  
B. Aschenbach ◽  
P. Durouchoux ◽  
L. M. Song
Keyword(s):  
Supernova Remnant ◽  
Crab Nebula ◽  
The Crab Nebula

DA 495 - an unusual supernova remnant with resemblances to the Crab nebula

1983 ◽  
Vol 88 ◽  
pp. 1810 ◽  
Author(s):  
T. L. Landecker ◽  
J. L. Caswell
Keyword(s):  
Supernova Remnant ◽  
Crab Nebula ◽  
The Crab Nebula

scholarly journals Investigations of Recently Discovered Supernova Remnants’ Spectral Plot: AT2019fya, SN2019fjp, SN2019fcc, SN2019fbv, SN2019ffi, and SN2019fce

2020 ◽  
Vol 84 ◽  
pp. 1-9
Author(s):  
Bjorn Jasper R. Raquel ◽  
Agnes C. Bantaculo ◽  
Shane Carlo B. Llemit ◽  
Eldrin P. Custodio
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Type Ii ◽  
Plot Analysis ◽  
The Individual ◽  
The Crab Nebula

This paper presents the spectroscopic graphs of recently discovered Supernova Remnants (AT2019fya, SN2019fjp, SN2019fcc, SN2019fce, SN2019fbv & SN2019ffi) for the determination of elements present. The researchers use the spectral plot analysis to analyze the presence of certain elements of the individual supernova remnants (SNR) for the assimilation, differentiation and classification of these SNR. Redshift and velocities of these SNR were also found using the observed wavelength and the rest wavelength ratio. Comparison suggests that AT2019fya is a Type II supernova remnant and some of the SNRs in this study exhibits an existence of krypton (Kr) on their composition which is recently discovered by M. Barlow (2013) to be present at the Crab Nebula. This might suggest that AT2019fya, SN2019fbv, SN2019fce, and SN2019ffi have a pulsar at their center.

scholarly journals VLA Observations of Sgr A

1983 ◽  
Vol 101 ◽  
pp. 65-69
Author(s):  
W. M. Goss ◽  
U. J. Schwarz ◽  
R. D. Ekers ◽  
J. H. van Gorkom
Keyword(s):  
Surface Brightness ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Galactic Centre ◽  
Thermal Source ◽  
Very Large Array ◽  
Sgr A ◽  
Cas A ◽  
Relationship Of ◽  
The Crab Nebula

The radio source Sgr A has been mapped with the Very Large Array (VLA) at 6 and 20 cm with an angular resolution of 5″ x 8″ arc. In agreement with the earlier “WORST” map, the non-thermal source Sgr A East shows a shell structure, while the thermal source Sgr A West shows a spiral-like morphology. We suggest that Sgr A East is a supernova remnant (SNR) near the galactic centre. Its surface brightness is the third largest in our galaxy after Cas A and the Crab Nebula. The diameter is 9 pc and the source fits the surface-brightness diameter relationship of Clark and Caswell (1976) if a distance of 10 kpc is assumed.

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 A Newly-Recognised Galactic Supernova Remnant with Shell-Type and Filled-Centre Features

1988 ◽  
Vol 101 ◽  
pp. 347-350
Author(s):  
Peter J. Barnes ◽  
A.J. Turtle
Keyword(s):  
Spectral Index ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Dual Nature ◽  
Valuable Addition ◽  
Shell Type ◽  
The Crab Nebula ◽  
Galactic Object

While the number of galactic supernova remnants (SNRs) now known is fairly large (>150), the subset among these that are known to resemble the Crab Nebula is still distressingly small, about 15 or so (Green, 1984). Thus any object that can be unambiguously included in this exclusive club forms a valuable addition to our knowledge of this class. We report here observations of a newly recognised nonthermal galactic object, G18.94-l.06, having all the hallmarks of the classical shell-type SNRs, while also appearing to have a filled-centre component located inside the shell. Among the known Crab-like remnants, about one third show this dual nature (Green, 1984). This diagnosis of G18.94-1.06 is supported mainly by the variations in spectral index α (Sν∝ να) across the source, as seen between the two observation frequencies, 408 MHz and 5.0 GHz.

scholarly journals The Spectral Turnover of the “Filled-Center” Supernova Remnant 3C 58: Implications for When Acceleration Occurs

1994 ◽  
Vol 142 ◽  
pp. 817-821
Author(s):  
D. A. Green
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Injection Rate ◽  
Power Law Distribution ◽  
Radiation Mechanisms ◽  
Particle Injection ◽  
The Past ◽  
Upper Limits ◽  
The Crab Nebula

AbstractIRASobservations the “filled-center” supernova remnant 3C 58 are used to derived upper limits of 0.4, 0.4, 0.8, and 1.5 Jy for its infrared flux density at 12, 25, 60, and 100 μm, respectively. These values imply a break in the spectrum of 3C58 above a few tens of gigahertz—two orders of magnitude below the break in the spectrum of the Crab Nebula—with a change of spectral index across the break for 3C 58 of more than 0.5. This is similar to previous results for another “filled-center” remnant, G74.9+1.2, from radio observations alone. This implies that their emission isnotdominated by a constant injection rate of particles with a power-law distribution. Either the break is due to synchrotron losses in the past, with little particle injection in recent times or it is intrinsic to the acceleration mechanism at work (presumably from a central neutron star).Subject headings: acceleration of particles — ISM: individual (3C 58) — radiation mechanisms: nonthermal — supernova remnants

scholarly journals Guest Stars: Historical Supernovae and Remnants

1987 ◽  
Vol 91 ◽  
pp. 265-270
Author(s):  
T. Velusamy
Keyword(s):  
Supernova Remnant ◽  
Crab Nebula ◽  
Electromagnetic Spectrum ◽  
Outer Envelope ◽  
Naked Eye ◽  
The Galaxy ◽  
Supernova Explosions ◽  
Ancient Times ◽  
Γ Rays ◽  
The Crab Nebula

Supernova explosions occur in massive stars in their final stages of stellar evolution. The explosion leaves behind a collapsed object, usually a neutron star observable as a pulsar, and an expanding outer envelope of the star observable as a supernova remnant (SNR). Because of the large amount of energy in the range of 1050 −1052 ergs released in the explosion, the energy radiated by the exploded star is equivalent to that of millions of normal stars. Thus a "new star" seems to appear and is easily visible to the naked eye for several months. Astronomers have estimated that in our galaxy such supernova explosions occur once about every 50 years. In ancient times, the occurrence of supernova might have been noticed as appearance of a bright new star which faded away into obscruity after a few months. Thus the ‘guest stars’ in the ancient records are indeed possible occurrences of supernova explosions in the galaxy. The guest star of 1054 A.D., well recorded by Chinese and Japanese astronomers is the best known historic supernova (Brecher et al. 1983; and references therein); today its remnants the Crab Nebula and the pulsar are observable over the entire electromagnetic spectrum from radio to γ-rays. Of the 150 SNRs known in our galaxy, only about 10 have been identified with guest stars of historical supernovae.

Observation of Polarization for the Crab Nebula with PHENEX Polarimeter

2010 ◽  
Vol 8 (ists27) ◽  
pp. Tm_35-Tm_40 ◽  
Author(s):  
Yuji KISHIMOTO ◽  
Shuichi GUNJI ◽  
Yushi ISHIKAWA ◽  
Makoto TAKADA ◽  
Tatehiro MIHARA ◽  
...  
Keyword(s):  
Crab Nebula ◽  
The Crab Nebula
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