A Continuous Injection Model for the Supernova Remnants Cassiopeia a and the Crab Nebula

1976 ◽  
Vol 210 ◽  
pp. 723 ◽  
Author(s):  
F. W. Peterson
Keyword(s):  
Supernova Remnants ◽  
Crab Nebula ◽  
Cassiopeia A ◽  
Injection Model ◽  
The Crab Nebula ◽  
Continuous Injection

scholarly journals The Secular Behavior of X-Ray and Radio Emission from Supernova Remnants

1971 ◽  
Vol 46 ◽  
pp. 268-272
Author(s):  
Wallace H. Tucker
Keyword(s):  
Radio Emission ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
X Ray ◽  
Cas A ◽  
The Crab Nebula ◽  
Continuous Injection

Continuous injection models for the secular behavior of the radio and X-ray emission from supernova remnants are examined and compared with the observations. Among other things, it is concluded that (1) continuous injection probably occurs for at least 10 yr in every case and about 1000 yr in most supernova remnants, in which case the supernova remnants 3C392, W28, Pup A and IC443 should produce 1–10 keV X-ray fluxes ≈ 10-10 ergs/cm2-sec, and (2) the X-ray sources in the Crab Nebula, Cas A and Tycho can be explained in terms of a model wherein continuous injection occurs for 300 yr for the Crab Nebula, much less than 250 yr for Cas A and much longer than 400 yr for Tycho. Finally, it is shown that if Tycho and Cas A contain an X-ray star such as NP 0532, it is quite possible that the X-ray emission from those sources is predominantly due to the X-ray star.

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 Nonstationary Phenomena in the Radiation of Young Supernova Remnants

1987 ◽  
Vol 40 (6) ◽  
pp. 801 ◽  
Author(s):  
VP Ivanov ◽  
KS Stankevich
Keyword(s):  
Radio Emission ◽  
Flux Density ◽  
Spectral Index ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Adiabatic Expansion ◽  
Cassiopeia A ◽  
Average Decrease ◽  
Tycho Brahe ◽  
The Crab Nebula

The time variation of the radio emission from the supernova remnants Cassiopeia A, the Crab Nebula and Tycho Brahe (SN 1572) is investigated. There is a frequency dependence on the rate of decrease in the flux density of Cassiopeia A for the period 1957 to 1984. The (positive) spectral index has a secular decrease and also, for frequencies above 320 MHz, slight oscillations with a six-year period. The radio emission from the Crab Nebula was constant from 1953 to 1975 but has since decreased accompanied by a change in spectral index. The average decrease of the flux density of SN 1572 from 1963 to 1983 was 0�52% per year, close to the value predicted for adiabatic expansion.

scholarly journals Supernova Remnants Resembling the Crab Nebula

1983 ◽  
Vol 101 ◽  
pp. 299-320 ◽  
Author(s):  
K. W. Weiler
Keyword(s):  
Large Class ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Origin And Evolution ◽  
Class C ◽  
The Individual ◽  
The Crab Nebula

While reviewing and systematizing the properties of the class of supernova remnants resembling the Crab Nebula it has been found that supernova remnants can be split into three morphological groups – Class S (shells), Class P (plerions), and Class C (combinations) – where the Class C objects appear to represent a new and especially interesting classification. In this overview, the identifying properties of all three classes are defined. Because the large Class S has been studied in detail many times previously, it is not discussed further here. For the smaller Classes P and C, the individual members and suspected members are presented and their properties reviewed. Finally, an origin and evolution for each class is suggested.

scholarly journals Physical Processes and Parameters in the Magnetosphere of NP 0532

1971 ◽  
Vol 46 ◽  
pp. 394-406
Author(s):  
F. Pacini
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
General Relation ◽  
Energy Generation ◽  
Main Pulse ◽  
Physical Processes ◽  
X Ray ◽  
The Crab Nebula

The Crab Nebula pulsar conforms to the model of a rotating magnetised neutron star in the rate of energy generation and the exponent of the rotation law.It is suggested that the main pulse is due to electrons and the precursor to protons. Both must radiate in coherent bunches. Optical and X-ray radiation is by the synchrotron process.The wisps observed in the Nebula may represent the release of an instability storing about 1043 erg and 1047–48 particles.Finally, some considerations are made about the general relation between supernova remnants and rotating neutron stars.

scholarly journals The Galactic Sources G5.4-1.2 and G5.27-0.90

1987 ◽  
Vol 125 ◽  
pp. 129-129
Author(s):  
J.L. Caswell ◽  
M.J. Kesteven ◽  
R.F. Haynes ◽  
D.K. Milne ◽  
M.M. Komesaroff ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Stellar Core ◽  
Galactic Sources ◽  
The Crab Nebula

Long after a supernova event, the stellar core (neutron star) may continue to excite an extended remnant of ejecta surrounding it, as in the case of the Crab nebula. In contrast, the more common shell supernova remnants (SNRs) appear unaffected by any embedded neutron star.

scholarly journals Peculiar Differences in Radio and X-ray Synchrotron Radiation from Pulsar Wind Nebulae

2004 ◽  
Vol 218 ◽  
pp. 221-224
Author(s):  
John R. Dickel ◽  
Shiya Wang
Keyword(s):  
Synchrotron Radiation ◽  
Radio Emission ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Pulsar Wind Nebulae ◽  
X Ray ◽  
Pulsar Wind ◽  
The Crab Nebula

Several Crab-type supernova remnants appear to have very bright non-thermal X-ray cores just around the pulsar or expected pulsar. This X-ray brightness is often not matched by a corresponding increase in radio emission. The best example of this phenomenon is in N157B in the LMC. G21.5−0.9 and possibly 3C 58 also show it while the Crab Nebula and 0540−69.3 do not. Some method to enhance the higher energy particles must be present in these objects.

scholarly journals The Interstellar Environment of Filled‐Center Supernova Remnants. III. The Crab Nebula

1999 ◽  
Vol 124 (1) ◽  
pp. 181-193 ◽  
Author(s):  
B. J. Wallace ◽  
T. L. Landecker ◽  
P. M. W. Kalberla ◽  
A. R. Taylor
Keyword(s):  
Supernova Remnants ◽  
Crab Nebula ◽  
The Crab Nebula

scholarly journals Optical and UV Observations of Supernova Remnants

1996 ◽  
Vol 145 ◽  
pp. 381-389
Author(s):  
Robert A. Fesen
Keyword(s):  
Mass Loss ◽  
Proper Motion ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Circumstellar Disk ◽  
Mantle Material ◽  
Cygnus Loop ◽  
Cas A ◽  
The Crab Nebula

Recent observations of the galactic supernova remnants the Crab Nebula, SN 1006, Cas A, and the Cygnus Loop are reviewed. New studies of the Crab Nebula suggest its progenitor may have had appreciable mass loss in the form of a circumstellar disk resulting in both a bipolar expansion and formation of the synchrotron ‘bays'. Unusually high proper motion knots near to and possibly directed away from the pulsar also have been reported. In the Cas A remnant, a NE jet of ejecta appears to be a plume of mantle material with expansion velocities up to 12000 km s-1 or nearly twice that seen in the main ejecta shell. HST observations of the sdOB star located behind SN 1006 indicate symmetrically expanding Fe II ejecta out to 8100 km s-1. Lastly, deep images of the Cygnus Loop reveal emission structures similar to those seen in 2D & 3D shocked cloud simulations.

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