scholarly journals On the magnetohydrodynamic modelling of the Crab nebula radio emission

2014 ◽  
Vol 438 (2) ◽  
pp. 1518-1525 ◽  
Author(s):  
B. Olmi ◽  
L. Del Zanna ◽  
E. Amato ◽  
R. Bandiera ◽  
N. Bucciantini
Keyword(s):  
Radio Emission ◽  
Crab Nebula ◽  
The Crab Nebula

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.

A singularity in the radio emission spectrum of the Crab nebula in the decimeter wavelength range

1969 ◽  
Vol 12 (2) ◽  
pp. 134-138
Author(s):  
V. A. Alekseev ◽  
�. D. Gat�lyuk ◽  
D. A. Dmitrenko ◽  
A. A. Romanychev ◽  
N. M. Tseitlin
Keyword(s):  
Radio Emission ◽  
Emission Spectrum ◽  
Wavelength Range ◽  
Crab Nebula ◽  
The Crab Nebula

Monitoring of the radio emission of the Crab Nebula pulsar at low frequencies

2011 ◽  
Vol 55 (5) ◽  
pp. 416-424 ◽  
Author(s):  
A. D. Kuz’min ◽  
Yu. A. Belyatsky ◽  
D. V. Dumsky ◽  
V. A. Izvekova ◽  
K. A. Lapaev ◽  
...  
Keyword(s):  
Radio Emission ◽  
Crab Nebula ◽  
Low Frequencies ◽  
The Crab Nebula

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.

scholarly journals The radio sources in the Cygnus loop and IC443

1959 ◽  
Vol 9 ◽  
pp. 323-327 ◽  
Author(s):  
E. Margaret Burbidge ◽  
G. R. Burbidge
Keyword(s):  
Synchrotron Radiation ◽  
Radio Emission ◽  
Strong Evidence ◽  
Crab Nebula ◽  
Radio Sources ◽  
Cassiopeia A ◽  
Cygnus Loop ◽  
Physical Conditions ◽  
Nonthermal Radio ◽  
The Crab Nebula

Within our Galaxy there are a number of nonthermal sources of radio emission. In the last few years a considerable amount of data has been collected about some of these sources, in particular the Crab nebula and the Cassiopeia A source. There is strong evidence now to suggest that all of the nonthermal radio sources emit by synchrotron radiation, or acceleration radiation as we shall describe it here. In this paper we want to discuss the physical conditions in two objects, the Cygnus loop and IC 443.

scholarly journals Model of radio emission from spherically symmetric pulsar wind nebulae

2012 ◽  
Vol 8 (S291) ◽  
pp. 511-513
Author(s):  
Shuta J. Tanaka
Keyword(s):  
Radio Emission ◽  
Spatial Structure ◽  
Power Law ◽  
Crab Nebula ◽  
Particle Energy ◽  
Zone Model ◽  
Pulsar Wind Nebulae ◽  
Adiabatic Cooling ◽  
Pulsar Wind ◽  
The Crab Nebula

AbstractWe study radio emission from pulsar wind nebulae (PWNe) considering the observed spatial structure. We assume spherical symmetry of the PWN, and model the evolution of the magnetic field and the particle energy distribution. We do not consider the synchrotron cooling of particles but consider the adiabatic cooling, because we are mostly interested in the radio emission from PWNe. The model is applied to the Crab Nebula and succeeds to reproduce the observed spatially integrated spectrum in radio with a single power-law injection. In our previous work (a one-zone model), in contrast, the integrated spectrum of the Crab Nebula is reproduced by a broken power-law injection of particles. However, the spatial structure in radio is inconsistent with observations and we need a radial velocity profile which is very different from the model by Kennel & Coroniti. Further studies of the spatial structure of PWNe are important to understand the origin of the radio emission from young PWNe.

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