High Resolution X-ray Observations of 3C 58

As the presumed remnant of SN 1181, 3C 58 houses one of the youngest known neutron stars in the Galaxy. The properties of this young pulsar and its associated pulsar wind nebula (PWN) differ considerably from those of the Crab Nebula, and may well offer a more typical example of the endpoint of massive star collapse. High resolution X-ray studies reveal structures in the inner nebula that may be associated with the pulsar wind termination shock, a jet that may be aligned with the rotation axis, and other regions of enhanced emission. Spectral variations in the PWN are consistent with the expected evolution of the postshock flow, and complex loops of emission are seen in the nebula interior. Limits on the neutron star surface temperature fall below standard cooling models, indicating that some more rapid neutrino cooling process is required. The outer regions of 3C 58 show thermal emission with enhanced levels of neon, indicative of shocked ejecta bounding the PWN.

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Year-scale Morphological Variation of the X-ray Crab Nebula

Symposium - International Astronomical Union ◽

10.1017/s007418090018091x ◽

2004 ◽

Vol 218 ◽

pp. 181-184 ◽

Cited By ~ 4

Author(s):

Koji Mori ◽

David N. Burrows ◽

George G. Pavlov ◽

J. Jeff Hester ◽

Shinpei Shibata ◽

...

Keyword(s):

Morphological Variation ◽

Crab Nebula ◽

The Other ◽

X Ray ◽

Morphological Variations ◽

Other Hand ◽

Pulsar Wind ◽

Circular Structures ◽

The Crab Nebula

We present year-scale morphological variations of the Crab Nebula revealed by the Chandra X-ray Observatory. Observations have been performed about every 1.7 years over the three years from launch. The variations are clearly recognized at two sites: the torus and the southern jet. The torus, which had been steadily expanding until 1.7 years ago, now appears to have shrunk in the latest observation. Additionally, the circular structures seen to the northeast of the torus have decayed into several arcs. On the other hand, the southern jet shows the growth of its overall kinked-structure. We discuss the nature of these variations in terms of the pulsar wind nebula mechanism.

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

Symposium - International Astronomical Union ◽

10.1017/s0074180900181033 ◽

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.

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High energy cosmic photons and neutrinos

Symposium - International Astronomical Union ◽

10.1017/s0074180900179628 ◽

1965 ◽

Vol 23 ◽

pp. 195-225

Author(s):

R. J. Gould ◽

G. R. Burbidge

Keyword(s):

Supernova Remnants ◽

Crab Nebula ◽

Meson Production ◽

Cosmic Ray ◽

High Energy ◽

Relativistic Electrons ◽

X Ray ◽

Hard Radiation ◽

The Galaxy ◽

The Crab Nebula

This review concentrates primarily on the problem of interpreting the recent X-ray and γ-ray observations of celestial sources. The expected fluxes of hard radiation from various processes are estimated (when possible) and are compared with the observations. We compute the synchrotron, bremsstrahlung, and (inverse) Compton spectra originating from relativistic electrons produced (via meson production) in the galaxy and intergalactic medium by cosmic ray nuclear collisions; the spectra from π°-decay are also computed. Neutron stars, stellar coronae, and supernova remnants are reviewed as possible X-ray sources. Special consideration is given to the processes in the Crab Nebula. Extragalactic objects as discrete sources of energetic photons are considered on the basis of energy requirements; special emphasis is given to the strong radio sources and the possibility of the emission of hard radiation during their formation. The problem of the detection of cosmic neutrinos is reviewed.As yet, no definite process can be identified with any of the observed fluxes of hard radiation, although a number of relevant conclusions can be drawn on the basis of the available preliminary observational results. In particular, some cosmogonical theories can be tested.

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CONSTRAINING THE PULSAR POWER IN GAMMA-RAY BINARIES THROUGH THERMAL X-RAY EMISSION

International Journal of Modern Physics Conference Series ◽

10.1142/s2010194512004515 ◽

2012 ◽

Vol 08 ◽

pp. 132-137

Author(s):

VÍCTOR ZABALZA ◽

VALENTÍ BOSCH-RAMON ◽

JOSEP MARIA PAREDES

Keyword(s):

Stellar Wind ◽

Binary Systems ◽

Massive Star ◽

Gamma Ray ◽

Thermal Emission ◽

Mass Loss Rate ◽

X Rays ◽

Orbital Inclination ◽

X Ray ◽

Pulsar Wind

Gamma-ray binaries are binary systems that show non-thermal broadband emission from radio to gamma rays. If the system comprises a massive star and a young non-accreting pulsar, their winds collide producing non-thermal emission, most likely from the shocked pulsar wind. Thermal X-rays are expected from the shocked stellar wind, with a spectrum akin to the one observed in massive star binaries. The goal of this work is, through the study of the thermal X-ray emission from the shocked stellar wind in pulsar gamma-ray binaries, constrain the pulsar spin-down luminosity and the stellar wind properties. A semi-analytic model is developed to compute the thermal X-ray emission from the shocked stellar wind in pulsar gamma-ray binaries. The model results are compared with XMM-Newton observations of LS 5039, a candidate pulsar gamma-ray binary with a strong stellar wind. Exploring the range of possible values for the stellar mass-loss rate and orbital inclination, we obtain an upper limit on the pulsar spin-down luminosity of 6 × 1036 erg s-1. We conclude that, to explain the non-thermal luminosity of LS 5039 in the pulsar wind scenario, a non-thermal to spin-down luminosity ratio very close to unity may be required.

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ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab2506 ◽

2021 ◽

Author(s):

Kohta Murase ◽

Conor M B Omand ◽

Deanne L Coppejans ◽

Hiroshi Nagai ◽

Geoffrey C Bower ◽

...

Keyword(s):

Supernova Remnants ◽

Gamma Ray ◽

Thermal Emission ◽

Crab Nebula ◽

Pulsar Wind Nebulae ◽

Pulsar Wind ◽

The Crab Nebula ◽

Gamma Ray Telescopes ◽

Very High ◽

Fast Rotating

Abstract Fast-rotating pulsars and magnetars have been suggested as the central engines of super-luminous supernovae (SLSNe) and fast radio bursts, and this scenario naturally predicts non-thermal synchrotron emission from their nascent pulsar wind nebulae (PWNe). We report results of high-frequency radio observations with ALMA and NOEMA for three SLSNe (SN 2015bn, SN 2016ard, and SN 2017egm), and present a detailed theoretical model to calculate non-thermal emission from PWNe with an age of ∼1 − 3 yr. We find that the ALMA data disfavors a PWN model motivated by the Crab nebula for SN 2015bn and SN 2017egm, and argue that this tension can be resolved if the nebular magnetization is very high or very low. Such models can be tested by future MeV-GeV gamma-ray telescopes such as AMEGO.

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Galactic X-Ray Polarimetry and High-Resolution X-Ray Spectroscopy

Symposium - International Astronomical Union ◽

10.1017/s0074180900100324 ◽

1973 ◽

Vol 55 ◽

pp. 118-131

Author(s):

R. Novick

Keyword(s):

High Resolution ◽

Crab Nebula ◽

Source Parameters ◽

Line Emission ◽

Theoretical Models ◽

Coronal Line ◽

X Ray ◽

Cygnus Loop ◽

Coronal Line Emission ◽

The Crab Nebula

Stellar X-ray spectroscopy and polarimetry are discussed in terms of the source parameters that can be determined through such studies and in terms of the constraints that these studies will place on theoretical models. The spectroscopic and polarimetric results that have been obtained to date are reviewed. These include the recent discovery of X-ray polarization in the Crab Nebula and the recent evidence for X-ray coronal line emission in the Cygnus Loop. Finally, the properties and predicted performance of a number of satellite-borne spectrometers and polarimeters are presented.

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X-ray Studies of the Pulsar Wind Nebula Around PSR B0540-69

Symposium - International Astronomical Union ◽

10.1017/s0074180900180933 ◽

2004 ◽

Vol 218 ◽

pp. 189-192

Author(s):

R. Petre ◽

U. Hwang ◽

S. S. Holt ◽

R. M. Williams

Keyword(s):

Particle Flux ◽

Crab Nebula ◽

Large Magellanic Cloud ◽

Thermal Component ◽

X Ray ◽

Average Ratio ◽

Spatially Resolved ◽

Pulsar Wind ◽

Spatially Resolved Spectroscopy ◽

The Crab Nebula

The pulsar wind nebula (PWN) surrounding the 50-ms pulsar B0540-69 in the Large Magellanic Cloud shares many properties with the Crab Nebula, the canonical Galactic PWN. We have used the ACIS instrument on the Chandra X-ray Observatory to perform spatially resolved spectroscopy of the PWN. The spectrum of the inner 10″ is characterized by a simple power law, with a spectral index that steepens strongly with radius. Outside the central 10″ the spectra also require a thermal component. This diameter corresponds to a shell detected in [OIII], suggesting that this shell represents a skin around the PWN, in analogy to the Crab. We infer the value of several key PWN parameters, including σ, the average ratio of electromagnetic to particle flux.

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The Binary X-Ray Stars – the Observational Picture

Symposium - International Astronomical Union ◽

10.1017/s0074180900010603 ◽

1975 ◽

Vol 67 ◽

pp. 411-464 ◽

Cited By ~ 2

Author(s):

Herbert Gursky ◽

Ethan Schreier

Keyword(s):

Neutron Star ◽

Thermal Radiation ◽

Crab Nebula ◽

Cosmic Ray ◽

Stellar Systems ◽

X Ray ◽

Pathological Conditions ◽

The Galaxy ◽

The Crab Nebula

When X-ray sources in the galaxy were discovered in 1962 (Giacconi et al., 1962) it was only possible to speculate on their nature, which centered on supernova and cosmic-ray phenomena since these were the only very energetic events known. In particular, the discovery of an X-ray source associated with the Crab Nebula led to the idea that the emission might be the thermal radiation from the surface of a hot, neutron star. However, it was soon demonstrated (Bowyer et al., 1964) that a neutron star could not be responsible for the bulk of the X-radiation from the Crab, and it was not possible to exclude highly pathological conditions in otherwise ordinary stellar systems as being responsible for the X-ray sources (cf. Hayakawa and Matsuoka, 1964).

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