The Binary X-Ray Stars – the Observational Picture

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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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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Physical Processes and Parameters in the Magnetosphere of NP 0532

Symposium - International Astronomical Union ◽

10.1017/s0074180900007749 ◽

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.

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High Resolution X-ray Observations of 3C 58

Symposium - International Astronomical Union ◽

10.1017/s0074180900180921 ◽

2004 ◽

Vol 218 ◽

pp. 185-188

Author(s):

Patrick Slane

Keyword(s):

High Resolution ◽

Massive Star ◽

Thermal Emission ◽

Rotation Axis ◽

Crab Nebula ◽

X Ray ◽

The Galaxy ◽

Pulsar Wind ◽

Star Surface ◽

The Crab Nebula

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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Superfluidity in Neutron Stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900099988 ◽

1974 ◽

Vol 53 ◽

pp. 151-165

Author(s):

George Greenstein

Keyword(s):

Neutron Star ◽

Neutron Stars ◽

Crab Nebula ◽

Crab Pulsar ◽

X Ray ◽

Effects Of Rotation ◽

The Crab Nebula

We present a short Cook's tour of the possible effects of rotation coupled with superfluid properties of neutron star interiors. A suggestion is made to take advantage of forthcoming lunar occultations of the Crab Nebula in order to search for blackbody X-ray emission from the Crab pulsar.

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High Speed Photometry at Mt Stromlo Observatory

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000013904 ◽

1974 ◽

Vol 2 (5) ◽

pp. 278-280 ◽

Cited By ~ 1

Author(s):

B. A. Peterson

Keyword(s):

Black Holes ◽

Neutron Star ◽

High Speed ◽

Crab Nebula ◽

Binary Star ◽

Rotation Period ◽

Radio Pulsars ◽

X Ray ◽

High Speed Photometry ◽

The Crab Nebula

Important observations of X-ray sources and searches for the optical counterparts of X-ray and radio pulsars require a capability of detecting and analysing light variations with a time scale of milliseconds. X-ray sources in binary star systems are expected to be collapsed objects – neutron stars or black holes (Peterson 1973) – and are expected to produce light variations. In the case of a neutron star, pulses with the same period as the rotation period of the neutron star would be produced, and such have been observed from Cen X-3 (schreier et al. 1972) in the X-ray, and from Her X-1 (Middleditch and Nelson 1973) and the Crab Nebula pulsar (Cocke et al. 1969) in the X-ray optical.

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Do neutron stars produce jets?

Canadian Journal of Physics ◽

10.1139/p86-087 ◽

1986 ◽

Vol 64 (4) ◽

pp. 474-478 ◽

Cited By ~ 3

Author(s):

Eric D. Feigelson

Keyword(s):

Neutron Star ◽

Neutron Stars ◽

Supernova Remnants ◽

Binary Systems ◽

Crab Nebula ◽

Compact Object ◽

Radio Pulsars ◽

X Ray ◽

The Crab Nebula ◽

X Ray Binaries

The evidence for jets emanating from neutron stars is reviewed. Isolated radio pulsars do not appear to produce collimated outflows. A few supernova remnants, notably the Crab nebula, exhibit jetlike protrusions at their outer boundaries. These are probably "blowouts" of the plasma in the remnant rather than true jets from a neutron star. However, several cases of degenerate stars in X-ray binary systems do make jets. SS433 has twin precessing jets moving outward at v ~ 0.26c, and Sco X-1 has radio lobes with v ~ 0.0001c. Cyg X-3 appears to eject synchrotron plasmoids at high velocities. Other X-ray binaries associated with variable radio sources are discussed; some are interesting candidates for collimated outflow. G109.1-1.0 is an X-ray binary in a supernova remnant that may have radio or X-ray jets. It is not clear in all these cases, however, that the compact object is a neutron star and not a black hole or white dwarf.A tentative conclusion is reached that isolated neutron stars do not produce jets, but degenerate stars in accreting binary systems can. This suggests that the presence of an accretion disk, rather than the characteristics of an isolated pulsar's dipole magnetosphere, is critical in making collimated outflows.

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