Curvature radiation of relativistic particles in the magnetosphere of pulsars

The most widely adopted model of pulsar radio emission is the hollow cone model, which fits much of the experimental data. The pulsar radio emission in this model is curvature radiation of relativistic particles flowing from the magnetic poles of the neutron star along a cone of open magnetic lines. The curvature radiation is amplified at the plasma frequency, therefore different radio frequencies f originate at different radii r of the emitting regions.

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Curvature radiation in rotating pulsar magnetosphere

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312024842 ◽

2012 ◽

Vol 8 (S291) ◽

pp. 552-554

Author(s):

P. F. Wang ◽

C. Wang ◽

J. L. Han

Keyword(s):

Magnetic Field ◽

Circular Polarization ◽

Field Line ◽

Pulsar Magnetosphere ◽

Curvature Radiation ◽

Line Region ◽

Open Field Line ◽

Polarized Emission ◽

Field Lines ◽

Relativistic Particles

AbstractWe investigate the curvature radiation from relativistic particles streaming along magnetic field lines and co-rotating with a pulsar. The co-rotation affects the trajectories of the particles and hence the emission properties, especially the polarization. For three density models in the form of core, cone and patches, we calculate the polarized emission at a given height and also the integrated emission for the whole open field line region, and try to explain the generation of circular polarization.

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Supernovae and interstellar gas dynamics

Symposium - International Astronomical Union ◽

10.1017/s0074180900100774 ◽

1967 ◽

Vol 31 ◽

pp. 117-119

Author(s):

F. D. Kahn ◽

L. Woltjer

Keyword(s):

Lower Limit ◽

High Velocity ◽

Gas Dynamics ◽

Interstellar Cloud ◽

Interstellar Gas ◽

Random Motions ◽

Relativistic Particles

The efficiency of the transfer of energy from supernovae into interstellar cloud motions is investigated. A lower limit of about 0·002 is obtained, but values near 0·01 are more likely. Taking all uncertainties in the theory and observations into account, the energy per supernova, in the form of relativistic particles or high-velocity matter, needed to maintain the random motions in the interstellar gas is estimated as 1051·4±1ergs.

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Spontaneous and induced emission by relativistic particles in a crystal and possibilities for utilization of this effect in physics

Uspekhi Fizicheskih Nauk ◽

10.3367/ufnr.0127.197903j.0531 ◽

1979 ◽

Vol 127 (3) ◽

pp. 531 ◽

Cited By ~ 6

Author(s):

M.A. Kumakhov

Keyword(s):

Relativistic Particles

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Active Nuclei and Redshift Problems

Highlights of Astronomy ◽

10.1017/s1539299600005542 ◽

1983 ◽

Vol 6 ◽

pp. 531-533

Author(s):

Geoffrey Burbidge

Keyword(s):

Galactic Nuclei ◽

Seyfert Galaxies ◽

Radio Sources ◽

Powerful Radio ◽

Radiation Mechanism ◽

X Ray ◽

Major Interest ◽

Relativistic Particles

More than 20 years ago V. A. Ambartsumian proposed that much of the activity in galaxies was dominated and even generated by their nuclei. Subsequent observational work in radio, optical and x-ray frequencies has borne out his prophecy, and major interest has centered about the nature of the machine in the galactic nucleus. The major characteristic of this machine is that it releases energy rapidly and often spasmodically by processes which are not thermonuclear in origin.The original studies which led to the conclusion that nuclei were all important were observations of the powerful radio sources and Seyfert galaxies, and evidence for the ejection of gas from galaxies of many types. The realization that the synchrotron mechanism was the dominant radiation mechanism and the later studies of Compton radiation were fundamental in leading to the conclusion that large fluxes of relativistic particles must be generated in galactic nuclei.

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