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Plasma Masers in Radio Pulsars

Published online by Cambridge University Press:  25 May 2016

M. Lyutikov ,
R. Blandford  and
G. Machabeli
M. Lyutikov
Affiliation:
Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, Canada
R. Blandford
Affiliation:
Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, Canada
G. Machabeli
Affiliation:
Abastumani Astrophysics Observatory, A. Kazbegi Av. 2a, Tbilisi 380060, Republic of Georgia

Abstract

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Relativistic plasma masers operating on the anomalous cyclotron-Cherenkov resonance (ω - k||v|| + ωB/γres = 0) and on the Cherenkovdrift resonance (ω - k||v|| - kxud = 0) are capable of explaining the main observational characteristics of pulsar radio emission. Both electromagnetic instabilities are due to the interaction of the fast particles of the primary beam and from the tail of the distribution with the normal modes of a strongly magnetized, one-dimensional electron-positron plasma. In a typical pulsar, both resonances occur in the outer parts of the magnetosphere at rres ≍ 109 cm.

Type
Part I: Talks
Information
Symposium - International Astronomical Union , Volume 195: Highly Energetic Physical Processes and Mechanisms , 2000 , pp. 243 - 244
Copyright
Copyright © Astronomical Society of the Pacific 2000 

References

Lyutikov, 1999, J. Plas. Phys., 62, 65.CrossRefGoogle Scholar
Lyutikov, M., Blandford, R. D., & Machabeli, G. Z. 1999a, ApJ, 512, 804.CrossRefGoogle Scholar
Lyutikov, Machabeli, & Blandford, 1999b, MNRAS, 305, 338.CrossRefGoogle Scholar