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On the nature of pulsar radio emission

Lyutikov, Maxim and Blandford, Roger D. and Machabeli, George (1999) On the nature of pulsar radio emission. Monthly Notices of the Royal Astronomical Society, 305 (2). pp. 338-352. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190603-094353813

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Abstract

A theory of pulsar radio emission generation, in which the observed waves are produced directly by maser-type plasma instabilities operating at the anomalous cyclotron-Cherenkov resonance ω — k∥v∥ + ω_B/γ_(res) = 0 and the Cherenkov drift resonance ω — k∥ v∥- k⊥ u_d =0, is capable of explaining the main observational characteristics of pulsar radio emission. The instabilities are due to the interaction of the fast particles from the primary beam and the tail of the distribution with the normal modes of a strongly magnetized one-dimensional electron-positron plasma. The waves emitted at these resonances are vacuum-like, electromagnetic waves that may leave the magnetosphere directly. In this model, the cyclotron-Cherenkov instability is responsible for the core-emission pattern and the Cherenkov drift instability produces conal emission. The conditions for the development of the cyclotron-Cherenkov instability are satisfied for both typical and millisecond pulsars provided that the streaming energy of the bulk plasma is not very high γ_p ≈ 10. In a typical pulsar the cyclotron-Cherenkov and Cherenkov drift resonances occur in the outer parts of the magnetosphere at r_(res), ≈ 10^9 cm. This theory can account for various aspects of pulsar phenomenology, including the morphology of the pulses, their polarization properties and their spectral behaviour. We propose several observational tests for the theory. The most prominent prediction is the high altitudes of the emission region and the linear polarization of conal emission in the plane orthogonal to the local osculating plane of the magnetic field.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1046/j.1365-8711.1999.02443.xDOIArticle
https://arxiv.org/abs/astro-ph/9806363arXivDiscussion Paper
ORCID:
AuthorORCID
Blandford, Roger D.0000-0002-1854-5506
Additional Information:© 1999 RAS. Accepted 1998 December 23. Received 1998 December 16; in original form 1998 July 8. Published: 11 May 1999. We would like to thank George Melikidze for his comments. ML would like to thank the Abastumani Astrophysics Observatory for the hospitality he received during his stays in Tbilisi. GZM acknowledges the support and hospitality during his stay at Caltech. This research was supported by NSF grant AST-9529170.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-9529170
Subject Keywords:plasmas - radiative transfer - waves - pulsars: general
Issue or Number:2
Record Number:CaltechAUTHORS:20190603-094353813
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190603-094353813
Official Citation:Maxim Lyutikov, Roger D. Blandford, George Machabeli, On the nature of pulsar radio emission, Monthly Notices of the Royal Astronomical Society, Volume 305, Issue 2, 11 May 1999, Pages 338–352, https://doi.org/10.1046/j.1365-8711.1999.02443.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96030
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 Jun 2019 18:42
Last Modified:03 Oct 2019 21:18

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