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Polarization evolution in strong magnetic fields

Heyl, Jeremy S. and Shaviv, Nir J. (2000) Polarization evolution in strong magnetic fields. Monthly Notices of the Royal Astronomical Society, 311 (3). pp. 555-564. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20111123-112839566

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Abstract

Extremely strong magnetic fields change the vacuum index of refraction. Although this polarization-dependent effect is small for typical neutron stars, it is large enough to decouple the polarization states of photons travelling within the field. The photon states evolve adiabatically and follow the changing magnetic field direction. The combination of a rotating magnetosphere and a frequency-dependent-state decoupling predicts polarization phase lags between different wavebands, if the emission process takes place well within the light cylinder. This QED effect may allow observations to distinguish between different pulsar-emission mechanisms and to reconstruct the structure of the magnetosphere.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1046/j.1365-8711.2000.03076.xDOIArticle
Additional Information:© 2000 Royal Astronomical Society. Accepted 1999 September 1; Received 1999 June 28; in original form 1999 February 1. Article first published online: 4 Apr. 2002.
Subject Keywords:magnetic fields; polarization; stars: neutron
Issue or Number:3
Record Number:CaltechAUTHORS:20111123-112839566
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20111123-112839566
Official Citation:Heyl, J. S. and Shaviv, N. J. (2000), Polarization evolution in strong magnetic fields. Monthly Notices of the Royal Astronomical Society, 311: 555–564. doi: 10.1046/j.1365-8711.2000.03076.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:27947
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:23 Nov 2011 21:17
Last Modified:19 May 2020 20:50

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