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dc.contributor.authorVenter, C.
dc.contributor.authorDe Jager, O.C.
dc.date.accessioned2014-05-08T10:49:18Z
dc.date.available2014-05-08T10:49:18Z
dc.date.issued2010
dc.identifier.citationVenter, C. & De Jager, O.C. 2010. Accelerating high-energy pulsar radiation codes. Astrophysical journal, 725(1):1903-1909. [http://iopscience.iop.org/0004-637X/]en_US
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357 (Online)
dc.identifier.urihttp://hdl.handle.net/10394/10488
dc.identifier.urihttp://dx.doi.org/10.1088/0004-637X/725/2/1903
dc.identifier.urihttp://iopscience.iop.org/0004-637X/725/2/1903/pdf/apj_725_2_1903.pdf
dc.description.abstractCurvature radiation (CR) is believed to be a dominant mechanism for creating gamma-ray emission from pulsars and is emitted by relativistic particles that are constrained to move along curved magnetic field lines. Additionally, synchrotron radiation (SR) is expected to be radiated by both relativistic primaries (involving cyclotron resonant absorption of radio photons and re-emission of SR photons), or secondary electron–positron pairs (created by magnetic or photon–photon pair production processes involving CR gamma rays in the pulsar magnetosphere). When calculating these high-energy spectra, especially in the context of pulsar population studies where several millions of CR and SR spectra have to be generated, it is profitable to consider approximations that would save computational time without sacrificing too much accuracy. This paper focuses on one such approximation technique, and we show that one may gain significantly in computational speed while preserving the accuracy of the spectral results.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.rights
dc.subjectPulsars: generalen_US
dc.subjectradiation mechanisms: non-thermalen_US
dc.titleAccelerating high-energy pulsar radiation codesen_US
dc.typeArticleen_US
dc.contributor.researchID12006653 - Venter, Christo
dc.contributor.researchID10065857 - De Jager, Ocker Cornelis


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