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dc.contributor.authorChang, Feng-Yinen_US
dc.contributor.authorChen, Pisinen_US
dc.contributor.authorLin, Guey-Linen_US
dc.contributor.authorNoble, Roberten_US
dc.contributor.authorSydora, Richarden_US
dc.date.accessioned2019-04-03T06:42:30Z-
dc.date.available2019-04-03T06:42:30Z-
dc.date.issued2009-03-20en_US
dc.identifier.issn0031-9007en_US
dc.identifier.urihttp://dx.doi.org/10.1103/PhysRevLett.102.111101en_US
dc.identifier.urihttp://hdl.handle.net/11536/7471-
dc.description.abstractMagnetowave induced plasma wakefield acceleration (MPWA) in a relativistic astrophysical outflow has been proposed as a viable mechanism for the acceleration of cosmic particles to ultrahigh energies. Here we present simulation results that clearly demonstrate the viability of this mechanism for the first time. We invoke the high frequency and high speed whistler mode for the driving pulse. The plasma wakefield obtained in the simulations compares favorably with our newly developed relativistic theory of the MPWA. We show that, under appropriate conditions, the plasma wakefield maintains very high coherence and can sustain high-gradient acceleration over hundreds of plasma skin depths. Invoking active galactic nuclei as the site, we show that MPWA production of ultrahigh energy cosmic rays beyond ZeV (10(21) eV) is possible.en_US
dc.language.isoen_USen_US
dc.titleMagnetowave Induced Plasma Wakefield Acceleration for Ultrahigh Energy Cosmic Raysen_US
dc.typeArticleen_US
dc.identifier.doi10.1103/PhysRevLett.102.111101en_US
dc.identifier.journalPHYSICAL REVIEW LETTERSen_US
dc.citation.volume102en_US
dc.citation.issue11en_US
dc.citation.spage0en_US
dc.citation.epage0en_US
dc.contributor.department物理研究所zh_TW
dc.contributor.departmentInstitute of Physicsen_US
dc.identifier.wosnumberWOS:000264380200012en_US
dc.citation.woscount16en_US
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