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000315502 020__ $$a978-3-935702-59-1
000315502 0247_ $$2datacite_doi$$a10.3204/DESY-PROC-2014-03/davidson_sacha
000315502 0247_ $$2ISSN$$a1435-8077
000315502 037__ $$aPUBDB-2016-05909
000315502 041__ $$aEnglish
000315502 1001_ $$0P:(DE-HGF)0$$aDavidson, Sacha $$b0$$eCorresponding author
000315502 1112_ $$0C14-06-29.1$$2inspire$$a10th Patras Workshop on Axions, WIMPs and WISPs$$cGeneva$$d2014-06-29 - 2014-07-04$$gAXION-WIMP 2014$$wSwitzerland
000315502 245__ $$aThe Pressure of Misalignment Axions: a Difference from WIMPs in Galaxy Formation?
000315502 260__ $$aHamburg$$bVerlag Deutsches Elektronen-Synchrotron$$c2014
000315502 29510 $$aDavidson, Sacha "The Pressure of Misalignment Axions:a Difference from WIMPs in Galaxy Formation?" in Proceedings, 10th Patras Workshop on Axions, WIMPs and WISPs (AXION-WIMP 2014)  / Tsesmelis, Emmanuel, Maroudas, Marios (eds.), Verlag Deutsches Elektronen-Synchrotron : 2014 ; AXION-WIMP 2014 : 10th Patras Workshop on Axions, WIMPs and WISPs, 2014-06-29 - 2014-07-04, Geneva
000315502 300__ $$a51-54
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000315502 4900_ $$0PERI:(DE-600)2450075-6$$aDESY-PROC
000315502 520__ $$aTwo populations of axions can contribute to cold dark matter: the classical field produced via the misalignment mechanism, and the modes produced in the decay of strings. The classical field has extra pressure, as compared to WIMPs, which could have observable consequences in non-linear galaxy formation.
000315502 7870_ $$0PUBDB-2016-05897$$aTsesmelis, Emmanuel et. al.$$dVerlag Deutsches Elektronen-Synchrotron$$iisPartOf$$rDESY-PROC-2014-03$$tProceedings, 10th Patras Workshop on Axions, WIMPs and WISPs (AXION-WIMP 2014) : Geneva, Switzerland, June 29-July 4, 2014
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