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dc.contributor.author한인식-
dc.date.accessioned2019-07-22T16:30:18Z-
dc.date.available2019-07-22T16:30:18Z-
dc.date.issued2019-
dc.identifier.issn1475-7516-
dc.identifier.otherOAK-25023-
dc.identifier.urihttp://dspace.ewha.ac.kr/handle/2015.oak/250103-
dc.description.abstractAssuming a standard Maxwellian for the WIMP velocity distribution, we obtain the bounds from null WIMP search results of 59.5 days of COSINE-100 data on the DAMA/LIBRA-phase2 modulation effect within the context of the non-relativistic effective theory of WIMP-nucleus scattering. Here, we systematically assume that one of the effective operators allowed by Galilean invariance dominates in the effective Hamiltonian of a spin-1/2 dark matter (DM) particle. We find that, although DAMA/LIBRA and COSINE-100 use the same sodium-iodide target, the comparison of the two results still depends on the particle-physics model. This is mainly due to two reasons: i) the WIMP signal spectral shape; ii) the expected modulation fractions, when the upper bound on the time-averaged rate in COSINE-100 is converted into a constraint on the annual modulation component in DAMA/LIBRA . We find that the latter effect is the dominant one. For several effective operators the expected modulation fractions are larger than in the standard spin-independent or spin-dependent interaction cases. As a consequence, compatibility between the modulation effect observed in DAMA/LIBRA and the null result from COSINE-100 is still possible for several non-relativistic operators. At low WIMP masses such relatively high values of the modulation fractions arise because COSINE-100 is mainly sensitive to WIMP-sodium scattering events, due to the higher threshold compared to DAMA/LIBRA . A next COSINE analysis is expected to have a full sensitivity for the 5 σ region of DAMA/LIBRA. © 2019 IOP Publishing Ltd and Sissa Medialab.-
dc.languageEnglish-
dc.publisherInstitute of Physics Publishing-
dc.subjectDark matter experiments-
dc.subjectDark matter theory-
dc.titleCOSINE-100 and DAMA/LIBRA-phase2 in WIMP effective models-
dc.typeArticle-
dc.relation.issue6-
dc.relation.volume2019-
dc.relation.indexSCIE-
dc.relation.indexSCOPUS-
dc.relation.journaltitleJournal of Cosmology and Astroparticle Physics-
dc.identifier.doi10.1088/1475-7516/2019/06/048-
dc.identifier.wosidWOS:000472954100001-
dc.identifier.scopusid2-s2.0-85069476681-
dc.author.googleAdhikari G.-
dc.author.googleAdhikari P.-
dc.author.googleDe Souza E.B.-
dc.author.googleCarlin N.-
dc.author.googleChoi S.-
dc.author.googleDjamal M.-
dc.author.googleEzeribe A.C.-
dc.author.googleHa C.-
dc.author.googleHahn I.S.-
dc.author.googleJeon E.J.-
dc.author.googleJo J.H.-
dc.author.googleJoo H.W.-
dc.author.googleKang W.G.-
dc.author.googleKang W.-
dc.author.googleKauer M.-
dc.author.googleKim G.S.-
dc.author.googleKim H.-
dc.author.googleKim H.J.-
dc.author.googleKim K.W.-
dc.author.googleKim N.Y.-
dc.author.googleKim S.K.-
dc.author.googleKim Y.D.-
dc.author.googleKim Y.H.-
dc.author.googleKo Y.J.-
dc.author.googleKudryavtsev V.A.-
dc.author.googleLee H.S.-
dc.author.googleLee J.-
dc.author.googleLee J.Y.-
dc.author.googleLee M.H.-
dc.author.googleLeonard D.S.-
dc.author.googleLynch W.A.-
dc.author.googleMaruyama R.H.-
dc.author.googleMouton F.-
dc.author.googleOlsen S.L.-
dc.author.googlePark B.J.-
dc.author.googlePark H.K.-
dc.author.googlePark H.S.-
dc.author.googlePark K.S.-
dc.author.googlePitta R.L.C.-
dc.author.googlePrihtiadi H.-
dc.author.googleRa S.J.-
dc.author.googleRott C.-
dc.author.googleShin K.A.-
dc.author.googleScarff A.-
dc.author.googleSpooner N.J.C.-
dc.author.googleThompson W.G.-
dc.author.googleYang L.-
dc.author.googleYu G.H.-
dc.author.googleKang S.-
dc.author.googleScopel S.-
dc.author.googleTomar G.-
dc.author.googleYoon J.-H.-
dc.author.googleThe COSINE-100 collaboration-
dc.author.googleThe Sogang Phenomenology Group-
dc.contributor.scopusid한인식(7201832280)-
dc.date.modifydate20190827100823-
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사범대학 > 과학교육과 > Journal papers
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