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1、TASI2008LECTURESONDARKMATTERDANHOOPERTheoreticalAstrophysicsGroup,FermiNationalAcceleratorLaboratory,DepartmentofAstronomyandAstrophysics,UniversityofChicagodhooper@fnal.govBasedonlecturesgivenatthe2008TheoreticalAdvancedStudyInstitute(TASI),Ireviewheresomeaspe
2、ctsofthephenomenologyofparticledarkmatter,includingtheprocessofthermalfreeze-outintheearlyuniverse,andthedirectandindirectdetectionofWIMPs.Ialsodescribesomeofthemostpopularparticlecandidatesfordarkmatterandsummarizethecurrentstatusofthequesttodiscoverdarkmatter
3、’sparticleidentity.1.EvidenceForDarkMatterAwidevarietyofevidencehasaccumulatedinsupportofdarkmatter’sexistence.Atgalacticandsub-galacticscales,thisevidenceincludesgalac-ticrotationcurves[1],theweakgravitationallensingofdistantgalaxiesbyforegroundstructure[2],an
4、dtheweakmodulationofstronglensingaroundindividualmassiveellipticalgalaxies[3].Furthermore,velocitydis-persionsofstarsinsomedwarfgalaxiesimplythattheycontainasmuchas∼103timesmoremassthancanbeattributedtotheirluminosity.Onthescaleofgalaxyclusters,observations(ofr
5、adialvelocities,weaklens-ing,andX-rayemission)indicateatotalcosmologicalmatterdensityofarXiv:0901.4090v1[hep-ph]26Jan2009ΩM≈0.2−0.3[4],whichismuchlargerthanthecorrespondingdensityinbaryons.Infact,itwasmeasurementsofvelocitydispersionsintheComaclusterwhichledFri
6、tzZwickytoclaimforthefirsttimein1933thatlargequantitiesofnon-luminousmatterarerequiredtobepresent[5].Oncos-mologicalscales,observationsoftheanisotropiesinthecosmicmicrowavebackgroundhaveleadtoadeterminationofthetotalmatterdensityofΩh2=0.1326±0.0063,wherehistheHu
7、bbleparameterinunitsofM100km/secperMpc(thisimprovestoΩh2=0.1358+0.0037ifdistanceM−0.0036measurementsfrombaryonacousticoscillationsandtypeIasupernovaeareincluded)[6].Incontrast,thisinformationcombinedwithmeasurementsof1thelightchemicalelementabundancesleadstoane
8、stimateofthebaryonicdensitygivenbyΩh2=0.02273±0.00062(Ωh2=0.02267+0.00058ifBAOBB−0.00059andSNareincluded)[7,6].Takentogether,theseobservationsstronglyleadustotheconclusionth