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Axions, Majorana Neutrino Masses and implications for the dark sector
of the Universe
Workshop on the Standard Model and Beyond
September 2 - 10, 2017
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• PART I: Mechanism (beyond seesaw) for right-handed neutrino mass generation through Axion-Right-handed Neutrino Interactions
• PART II – Astrophysical Implications: ΛCDMfitsverywellAstrophysicalDataforUniverseatLarge scales
• BUT:@GALACTICSCALES,DWARFGALAXIES)–DISCREPANCYbetweenΛCDM-basedsimula?onsandobserva?ons–“small scale Cosmology crisis” – problems (i)Core-cuspproblem,(ii)Themissingsatellitesproblem
(iii)Too-Big-to-failproblem•
• Self-Interac?ngDarkmaLer(SIDM)asasoluDon(ontopofastrophysicalones)?
• PART III:Right-Handed(50keVmass)neutrinoswithmassivevectorself-interacDonsasaconcreteSIDMmodel&consequencesforgalacDcstructure
Arguelles,NEM,Rueda,RuffiniJCAP1604(2016)no.04,038
NEM&PilaXsisPhys.Rev.D86(2012)124038
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• PART I: Mechanism (beyond seesaw) for right-handed neutrino mass generation through Axion-Right-handed Neutrino Interactions
• PART II – Astrophysical Implications: ΛCDMfitsverywellAstrophysicalDataforUniverseatLarge scales
• BUT:@GALACTICSCALES,DWARFGALAXIES)–DISCREPANCYbetweenΛCDM-basedsimula?onsandobserva?ons–“small scale Cosmology crisis” – problems (i)Core-cuspproblem,(ii)Themissingsatellitesproblem
(iii)Too-Big-to-failproblem•
• Self-Interac?ngDarkmaLer(SIDM)asasoluDon(ontopofastrophysicalones)?
• PART III:Right-Handed(50keVmass)neutrinoswithmassivevectorself-interacDonsasaconcreteSIDMmodel&consequencesforgalacDcstructure
Arguelles,NEM,Rueda,RuffiniJCAP1604(2016)no.04,038
NEM&PilaXsisPhys.Rev.D86(2012)124038
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• PART I: Mechanism (beyond seesaw) for right-handed neutrino mass generation through Axion-Right-handed Neutrino Interactions
• PART II – Astrophysical Implications: ΛCDMfitsverywellAstrophysicalDataforUniverseatLarge scales
• BUT:@GALACTICSCALES,DWARFGALAXIES)–DISCREPANCYbetweenΛCDM-basedsimula?onsandobserva?ons–“small scale Cosmology crisis” – problems (i)Core-cuspproblem,(ii)Themissingsatellitesproblem
(iii)Too-Big-to-failproblem•
• Self-Interac?ngDarkmaLer(SIDM)asasoluDon(ontopofastrophysicalones)?
• PART III:Right-Handed(50keVmass)neutrinoswithmassivevectorself-interacDonsasaconcreteSIDMmodel&consequencesforgalacDcstructure
Arguelles,NEM,Rueda,RuffiniJCAP1604(2016)no.04,038
NEM&PilaXsisPhys.Rev.D86(2012)124038
Anomalies, Kalb-Ramond Axions and Gravity Basic String-Inspired Effective Field theory
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• PART I: Mechanism (beyond seesaw) for right-handed neutrino mass generation through Axion-Right-handed Neutrino Interactions
• PART II – Astrophysical Implications: ΛCDMfitsverywellAstrophysicalDataforUniverseatLarge scales
• BUT:@GALACTICSCALES,DWARFGALAXIES)–DISCREPANCYbetweenΛCDM-basedsimula?onsandobserva?ons–“small scale Cosmology crisis” – problems (i)Core-cuspproblem,(ii)Themissingsatellitesproblem
(iii)Too-Big-to-failproblem•
• Self-Interac?ngDarkmaLer(SIDM)asasoluDon(ontopofastrophysicalones)?
• PART III:Right-Handed(50keVmass)neutrinoswithmassivevectorself-interacDonsasaconcreteSIDMmodel&consequencesforgalacDcstructure
Arguelles,NEM,Rueda,RuffiniJCAP1604(2016)no.04,038
NEM&PilaXsisPhys.Rev.D86(2012)124038
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• PART I: Mechanism (beyond seesaw) for right-handed neutrino mass generation through Axion-Right-handed Neutrino Interactions
• PART II – Astrophysical Implications: ΛCDMfitsverywellAstrophysicalDataforUniverseatLarge scales
• BUT:@GALACTICSCALES,DWARFGALAXIES)–DISCREPANCYbetweenΛCDM-basedsimula?onsandobserva?ons–“small scale Cosmology crisis” – problems (i)Core-cuspproblem,(ii)Themissingsatellitesproblem
(iii)Too-Big-to-failproblem•
• Self-Interac?ngDarkmaLer(SIDM)asasoluDon(ontopofastrophysicalones)?
• PART III:Right-Handed(50keVmass)neutrinoswithmassivevectorself-interacDonsasaconcreteSIDMmodel&consequencesforgalacDcstructure
Arguelles,NEM,Rueda,RuffiniJCAP1604(2016)no.04,038
NEM&PilaXsisPhys.Rev.D86(2012)124038
Willarguethat:(i)resoluDonofGalac?ccore-halostructureproblemsofΛCDMsimulaDonsvsobservaDons+core-cuspandotherproblemsofsmall-scalecosmology``crisis’’canbeprovidedbyself-interac?ngRight-handed(Majorana)neutrinoswithmasses,m,atleast 47 keV (ii)FromaparDclephysicsperspecDveofνMSM,withHiggsportalcommunica?ontostandardmodelsector,cosmologicalconstraintsimplymassesoflightestofRHneutrinos,m,at most 50 keV SocombinaDonofthese(diverse)constraintsimplynarrowwindow 47 keV c-2 ≤ m ≤ 50 keV c-2
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PART I Right-Handed Neutrino
Majorana Mass generation (beyond seesaw)
& the role of Axions...
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ANOMALOUS GENERATION OF RIGHT-HANDED MAJORANA NEUTRINO MASSES THROUGH TORSIONFUL QUANTUM GRAVITY UV complete string models ?
NEM&PilaXsis2012PRD86,124038arXiv:1209.6387
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MasslessGravita?onalmul?pletof(closed)strings:spin0scalar(dilaton)spin2tracelesssymemtricrank2tensor(graviton)spin1asn?symmetricrank2tensor
Bµ⌫ = �B⌫µ
EffecDvefieldtheories(lowenergyscaleE<<Ms)``gauge’’invariant
Bµ⌫ ! Bµ⌫ + @[µ✓(x)⌫]
Dependonlyonfieldstrength: Hµ⌫⇢ = @[µB⌫⇢]
Bianchi identity : @[�Hµ⌫⇢] = 0 ! d ?H = 0
String Theories with Antisymmetric Tensor Backgrounds
KALB-RAMOND FIELD
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ROLEOFH-FIELDASTORSION
EFFECTIVEGRAVITATIONALACTIONINSTRINGLOW-ENERGYLIMIT
4-DIMPART
Contorsion
)
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ROLEOFH-FIELDASTORSION–AXIONFIELD
EFFECTIVEGRAVITATIONALACTIONINSTRINGLOW-ENERGYLIMIT
4-DIMPART
IN 4-DIM DEFINE DUAL OF H AS : b(x)=Pseudoscalar
(Kalb-Ramond(KR)axion)
)
⇠ 1
2@µb @µb
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FERMIONSCOUPLETOH–TORSIONVIAGRAVITATIONALCOVARIANTDERIVATIVE
TORSIONFULCONNECTION,FIRST-ORDERFORMALISM
contorsion
Hcab
Kabc =1
2
⇣Tcab � Tabc � Tbca
�
Non-trivialcontribuDonstoBμ
Da = @a �i
4!bca�
bc
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FERMIONSCOUPLETOH–TORSIONVIAGRAVITATIONALCOVARIANTDERIVATIVE
TORSIONFULCONNECTION,FIRST-ORDERFORMALISM
contorsion
Hcab
Kabc =1
2
⇣Tcab � Tabc � Tbca
�
Non-trivialcontribuDonstoBμ
Bd ⇠ ✏abcdHbca
S 3Z
d
4x �
a�
5Ba
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FermionicFieldTheorieswithH-TorsionEFFECTIVEACTIONAFTERINTEGRATINGOUT
QUANTUMTORSIONFLUCTUATIONS
+standardDiractermswithouttorsion
Fermions:
Bianchi identity
conserved``torsion‘’charge
classical
Postulate conservation at quantum level by adding counterterms
Implement via constraint à lagrange multiplier in Path integral à b-field
Tabc ! Hcab = ✏cabd @db
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FermionicFieldTheorieswithH-TorsionEFFECTIVEACTIONAFTERINTEGRATINGOUT
QUANTUMTORSIONFLUCTUATIONS
+standardDiractermswithouttorsion
Fermions:
Bianchi identity
conserved``torsion‘’charge
classical
Postulate conservation at quantum level by adding counterterms
Implement via constraint à lagrange multiplier in Path integral à b-field
Tabc ! Hcab = ✏cabd @db
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?
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?
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par?alintegrate
?
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par?alintegrate
Use chiral anomaly equation (one-loop) in curved space-time:
Hence, effective action of torsion-full QED
?
?
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par?alintegrate
Use chiral anomaly equation (one-loop) in curved space-time:
Hence, effective action of torsion-full QED bRR̃� bF F̃
coupling
?
?
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FermionicFieldTheorieswithH-TorsionEFFECTIVEACTIONAFTERINTEGRATINGOUT
QUANTUMTORSIONFLUCTUATIONS
+
+StandardModeltermsforfermions
SHIFTSYMMETRYb(x)àb(x)+c
totalderivaDves
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ANOMALOUSMAJORANANEUTRINOMASSTERMSfromQUANTUMTORSION
OURSCENARIOBreaksuchshiAsymmetrybycouplingfirstb(x)toanotherpseudoscalarfieldsuchasQCDaxiona(x)(ore.g.otherstringaxions)
Mavromatos,PilafsisarXiv:1209.6387
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ANOMALOUSMAJORANANEUTRINOMASSTERMSfromQUANTUMTORSION
OURSCENARIOBreaksuchshiAsymmetrybycouplingfirstb(x)toanotherpseudoscalarfieldsuchasQCDaxiona(x)(ore.g.otherstringaxions)
Mavromatos,PilafsisarXiv:1209.6387
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ANOMALOUSMAJORANANEUTRINOMASSTERMSfromQUANTUMTORSION
OURSCENARIOBreaksuchshiAsymmetrybycouplingfirstb(x)toanotherpseudoscalarfieldsuchasQCDaxiona(x)(ore.g.otherstringaxions)
Yukawaright-handedneutrinofields
Mavromatos,PilafsisarXiv:1209.6387
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Field redefinition
so, effective action becomes
musthaveotherwiseaxionfielda(x)appearsasaghostàcanonicallynormalisedkinePcterms
CHIRALITYCHANGE
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THREE-LOOPANOMALOUSFERMIONMASSTERMS
ONE-LOOP
CHIRALITYCHANGE
GRAVITONGRAVITON AXION
Λ=UVcutoff
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SOME NUMBERS
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SOME NUMBERS
INTERESTINGWARMDARKMATTER
REGIMEAppropriateHierarchyfortheothertwomassiveRight-handedneutrinosforLeptogenesis-Baryogenesis&DarkmaLerconstraintscanbearrangedbychoosingYukawacouplings
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SOME NUMBERS
INTERESTINGWARMDARKMATTER
REGIMEAppropriateHierarchyfortheothertwomassiveRight-handedneutrinosforLeptogenesis-Baryogenesis&DarkmaLerconstraintscanbearrangedbychoosingYukawacouplings
Maybe(discrete)symmetryreasons(cfLeontaris-Vlachosapproach)forcetwooftheheavierRHneutrinostobedegenerateàdictatepanernsfortheaxion-RH-neutrinoYukawacouplingsya
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FINITENESSOFTHEMASS
MULTI-AXION SCENARIOS (e.g. string axiverse)
posi?vemassspectrumforallaxions
simplifyingallmixingequals
Arvanitaki,Dimopoulosetal.
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MULTI-AXION SCENARIOS (e.g. string axiverse)
posi?vemassspectrumforallaxions
simplifyingallmixingequals
MR:UVfiniteforn=3@2-loopindependentofaxionmass
FINITENESSOFTHEMASS
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MULTI-AXION SCENARIOS (e.g. string axiverse)
posi?vemassspectrumforallaxions
simplifyingallmixingequals
MR:UVfiniteforn=3@2-loopindependentofaxionmass
FINITENESSOFTHEMASS
Three RH neutrinos Three axions Three generations
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PART II Implications for the Dark Sector-
Astro/Cosmological Phenomenology
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THEDARKSECTOROFTHEUNIVERSE
Active ν
ObservaPonsfrom:SupernovaeIaCMBBaryonAcousDcOscillaDonsGalaxySurveysStructureFormaDondataStrong&Weaklensing
68.3%]DarkEnergy%
26.8%]DarkManer
4.9%Atoms
http://www.cosmos.esa.int/web/planck/publications#Planck2015
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THEDARKSECTOROFTHEUNIVERSE
Active ν
ObservaPonsfrom:SupernovaeIaCMBBaryonAcousDcOscillaDonsGalaxySurveysStructureFormaDondataStrong&Weaklensing
68.3%]DarkEnergy%
26.8%]DarkManer
4.9%Atoms
http://www.cosmos.esa.int/web/planck/publications#Planck2015
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But.....therearesDllopenissueswith
theΛCDMframework@small(galac?c)scales
What are they? and what do
sterile neutrinos have to do with them???
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PART IIb
Small-scale Cosmology ``crisis’’
Collisionless ΛCDM - based N-body simulations
≠ galactic scale observations
especially Dwarf Galaxy structure
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The 3-Problems of�Galactic-Scale-Cosmology (GSC)
(i) The Core-Cusp problem (or cuspy-halo problem):
Nearlyallsimula?onsformdarkmanerhaloswhichhavecuspydarkmaYerdistribuDons,withthedensityincreasingsteeplyatsmallradii;onthecontrary,therotaPoncurvesofmostoftheobserveddwarfgalaxiesindicateflatcentraldensityprofiles("cores”).
B.Moore(1994)J.G.deBlok[arXiv:0910.3538]Se-HeonOhetal.,Astrophys.J.149(6),96(2015).
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The 3-Problems of�Galactic-Scale-Cosmology (GSC)
(ii) The missing satellite problem (or, dwarf galaxy problem)
Althoughthereseemtobeenoughobservednormal-sizedgalaxiestoaccountforsuchadistribuDon,thenumberofdwarfgalaxiesisordersofmagnitudelowerthanthatexpectedfromthesimula?ons.E.g.therewereobservedtobearound38dwarfgalaxiesintheLocalGroup,andonlyaround11orbiDngtheMilkyWay,yetonedarkmaLersimula?onpredictedaround500MilkyWaydwarfsatellites
B.Mooreetal.,Astrophys.J.524,L19(1999)A.Klypin,etal.,Astrophys.J.522,82(1999)E.PolisenskyandM.Ricot,PRD83,043506(2011)
simulated observed Mostmassivesubhaloes
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(ii) The missing satellite (dwarves) problem
v<40km/sec(M<1010M¤) discrepancyapparent
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The 3-Problems of�Galactic-Scale-Cosmology (GSC)
simulated observed Mostmassivesubhaloes
(iii) The Too-Big-to-Fail Problem
ΛCDMsimulaDonspredictthatthemostmassivesubhaloesoftheMilkyWayaretoodensetohostanyofitsbrightestsatellites,withluminosityhigherthan105theluminosityoftheSun.
(Modelsthatarebasedonsimula?onspredictmuchlargerrota?onalveloci?esthantheobservedones
Rota?onalveloci?esàmeasureofenclosedmassàΛCDMpredictedsatellitesaretoomassive(toobig).)
M.Boylan-Kolchin,J.S.Bullock&M.Kaplinghat,MNRAS415,L11(2011);ibid.422,1203(2012)
Central density of most massive subhaloes (left) too high to host dwarf galaxies of MW (right)
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(iii) The too-big-to-fail Problem
Con?nuouscurve:rota?oncurveoftypicallargestsub-halooftheMilkyWayassimulatedbycollisionlessΛCDM
Datapointspertaintoobservedcircularveloci?esofthelargestsubhaloesoftheMilkyWayattheirhalf-lightradii
M.Boylan-Kolchin,J.S.Bullock&M.Kaplinghat,MNRAS415,L11(2011);ibid.422,1203(2012)
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Astrophysicalexplana?onsThe missing satellite problem: (i)Smallerhalosdoexistbutonlyafewofthemendupbecomingvisible(havenotbeenabletoanractenoughbaryonicmanertocreateavisibledwarf)(cfKeckobserva?ons(2007)ofeightnewlydiscoveredultrafaintMilkyWaydwarfsatellitesshowedthatsixwerealmostexclusivelycomposedofDM,around99.9%(withamass-to-lightraDoofabout1000))–Suchultra-faintdwarfssubstanDallyalleviatethediscrepancy,buttherearesDlldiscrepanciesbyafactorofaboutfourtoofewdwarvesoverasignicantrangeofmasses.(ii)Galaxyforma?oninlow-massdarkmanerhalosisstronglysuppressedaXerre-ioniza?onàsimulatedcircularvelocityfuncDonofCDMsubhalosinapproximateagreementwiththeobservedcircularvelocityfuncDonofMilkyWaysatellitegalaxies.(iii) Dwarvestendtobemergedintoor?dallystrippedapartbylargergalaxiesdueto
complexinteracDons.ThisDdalstrippinghasbeenpartoftheprobleminidenDfyingdwarfgalaxiesinfirstplace,whichisdifficultduetotheirlowsurfacebrightnessandhighdiffusionsothattheyarevirtuallyunno?ceable.
Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
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(iv)(Baryonic)Feedbackplaysanimportantrole:complexprocessesbymeansofwhichstarformaDonandmaneraccreDonontoblackholesdepositenergyinthesurroundingenvironmentsofgalaxies
Astrophysicalexplana?ons
Varioustypesoffeedback:
RadiaPve:photoionizaDon,radiaDonpressure(stellar,orfromaccreDondiskofasupermassiveBH(AGN))Mechanical:supernovaeexplosions,cosmicrayexertedpressure
PossibletoexplainMissingsatelliteproblemwithBaryonic(notwellunderstood)physicsfeedback
Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)MicroscopicPhysicsexplana?onsneeded?
All of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)MicroscopicPhysicsexplana?onsneeded?
All of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
MicroscopicPhysicsexplana?onsAll of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à
(i)Exo?cmechanismsofEarlyUniverseimplysuppresseddensityfluctsatsubgalac?cscales(e.g.modelswithbrokenscaleinvarianceduringinfla?on,butsomewhatlackingclearmicroscopicmo?va?onfrompar?clephysics)
Kamionkowski,Liddleastro-ph/9911103;Yokohama,astro-ph/0009127;Zentner,Bullock,astro-ph/0205216;Ashoorioon,Krause,hep-th/0607001;Kobayashi,Takahashi,arXiv:1011.3988,...
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
MicroscopicPhysicsexplana?onsAll of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à (ii) modify gravity models (no DM except neutrinos)a0≈1.2x10−10ms−2ModifiedGravita?onalaccelera?on@galac?cscales
Milgrom,Bekenstein(TeVeS)
simplestmodels
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
MicroscopicPhysicsexplana?onsAll of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à (ii) modify gravity models (no DM except neutrinos)à lensing problematic (bullet cluster or other merging galaxies, offer observational support for DM)
Milgrom,Bekenstein(TeVeS)
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
MicroscopicPhysicsexplana?onsAll of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à (ii) modify gravity models (no DM except neutrinos)à lensing problematic (bullet cluster or other merging galaxies, offer observational support for DM)
for our talk
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Towards a Solution of the 3-Problems of�Galactic-Scale-Cosmology (GSC)
MicroscopicPhysicsexplana?onsAll of the above problems seem that cannot be entirely solved by conventional Astrophysics explanations – discrepancies still remain moreover: case by case studies
CHANGE THE ΛCDM à (ii) modify gravity models (no DM except neutrinos)à lensing problematic (bullet cluster or other merging galaxies, offer observational support for DM)(iii) CHANGE the DM properties à include self interactions or assume more than one dominant species ... with non-trivial role in galactic structure
for our talk
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Self-Interacting Dark Matter (SIDM)& small-scale Cosmology
Early pioneering works in implementing SIDM in N-body simulations
D.N.SpergelandP.J.Steinhardt,PRL84,3760(2000)
Figure of merit: (total) cross section per unit DM particle mass
σ/m
Early days:10GeVc-2≥m≥1MeVc-2inDMhaloeswithdensiDes
would imply observational effects in the inner haloes
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Self-Interacting Dark Matter (SIDM)& small-scale Cosmology
SIDM
SIDM
ΛCDM
ΛCDM
LargeScaleStructure:roughlythesame
Individualgalaxies:morecored&sphericalinSIDMmodels
MRochaetal.MNRAS430,81(2013)
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Self-Interacting Dark Matter (SIDM)& small-scale Cosmology
Early pioneering works in implementing SIDM in N-body simulations
D.N.SpergelandP.J.Steinhardt,PRL84,3760(2000)
Figure of merit: (total) cross section per unit DM particle mass
σ/m
Early days:10GeVc-2≥m≥1MeVc-2inDMhaloeswithdensiDes
would imply observational effects in the inner haloes
=1 barn/GeVconsistent withall current constraints ofGSC
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Compare with typical WIMPs , cross section in e.g. in SUSY modelsσ/m ≈ 10-22 barn/GeV
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Harvey,Massey,Kitching,Taylor,TitleyarXiv:1503.07675,Science
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Self-Interacting Dark Matter (SIDM)& small-scale Cosmology
Harvey,Massey,Kitching,Taylor,TitleyarXiv:1503.07675,Science
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massivevectorVμexchange
χ=Right-handedneutrino
Arguelles,NEM,Ruffini,Rueda,JCAP(2016)
InRight-handedneutrinoWDM:(i) massofO(50)keV,(ii) self-interac?onsstrongerthantheweakforce,108GF(iii)massive~104keVexchangevectorisOKforcore-galaxystructure
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PART III Self-Interacting Right-Handed Neutrino Warm Dark matter
& galactic core-halo structures
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A concrete model for SIDM – Right-handed keV Neutrinos with vector interactions
Arguelles,NEM,Rueda,Ruffini,JCAP1604,038(2016)
• Assume minimal extension of the Standard Model (non-supersymmetric) with right-handed neutrinos (RHN) self interacting via massive vector exchange interactions in the dark sector
• Use models of particle physics, e.g. νMSM (Shaposhnikov et al.) with three RHN, but augment them with these self-interactions• among the lightest of the RHN (quasi stable à DM) • Consistency of the halo-core profile of dwarf galaxies in Milky Way or large Elliptical à mass of lightest RHN in O(10) keV (WDM) ß Cosmological constraints of νMSM Two different approaches yield similar range for WDM mass!
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A concrete model for SIDM – Right-handed keV Neutrinos with vector interactions
Arguelles,NEM,Rueda,Ruffini,JCAP1604,038(2016)
• Assume minimal extension of the Standard Model (non-supersymmetric) with right-handed neutrinos (RHN) self interacting via massive vector exchange interactions in the dark sector
• Use models of particle physics, e.g. νMSM (Shaposhnikov et al.) with three RHN, but augment them with these self-interactions• among the lightest of the RHN (quasi stable à DM) • Consistency of the halo-core profile of dwarf galaxies in Milky Way or large Elliptical à mass of lightest RHN in O(10) keV (WDM) ß Cosmological constraints of νMSM Two different approaches yield similar range for WDM mass!
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SMExtensionwithNextraright-handedneutrinos
Minkowski,Fukugita,Yanagida,Mohapatra,Senjanovic,Lazarides,Shafi,WeLerich,Sechter,Valle,Paschos,Hill,Luty,Vergados,deGouvea…,Liao,Nelson,Buchmuller,Anisimov,diBari…,Akhmedov,Rubakov,Smirnov,Davidson,Giudice,Notari,Raidal,RioLo,Strumia,PilaXsis,Underwood,Asaka,Blanchet,Shaposhnikov,Boyarski,Ruchayskiy…Hernandez,Giun?...
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SMExtensionwithNextraright-handedneutrinos
Right-handedMassiveMajorananeutrinos
Leptons L↵ =
✓⌫↵↵�
◆, ↵ = e, µ, ⌧
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SMExtensionwithNextraright-handedneutrinos
HiggsscalarSU(2)Dual:
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SMExtensionwithNextraright-handedneutrinos
YukawacouplingsMatrix(I=1,2,3)
Majoranaphases
Mixing
⌫MSM Asaka, Blanchet, Boyarski, Ruchayskiy, Shaposhnikov
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SMExtensionwithNextraright-handedneutrinos
YukawacouplingsMatrix(I=1,...N=2or3)
Modelwith2or3singletfermionsworkswellinreproducingBaryonAsymmetryandisconsistentwithExperimentalDataonneutrinooscillaDons
ModelwithN=3alsoworksfine,andinfactitallowsoneoftheMajoranafermionstoalmostdecouplefromtherestoftheSMfields,thusprovidingcandidatesforlight(keVregionofmass)sterileneutrinoDarkMaYer.
For Constraints (compiled ν oscillation data) on (light) sterile neutrinos cf.: Giunti, Hernandez , … N=1 excluded by data
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SMExtensionwithNextraright-handedneutrinos
YukawacouplingsMatrix(I=1,...N=2or3)
Modelwith2or3singletfermionsworkswellinreproducingBaryonAsymmetryandisconsistentwithExperimentalDataonneutrinooscillaDons
ModelwithN=3alsoworksfine,andinfactitallowsoneoftheMajoranafermionstoalmostdecouplefromtherestoftheSMfields,thusprovidingcandidatesforlight(keVregionofmass)sterileneutrinoDarkMaYer.
For Constraints (compiled ν oscillation data) on (light) sterile neutrinos cf.: Giunti, Hernandez , … N=1 excluded by data
⌫MSM Asaka, Blanchet, Boyarski, Ruchayskiy, Shaposhnikov
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SMExtensionwithNextraright-handedneutrinos
YukawacouplingsMatrix(N=2or3)
⌫MSM
Majoranamassesto(2or3)acDve(light)neutrinosviaseesaw
NB:UponSymmetryBreaking<Φ>=v≠0àDiracmassterm
Minkowski,Fugujita,Yanagida,Lazarides,Shafi,WeLerich,Sechter,Valle,Mohapatra,Senjanovic,...
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LightNeutrinoMassesthroughseesaw
massoflightestofNIbyagreementwithCosmologicaldata
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LightNeutrinoMassesthroughseesaw
NàHν
Fα1≈10-10àmν2≈10-3eV2
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νMSMBoyarski, Ruchayskiy, Shaposhnikov…
MODEL CONSISTENT WITH BBN, STRUCTURE FORMATION DATA IN THE UNIVERSE & ALL OTHER ASTROPHYSICAL CONSTRAINTS
NàHνγ
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νMSMBoyarski, Ruchayskiy, Shaposhnikov…
MODEL CONSISTENT WITH BBN, STRUCTURE FORMATION DATA IN THE UNIVERSE & ALL OTHER ASTROPHYSICAL CONSTRAINTS
NàHνγ
Μ1=Ο(10)keV
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More than one sterile neutrino needed to reproduce Observed oscillations
νMSM Boyarski, Ruchayskiy, Shaposhnikov…
Constraintsontwoheavydegeneratesingletneutrinos
N1 DM production estimation in Early Universe must take into account its interactions with N2,3 heavy neutrinos
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More than one sterile neutrino needed to reproduce Observed oscillations
νMSM Boyarski, Ruchayskiy, Shaposhnikov…
Constraintsontwoheavydegeneratesingletneutrinos
N1 DM production estimation in Early Universe must take into account its interactions with N2,3 heavy neutrinos
Increased CPV
PilaXsis,
Underwood
...
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LightNeutrinoMassesthroughseesaw
This talk:restrictmassofN1byagreementwithobservedgalac?ccore-halostructureinSIDMversionsofthemodel
Fα1≈10-10àmν2≈10-3eV2
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LightNeutrinoMassesthroughseesaw
This talk:restrictmassofN1byagreementwithobservedgalac?ccore-halostructureinSIDMversionsofthemodel
Fα1≈10-10àmν2≈10-3eV2
Ignore in front of strong self-interactions for our purposes
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Right-handed keV Neutrinos with vector self-interactions & galactic structure
Arguelles,NEM,Rueda,Ruffini,JCAP1604,038(2016)
PlacetheνMSMincurvedspace?me
Classical fields (eqs of motion) satisfy detailed thermodynamic equilibrium conditionsin a galaxy at a temperature T < O(keV)
ν=ν(r)λ=λ(r)
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Right-handed keV Neutrinos with vector self-interactions & galactic structure
PlacetheνMSMincurvedspace?meν=ν(r)λ=λ(r)
Classical fields (eqs of motion) satisfy detailed thermodynamic equilibrium conditionsin a galaxy at a temperature T < O(keV)
Arguelles,NEM,Rueda,Ruffini,JCAP1604,038(2016)
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Measure of Strength of self Interactions
Right-handed keV Neutrinos with vector self-interactions & galactic structure
effec?veinterac?onsingalac?cmedium rm=core-halomatchingpoint=rc+δr
coreradius
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Right-handed keV Neutrinos with vector self-interactions & galactic structure
sterileνmass
No solution for gravitational collapse
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47keVc-2≤m≤350keVc-2
Right-handed keV Neutrinos with vector self-interactions & galactic structure
sterileνmass
Allowed WDM mass range
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47keVc-2≤m≤50keVc-2
Right-handed keV Neutrinos with vector self-interactions & galactic structure
Ifmixingwithobservablesectorisnon zero (νΜSM)ànarrow windowof allowed WDM mass!
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Noninterac?ngright-handedneutrinocasewithm=O(10)keV
Interactions make inner Core more compactand increase central degeneracycompared to non-interacting case
Arguelles,NEM,Rueda,Ruffini,
JCAP1604,038(2016)
Ruffini,Arguelles,Rueda,MNRAS(2015)
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Noninterac?ngright-handedneutrinocasewithm=O(10)keV
Interactions make inner Core more compactand increase central degeneracycompared to non-interacting case
Arguelles,NEM,Rueda,Ruffini,
JCAP1604,038(2016)
Provide natural resolution of Core-Cusp Problembecause the density profiles based on fermionic (as RH neutrinos) phase-space distributions develop always anextended plateau on halo scales, resembling Burkert or cored Einasto profilesMoreover,astheright-handedneutrinoDMmassis`colder'byafewkeV(m≈47keVc-2)comparedtomostoftheWDMmodelsavailableintheliterature,ourmodeldoesnotsufferfromstandardWDMproblems,associatedwiththe`toowarm'natureofthepar?clesinvolved
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N-N Cross sections under massive vector exchange
(perturbation theory gV < 1 OK)
to resolve issues of small-scalecosmology crisis
Hiddensectorvectorinterac?ons->Muchstrongerthanweakinterac?onsinvisiblesector
Arguelles,NEM,Rueda,Ruffini,
JCAP1604,038(2016)
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Conclusions-Outlook – so far • AtgalacDcscalesΛCDMmodelsuffersfromdiscrepancieswithobservaDonsregardingthecore-cusp,missingsatellite,andtoobigtofailproblemsofsmall-scale Cosmology ``crisis’’ ...
• Toremediethis,selfinterac?onsamongDMhavebeenintroducedwithrelaDvelystrongcrosssecDonsperunitdarkmanermassσ/m:
• Wehaveconsideredtheroleofthelightestoftheright-handedneutrinosinνΜSMextensionsofthestandardmodel,andaddedappropriatelystrongvectorinterac?onsinthedarksectoramongtheneutrinosàincreaseinnerdegeneracyandinnercoreregionindwarfsatellitesoftheMilkyWayorLargeellipDcalgalaxiesForinteracDonstrengths108 GF,WDM mass = 47-50 keV,&vectormass<104 keV,wecanresolvethethreesmall-scaleCosmologyproblems.
• TheRHneutrinoWDM,whichsolvescore-halostructureingalaxies,mayco-existwithotherCDMDMspeciesàsearchforitinpar?clephysicsandneutrinooscilla?onexperiments
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Conclusions - Outlook• AtgalacDcscalesΛCDMmodelsuffersfromdiscrepancieswithobservaDonsregardingthecore-cusp,missingsatellite,andtoobigtofailproblemsofsmall-scale Cosmology ``crisis’’ ...
• Toremediethis,selfinterac?onsamongDMhavebeenintroducedwithrelaDvelystrongcrosssecDonsperunitdarkmanermassσ/m:
• Wehaveconsideredtheroleofthelightestoftheright-handedneutrinosinνΜSMextensionsofthestandardmodel,andaddedappropriatelystrongvectorinterac?onsinthedarksectoramongtheneutrinosàincreaseinnerdegeneracyandinnercoreregionindwarfsatellitesoftheMilkyWayorLargeellipDcalgalaxiesForinteracDonstrengths108 GF,WDM mass = 47-50 keV,&vectormass<104 keV,wecanresolvethethreesmall-scaleCosmologyproblems.
• TheRHneutrinoWDM,whichsolvescore-halostructureingalaxies,mayco-existwithotherCDMDMspeciesàsearchforitinpar?clephysicsandneutrinooscilla?onexperiments(egSHiP)...
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Conclusions - Outlook • AtgalacDcscalesΛCDMmodelsuffersfromdiscrepancieswithobservaDonsregardingthecore-cusp,missingsatellite,andtoobigtofailproblemsofsmall-scale Cosmology ``crisis’’ ...
• Toremediethis,selfinterac?onsamongDMhavebeenintroducedwithrelaDvelystrongcrosssecDonsperunitdarkmanermassσ/m:
• Wehaveconsideredtheroleofthelightestoftheright-handedneutrinosinνΜSMextensionsofthestandardmodel,andaddedappropriatelystrongvectorinterac?onsinthedarksectoramongtheneutrinosàincreaseinnerdegeneracyandinnercoreregionindwarfsatellitesoftheMilkyWayorLargeellipDcalgalaxiesForinteracDonstrengths108 GF,WDM mass = 47-50 keV,&vectormass<104 keV,wecanresolvethethreesmall-scaleCosmologyproblems.
• TheRHneutrinoWDM,whichsolvescore-halostructureingalaxies,mayco-existwithotherCDMDMspeciesàcouplingwithaxions may lead to Mass generation for Right Handed Neutrinos
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THANK YOU !
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SPARES
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DarkMatter
Rotational Curves of galaxies, gravitational lensing growth of structure
Baryon-onlyModels,withoutDarkManer
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavourTYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
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DarkMatter
Rotational Curves of galaxies, gravitational lensing growth of structure
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavour
TYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
X
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DarkMatter
Rotational Curves of galaxies, gravitational lensing growth of structure
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavour
TYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
X mWDM=10keV
DistribuDonofdarkhaloeswithmassM>
WMAP,PlanckColl2015
Yoshidaetal.astro-ph/0303622
Re-ionization of the Universe @ redshift z=20 numericalN-bodysimula?onsbasedonwarm&ΛCDMmodels
excludes Warm DMmWDM ≤ 10 keV !
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DarkMatter
Rotational Curves of galaxies, gravitational lensing growth of structure
Baryon-onlyModels,withoutDarkManer
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavour
TYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
Compatible withall current data !m ≥ 100 keV 100 keV ≤ mWDM = mCDM
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THEORETICALSCENARIOSSUPERSYMMETRYneutralino
SUPERGRAVITYgraviPno(ifsufficientlylight)
AXIONS(standardQCDorstringy)
STERILENEUTRINOS...
DarkMatter
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavourTYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
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THEORETICALSCENARIOSSUPERSYMMETRYneutralino
SUPERGRAVITYgraviPno(ifsufficientlylight)
AXIONS(standardQCDorstringy)
STERILENEUTRINOS...
Theore?calModeldependenceinderivingboundsinexperimentalsearches
DarkMatter
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavourTYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
e.g. typical thermal WIMPsCMB-observations-compatible DM relic abundance occurs cross sections of weak-interactions type
``WIMP miracle’’
m� ⇠ O(100 GeV � TeV)
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σ/m≈10-22barn/GeV
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THEORETICALSCENARIOSSUPERSYMMETRYneutralino
SUPERGRAVITYgraviPno(ifsufficientlylight)
AXIONS(standardQCDorstringy)
STERILENEUTRINOS...
Theore?calModeldependenceinderivingboundsinexperimentalsearches
DarkMatter
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavourTYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
e.g. typical thermal WIMPsCMB-observations-compatible DM relic abundance occurs cross sections of weak-interactions type
``WIMP miracle’’
m� ⇠ O(100 GeV � TeV)
![Page 101: Axions, Majorana Neutrino Masses and implications for the dark …cern_ch_01.pdf · 2017. 9. 18. · Workshop on the Standard Model and Beyond September 2 - 10, 2017 • PART I: Mechanism](https://reader035.vdocuments.pub/reader035/viewer/2022071109/5fe380692f9aa0757d7fd8ab/html5/thumbnails/101.jpg)
THEORETICALSCENARIOSSUPERSYMMETRYneutralino
SUPERGRAVITYgraviPno(ifsufficientlylight)
AXIONS(standardQCDorstringy)
STERILENEUTRINOS...
Theore?calModeldependenceinderivingboundsinexperimentalsearches
DarkMatter
DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavourTYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)
This talk