Axions, Majorana Neutrino Masses and implications for the dark …cern_ch_01.pdf · 2017. 9....

Axions, Majorana Neutrino Masses and implications for the dark sector

of the Universe

Workshop on the Standard Model and Beyond

September 2 - 10, 2017

•  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









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

PART I Right-Handed Neutrino

Majorana Mass generation (beyond seesaw)

& the role of Axions...

ANOMALOUS GENERATION OF RIGHT-HANDED MAJORANA NEUTRINO MASSES THROUGH TORSIONFUL QUANTUM GRAVITY UV complete string models ?

NEM&PilaXsis2012PRD86,124038arXiv:1209.6387

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

ROLEOFH-FIELDASTORSION

EFFECTIVEGRAVITATIONALACTIONINSTRINGLOW-ENERGYLIMIT

4-DIMPART

Contorsion

)

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

FERMIONSCOUPLETOH–TORSIONVIAGRAVITATIONALCOVARIANTDERIVATIVE

TORSIONFULCONNECTION,FIRST-ORDERFORMALISM

contorsion

Hcab

Kabc =1

2

⇣Tcab � Tabc � Tbca

�

Non-trivialcontribuDonstoBμ

Da = @a �i

4!bca�

bc

FERMIONSCOUPLETOH–TORSIONVIAGRAVITATIONALCOVARIANTDERIVATIVE

TORSIONFULCONNECTION,FIRST-ORDERFORMALISM

contorsion

Hcab

Kabc =1

2

⇣Tcab � Tabc � Tbca

�

Non-trivialcontribuDonstoBμ

Bd ⇠ ✏abcdHbca

S 3Z

d

4x �

a�

5Ba

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

par?alintegrate

?

par?alintegrate

Use chiral anomaly equation (one-loop) in curved space-time:

Hence, effective action of torsion-full QED

?

?

par?alintegrate

Use chiral anomaly equation (one-loop) in curved space-time:

Hence, effective action of torsion-full QED bRR̃� bF F̃

coupling

?

?

FermionicFieldTheorieswithH-TorsionEFFECTIVEACTIONAFTERINTEGRATINGOUT

QUANTUMTORSIONFLUCTUATIONS

+

+StandardModeltermsforfermions

SHIFTSYMMETRYb(x)àb(x)+c

totalderivaDves

ANOMALOUSMAJORANANEUTRINOMASSTERMSfromQUANTUMTORSION

OURSCENARIOBreaksuchshiAsymmetrybycouplingfirstb(x)toanotherpseudoscalarfieldsuchasQCDaxiona(x)(ore.g.otherstringaxions)

Mavromatos,PilafsisarXiv:1209.6387

ANOMALOUSMAJORANANEUTRINOMASSTERMSfromQUANTUMTORSION

OURSCENARIOBreaksuchshiAsymmetrybycouplingfirstb(x)toanotherpseudoscalarfieldsuchasQCDaxiona(x)(ore.g.otherstringaxions)

Yukawaright-handedneutrinofields

Mavromatos,PilafsisarXiv:1209.6387

Field redefinition

so, effective action becomes

musthaveotherwiseaxionfielda(x)appearsasaghostàcanonicallynormalisedkinePcterms

CHIRALITYCHANGE

THREE-LOOPANOMALOUSFERMIONMASSTERMS

ONE-LOOP

CHIRALITYCHANGE

GRAVITONGRAVITON AXION

Λ=UVcutoff

SOME NUMBERS

SOME NUMBERS

INTERESTINGWARMDARKMATTER

REGIMEAppropriateHierarchyfortheothertwomassiveRight-handedneutrinosforLeptogenesis-Baryogenesis&DarkmaLerconstraintscanbearrangedbychoosingYukawacouplings

SOME NUMBERS

INTERESTINGWARMDARKMATTER

REGIMEAppropriateHierarchyfortheothertwomassiveRight-handedneutrinosforLeptogenesis-Baryogenesis&DarkmaLerconstraintscanbearrangedbychoosingYukawacouplings

Maybe(discrete)symmetryreasons(cfLeontaris-Vlachosapproach)forcetwooftheheavierRHneutrinostobedegenerateàdictatepanernsfortheaxion-RH-neutrinoYukawacouplingsya

FINITENESSOFTHEMASS

MULTI-AXION SCENARIOS (e.g. string axiverse)

posi?vemassspectrumforallaxions

simplifyingallmixingequals

Arvanitaki,Dimopoulosetal.




MR:UVfiniteforn=3@2-loopindependentofaxionmass

FINITENESSOFTHEMASS




MR:UVfiniteforn=3@2-loopindependentofaxionmass

FINITENESSOFTHEMASS

Three RH neutrinos Three axions Three generations

PART II Implications for the Dark Sector-

Astro/Cosmological Phenomenology

THEDARKSECTOROFTHEUNIVERSE

Active ν

ObservaPonsfrom:SupernovaeIaCMBBaryonAcousDcOscillaDonsGalaxySurveysStructureFormaDondataStrong&Weaklensing

68.3%]DarkEnergy%

26.8%]DarkManer

4.9%Atoms

http://www.cosmos.esa.int/web/planck/publications#Planck2015

But.....therearesDllopenissueswith

theΛCDMframework@small(galac?c)scales

What are they? and what do

sterile neutrinos have to do with them???

PART IIb

Small-scale Cosmology ``crisis’’

Collisionless ΛCDM - based N-body simulations

≠ galactic scale observations

especially Dwarf Galaxy structure

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).


(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

(ii) The missing satellite (dwarves) problem

v<40km/sec(M<1010M¤) discrepancyapparent


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)

(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)

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)

(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)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

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


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,...



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



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)



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



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

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


SIDM

SIDM

ΛCDM

ΛCDM

LargeScaleStructure:roughlythesame

Individualgalaxies:morecored&sphericalinSIDMmodels

MRochaetal.MNRAS430,81(2013)


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

Compare with typical WIMPs , cross section in e.g. in SUSY modelsσ/m ≈ 10-22 barn/GeV

Harvey,Massey,Kitching,Taylor,TitleyarXiv:1503.07675,Science

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

PART III Self-Interacting Right-Handed Neutrino Warm Dark matter

& galactic core-halo structures

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!

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?...


Right-handedMassiveMajorananeutrinos

Leptons L↵ =

✓⌫↵↵�

◆, ↵ = e, µ, ⌧


HiggsscalarSU(2)Dual:


YukawacouplingsMatrix(I=1,2,3)

Majoranaphases

Mixing

⌫MSM Asaka, Blanchet, Boyarski, Ruchayskiy, Shaposhnikov


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


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


YukawacouplingsMatrix(N=2or3)

⌫MSM

Majoranamassesto(2or3)acDve(light)neutrinosviaseesaw

NB:UponSymmetryBreaking<Φ>=v≠0àDiracmassterm

Minkowski,Fugujita,Yanagida,Lazarides,Shafi,WeLerich,Sechter,Valle,Mohapatra,Senjanovic,...

LightNeutrinoMassesthroughseesaw

massoflightestofNIbyagreementwithCosmologicaldata


NàHν

Fα1≈10-10àmν2≈10-3eV2

νMSMBoyarski, Ruchayskiy, Shaposhnikov…

MODEL CONSISTENT WITH BBN, STRUCTURE FORMATION DATA IN THE UNIVERSE & ALL OTHER ASTROPHYSICAL CONSTRAINTS

NàHνγ

νMSMBoyarski, Ruchayskiy, Shaposhnikov…

MODEL CONSISTENT WITH BBN, STRUCTURE FORMATION DATA IN THE UNIVERSE & ALL OTHER ASTROPHYSICAL CONSTRAINTS

NàHνγ

Μ1=Ο(10)keV

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

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

...


This talk:restrictmassofN1byagreementwithobservedgalac?ccore-halostructureinSIDMversionsofthemodel

Fα1≈10-10àmν2≈10-3eV2


This talk:restrictmassofN1byagreementwithobservedgalac?ccore-halostructureinSIDMversionsofthemodel

Fα1≈10-10àmν2≈10-3eV2

Ignore in front of strong self-interactions for our purposes

Right-handed keV Neutrinos with vector self-interactions & galactic structure


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)


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)


Measure of Strength of self Interactions


effec?veinterac?onsingalac?cmedium rm=core-halomatchingpoint=rc+δr

coreradius


sterileνmass

No solution for gravitational collapse

47keVc-2≤m≤350keVc-2


sterileνmass

Allowed WDM mass range

47keVc-2≤m≤50keVc-2


Ifmixingwithobservablesectorisnon zero (νΜSM)ànarrow windowof allowed WDM mass!

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)

Noninterac?ngright-handedneutrinocasewithm=O(10)keV

Interactions make inner Core more compactand increase central degeneracycompared to non-interacting case


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

N-N Cross sections under massive vector exchange

(perturbation theory gV < 1 OK)

to resolve issues of small-scalecosmology crisis

Hiddensectorvectorinterac?ons->Muchstrongerthanweakinterac?onsinvisiblesector


JCAP1604,038(2016)

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

Conclusions - Outlook•  AtgalacDcscalesΛCDMmodelsuffersfromdiscrepancieswithobservaDonsregardingthecore-cusp,missingsatellite,andtoobigtofailproblemsofsmall-scale Cosmology ``crisis’’ ...



•  TheRHneutrinoWDM,whichsolvescore-halostructureingalaxies,mayco-existwithotherCDMDMspeciesàsearchforitinpar?clephysicsandneutrinooscilla?onexperiments(egSHiP)...

Conclusions - Outlook •  AtgalacDcscalesΛCDMmodelsuffersfromdiscrepancieswithobservaDonsregardingthecore-cusp,missingsatellite,andtoobigtofailproblemsofsmall-scale Cosmology ``crisis’’ ...



•  TheRHneutrinoWDM,whichsolvescore-halostructureingalaxies,mayco-existwithotherCDMDMspeciesàcouplingwithaxions may lead to Mass generation for Right Handed Neutrinos

THANK YOU !

SPARES

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)

DarkMatter


DARKMATTER(DM):CURRENTEVIDENCEArgumentsinFavour

TYPESOFDM:hot,warm,coldASTROPHYSICALCONSTRAINTS(MODELINDEPENDENT)INDIRECTSEARCHES:collider(LHC&beyond)searchesphotons,neutrinos,maLer-an?maLerasymmetries(electron-positron,proton-an?proton)

X

DarkMatter




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 !

DarkMatter


Baryon-onlyModels,withoutDarkManer



Compatible withall current data !m ≥ 100 keV 100 keV ≤ mWDM = mCDM

THEORETICALSCENARIOSSUPERSYMMETRYneutralino

SUPERGRAVITYgraviPno(ifsufficientlylight)

AXIONS(standardQCDorstringy)

STERILENEUTRINOS...

DarkMatter





STERILENEUTRINOS...

Theore?calModeldependenceinderivingboundsinexperimentalsearches

DarkMatter


e.g. typical thermal WIMPsCMB-observations-compatible DM relic abundance occurs cross sections of weak-interactions type

``WIMP miracle’’

m� ⇠ O(100 GeV � TeV)

σ/m≈10-22barn/GeV




STERILENEUTRINOS...


DarkMatter


e.g. typical thermal WIMPsCMB-observations-compatible DM relic abundance occurs cross sections of weak-interactions type

``WIMP miracle’’

m� ⇠ O(100 GeV � TeV)




STERILENEUTRINOS...


DarkMatter


This talk

Axions, Majorana Neutrino Masses and implications for the dark …cern_ch_01.pdf · 2017. 9....

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