models for dark energy - heidelberg universitywetteric/talks/cosmo/y0608/...dicke parameter ωin...
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Models for Dark Energy
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QuintessenceQuintessence
C.WetterichC.Wetterich
A.HebeckerA.Hebecker, , M.DoranM.Doran, , M.LilleyM.Lilley, , J.SchwindtJ.Schwindt,,C.MC.Müüllerller, , G.SchG.Schääferfer, , E.ThommesE.Thommes,,R.CaldwellR.Caldwell, , M.BartelmannM.Bartelmann,,K.KharwanK.Kharwan, , G.Robbers,T.DentG.Robbers,T.Dent, , S.SteffenS.Steffen,,L.AmendolaL.Amendola, , M.BaldiM.Baldi
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What is our universe made of ?What is our universe made of ?
quintessence !fire , air,
water, soil !
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Dark Energy Dark Energy dominates the Universedominates the Universe
Energy Energy -- density in the Universedensity in the Universe==
Matter + Dark EnergyMatter + Dark Energy
25 % + 75 %25 % + 75 %
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gravitational lens , HST
ΩΩmm= 0.25= 0.25
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ΩΩtottot=1=1
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Matter : everything that clumpsMatter : everything that clumps
----------------------------------------
Dark Energy density isDark Energy density isthe same at every point of space the same at every point of space
““ homogeneous homogeneous ““
Space between clumpsSpace between clumps
is not emptyis not empty
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Composition of the UniverseComposition of the Universe
ΩΩb b = 0.045 = 0.045 visible visible clumpingclumping
ΩΩdmdm= 0.2 = 0.2 invisibleinvisible clumpingclumping
ΩΩh h = 0.75 = 0.75 invisibleinvisible homogeneoushomogeneous
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What is Dark Energy ?
Cosmological Constant or
Quintessence ?
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Cosmological ConstantCosmological Constant-- Einstein Einstein --
Constant Constant λλ compatible with all symmetriescompatible with all symmetriesNo time variation in contribution to energy No time variation in contribution to energy densitydensity
Why so small ? Why so small ? λλ/M/M44 = 10= 10--120120
Why important just today ?Why important just today ?
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Cosm. Const. | Quintessencestatic | dynamical
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Cosmological mass scalesCosmological mass scales
Energy densityEnergy density
ρρ ~ ( 2.4~ ( 2.4××10 10 --33 eVeV ))-- 4
Reduced Planck massReduced Planck massM=2.44M=2.44××10101818GeVGeVNewtonNewton’’s constants constantGGNN=(8=(8ππMM²²)
4
)
Only ratios of mass scales are observable !Only ratios of mass scales are observable !
homogeneous dark energy: homogeneous dark energy: ρρhh/M/M44 = 6.5 = 6.5 1010¯¹²¹¹²¹
matter: matter: ρρmm/M/M4= 3.5 10= 3.5 10¯¹²¹¹²¹
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QuintessenceQuintessenceDynamical dark energy ,Dynamical dark energy ,
generated by scalargenerated by scalar fieldfield
((cosmoncosmon))C.Wetterich,Nucl.Phys.B302(1988)668, 24.9.87C.Wetterich,Nucl.Phys.B302(1988)668, 24.9.87P.J.E.Peebles,B.Ratra,ApJ.Lett.325(1988)L17, 20.10.87P.J.E.Peebles,B.Ratra,ApJ.Lett.325(1988)L17, 20.10.87
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Prediction :Prediction :
homogeneous dark energyhomogeneous dark energyinfluences recent cosmologyinfluences recent cosmology
-- of same order as dark matter of same order as dark matter --
Original models do not fit the present observationsOriginal models do not fit the present observations……. modifications. modifications
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QuintessenceQuintessence
CosmonCosmon –– Field Field φφ((x,y,z,tx,y,z,t))
Homogeneous und isotropic Universe : Homogeneous und isotropic Universe : φφ((x,y,z,tx,y,z,t)=)=φφ(t)(t)
Potential und kinetic energy of the Potential und kinetic energy of the cosmoncosmon --fieldfieldcontribute to a dynamical energy density of the Universe ! contribute to a dynamical energy density of the Universe !
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CosmonCosmon
Scalar field changes its value even in the Scalar field changes its value even in the present present cosmological epochcosmological epochPotential und kinetic energy of Potential und kinetic energy of cosmoncosmoncontribute to the energy density of the Universecontribute to the energy density of the UniverseTime Time -- variable dark energy : variable dark energy : ρρhh(t(t) decreases with time !) decreases with time !
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CosmonCosmon
Tiny massTiny mass
mmcc ~ H~ H
New long New long -- range interactionrange interaction
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““FundamentalFundamental”” InteractionsInteractions
Strong, electromagnetic, weakinteractions
gravitation cosmodynamics
On astronomical length scales:
graviton
+
cosmon
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Evolution of Evolution of cosmoncosmon fieldfield
Field equationsField equations
Potential V(Potential V(φφ) determines details of the model) determines details of the modele.g. e.g. V(V(φφ) =M) =M4 4 exp( exp( -- αφαφ/M )/M )
for increasing for increasing φφ the potential decreases the potential decreases towards zero !towards zero !
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Cosmic AttractorsCosmic Attractors
Solutions independent of initial conditions
typically V~t -2
φ ~ ln ( t )
Ωh ~ const.
details depend on V(φ)or kinetic term
early cosmology
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exponential potentialexponential potentialconstant fraction in dark energyconstant fraction in dark energy
ΩΩh h = n/= n/αα22
can explain order of magnitude can explain order of magnitude of dark energy !of dark energy !
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realistic quintessencerealistic quintessence
fraction in dark energy has to fraction in dark energy has to increase in increase in ““recent timerecent time”” !!
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cosmic coincidencecosmic coincidence
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Quintessence becomes important Quintessence becomes important ““todaytoday””
No reason why w shouldNo reason why w shouldbe constant in time !be constant in time !
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coincidence problemcoincidence problem
What is responsible for increase of What is responsible for increase of ΩΩhh for z < 6 ?for z < 6 ?
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a) Properties of a) Properties of cosmoncosmon potential or potential or kinetic termkinetic term
Late quintessenceLate quintessencew close to w close to --11ΩΩhh negligible in early negligible in early cosmologycosmology
needs tiny parameter, needs tiny parameter, similar to cosmological similar to cosmological constantconstant
Early quintessenceEarly quintessenceΩΩhh changes only modestlychanges only modestlyw changes in timew changes in time
transitiontransitionspecial feature in special feature in cosmoncosmonpotential or kinetic term potential or kinetic term becomes important becomes important ““nownow””tuning at tuning at ‰‰ levellevel
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b) Quintessence reacts to some b) Quintessence reacts to some special event in cosmologyspecial event in cosmology
Onset of Onset of matter dominancematter dominance
KK-- essenceessenceAmendarizAmendariz--PiconPicon, , MukhanovMukhanov,,SteinhardtSteinhardt
needs higher derivativeneeds higher derivativekinetic term
Appearance of Appearance of nonnon--linear structurelinear structure
BackBack--reaction effectreaction effect
needs coupling betweenneeds coupling betweenDark Matter and Dark Matter and Dark Energy
kinetic termDark Energy
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growing neutrino mass growing neutrino mass triggers transition to triggers transition to
almost static dark energyalmost static dark energy
growinggrowingneutrinoneutrinomassmass
L.Amendola,M.BaldiL.Amendola,M.Baldi,,……
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connection between dark energy connection between dark energy and neutrino propertiesand neutrino properties
present dark energy density given by neutrino masspresent dark energy density given by neutrino mass
present equationpresent equationof state given byof state given byneutrino mass !neutrino mass !
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dark energy fraction determined by dark energy fraction determined by neutrino massneutrino mass
constant neutrino constant neutrino -- cosmoncosmon coupling coupling ββ
variable neutrino variable neutrino -- cosmoncosmon couplingcoupling
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basic ingredient :basic ingredient :
cosmoncosmon coupling to neutrinoscoupling to neutrinos
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CosmonCosmon coupling to atomscoupling to atoms
Tiny !!!Tiny !!!Substantially weaker than gravity.Substantially weaker than gravity.NonNon--universal couplings bounded by testsuniversal couplings bounded by testsof equivalence principle.of equivalence principle.Universal coupling bounded by tests of Universal coupling bounded by tests of BransBrans--DickeDicke parameter parameter ωω in solar system.in solar system.Only very small influence on cosmology.Only very small influence on cosmology.
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CosmonCosmon coupling to Dark Mattercoupling to Dark Matter
Only bounded by cosmologyOnly bounded by cosmologySubstantial coupling possibleSubstantial coupling possibleCan modify scaling solution and late cosmologyCan modify scaling solution and late cosmologyRole in clustering of extended objects ?Role in clustering of extended objects ?
L. L. AmendolaAmendola
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CosmonCosmon coupling to neutrinoscoupling to neutrinos
can be large !can be large !Fardon,Nelson,WeinerFardon,Nelson,Weiner
interesting effects for cosmology if neutrino interesting effects for cosmology if neutrino mass is growingmass is growinggrowing neutrinos can stop the evolution of the growing neutrinos can stop the evolution of the cosmoncosmontransition from early scaling solution to transition from early scaling solution to cosmological constant dominated cosmologycosmological constant dominated cosmology
L.Amendola,M.BaldiL.Amendola,M.Baldi,,……
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growing neutrino mass growing neutrino mass triggers transition to triggers transition to
almost static dark energyalmost static dark energy
growinggrowingneutrinoneutrinomassmass
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cosmological selectioncosmological selection
present value of dark energy density set by present value of dark energy density set by cosmological event cosmological event
( neutrinos become non ( neutrinos become non –– relativistic )relativistic )
not given by ground state properties !not given by ground state properties !
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growing neutrinosgrowing neutrinos
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end of matter dominationend of matter domination
growing mass of neutrinosgrowing mass of neutrinos
at some moment energy density of neutrinos becomes at some moment energy density of neutrinos becomes more important than energy density of dark mattermore important than energy density of dark matter
end of matter dominated periodend of matter dominated periodsimilar to transition from radiation domination to similar to transition from radiation domination to matter dominationmatter dominationthis transition happens in the recent pastthis transition happens in the recent past
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neutrino massneutrino mass
seesaw andseesaw andcascadecascademechanismmechanism
triplet expectation value ~ doublet squaredtriplet expectation value ~ doublet squared
omit generation omit generation structurestructure
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cascade mechanismcascade mechanism
triplet expectation value ~triplet expectation value ~
M.MaggM.Magg , , ……G.LazaridesG.Lazarides , , Q.ShafiQ.Shafi , , ……
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varying neutrino massvarying neutrino mass
εε ≈≈ --0.050.05
triplet mass depends on triplet mass depends on cosmoncosmon field field φφ
neutrino mass depends on neutrino mass depends on φφ
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singular neutrino masssingular neutrino mass
triplet mass vanishes for triplet mass vanishes for φφ →→ φφtt
neutrino mass diverges for neutrino mass diverges for φφ →→ φφtt
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early scaling solution ( tracker solution )early scaling solution ( tracker solution )
neutrino mass unimportant in early cosmologyneutrino mass unimportant in early cosmology
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growing neutrinos growing neutrinos change change cosmoncosmon evolutionevolution
modification of conservation equation for neutrinosmodification of conservation equation for neutrinos
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effective stop of effective stop of cosmoncosmon evolutionevolution
cosmoncosmon evolution almost stops onceevolution almost stops onceneutrinos get non neutrinos get non ––relativisticrelativisticßß gets largegets large
This alwaysThis alwayshappens happens for for φφ →→ φφt t !!
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effective cosmological triggereffective cosmological triggerfor stop of for stop of cosmoncosmon evolution :evolution :neutrinos get nonneutrinos get non--relativisticrelativistic
this has happened recently !this has happened recently !
sets scales for dark energy !sets scales for dark energy !
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effective cosmological constanteffective cosmological constantat late timeat late time
realistic value realistic value forforαα φφt t / M / M ≈≈ 276276
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crossover to dark energy crossover to dark energy dominated universedominated universe
starts at time when starts at time when ““neutrino forceneutrino force”” becomes becomes important for the evolution of the important for the evolution of the cosmoncosmon fieldfield
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cosmological selection !cosmological selection !
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cosmoncosmon evolutionevolution
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neutrino fraction remains smallneutrino fraction remains small
mmνν = 0.45 = 0.45 eVeV
ΩΩνν
zz
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equation of stateequation of state
present equationpresent equationof state given byof state given byneutrino mass !neutrino mass !
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oscillating neutrino massoscillating neutrino mass
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Hubble parameterHubble parameter
as compared to as compared to ΛΛCDMCDM
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Hubble parameter ( z < Hubble parameter ( z < zzcc ))
only small only small differencedifferencefrom from ΛΛCDM !CDM !
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How can quintessence be How can quintessence be distinguished from a distinguished from a
cosmological constant ?cosmological constant ?
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Time dependence of dark energyTime dependence of dark energy
cosmological constant : Ωh ~ t² ~ (1+z)-3
M.Doran,…
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small early and large presentsmall early and large presentdark energydark energy
fraction in dark energy has substantially fraction in dark energy has substantially increased since end of structure formationincreased since end of structure formation
expansion of universe accelerates in present expansion of universe accelerates in present epochepoch
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effects of early dark energyeffects of early dark energy
modifies cosmological evolution (CMB)modifies cosmological evolution (CMB)slows down the growth of structureslows down the growth of structure
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Early quintessence slows down the Early quintessence slows down the growth of structuregrowth of structure
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interpolation of interpolation of ΩΩhh
bounds on bounds on Early Dark EnergyEarly Dark Energyafter WMAPafter WMAP’’0606
G.Robbers,M.DoranG.Robbers,M.Doran,,……
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bounds on bounds on Early Dark EnergyEarly Dark Energyafter WMAPafter WMAP’’0606
G.Robbers,M.DoranG.Robbers,M.Doran,,……
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Cluster number relative to ΛCDM
Little Early Dark Energy can make large effect !Little Early Dark Energy can make large effect !Non Non –– linear enhancementlinear enhancement
Two models with 4% Dark Energyduring structure formation
Fixed σ8 ( normalization dependence ! )
Bartelmann,DoranBartelmann,Doran,,……More clusters at high redshift !
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How to distinguish Q from How to distinguish Q from ΛΛ ??
A) Measurement A) Measurement ΩΩhh(z(z) ) H(zH(z))i) i) ΩΩhh(z(z) at the time of) at the time of
structure formation , CMB structure formation , CMB -- emissionemissionor or nucleosynthesisnucleosynthesis
ii) equation of state ii) equation of state wwhh((todaytoday) > ) > --11B) Time variation of fundamental B) Time variation of fundamental ““constantsconstants””C) Apparent violation of equivalence principleC) Apparent violation of equivalence principleD) Possible coupling between Dark Energy D) Possible coupling between Dark Energy
and Dark Materand Dark Mater
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CosmodynamicsCosmodynamics
CosmonCosmon mediates new longmediates new long--range interactionrange interactionRange : size of the Universe Range : size of the Universe –– horizonhorizonStrength : weaker than gravityStrength : weaker than gravity
photon electrodynamicsphoton electrodynamicsgraviton gravitygraviton gravitycosmoncosmon cosmodynamicscosmodynamics
Small correction to NewtonSmall correction to Newton’’s laws law
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Quintessence and time variation of Quintessence and time variation of fundamental constantsfundamental constants
Strong, electromagnetic, weakinteractions
gravitation cosmodynamics
Generic prediction
Strengthunknown
C.WetterichC.Wetterich , , Nucl.Phys.B302,645(1988Nucl.Phys.B302,645(1988))
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Time varying constantsTime varying constants
It is not difficult to obtain quintessence It is not difficult to obtain quintessence potentials from higher dimensional or string potentials from higher dimensional or string theoriestheoriesExponential form rather generic Exponential form rather generic ( after ( after WeylWeyl scaling)scaling)But most models show too strong time But most models show too strong time dependence of constants !dependence of constants !
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Are fundamental Are fundamental ““constantsconstants””time dependent ?time dependent ?
Fine structure constant Fine structure constant αα (electric charge)(electric charge)
Ratio electron mass to proton massRatio electron mass to proton mass
Ratio nucleon mass to Planck massRatio nucleon mass to Planck mass
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Quintessence and Quintessence and Time dependence of Time dependence of
““fundamental constantsfundamental constants””
Fine structure constant depends on value ofFine structure constant depends on value ofcosmoncosmon field : field : αα((φφ))
(similar in standard model: couplings depend on (similar in standard model: couplings depend on value of Higgs scalar field)value of Higgs scalar field)
Time evolution of Time evolution of φφTime evolution of Time evolution of αα
Jordan,Jordan,……
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baryons :
the matter of stars and humans
ΩΩbb = 0.045= 0.045
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primordial abundances primordial abundances for three GUT modelsfor three GUT models
T.DentT.Dent,,S.SternS.Stern,,……
present present observations : observations : 11σσ
HeHe
DD
LiLi
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three GUT modelsthree GUT models
unification scale ~ Planck scaleunification scale ~ Planck scale1) All particle physics scales ~1) All particle physics scales ~ΛΛQCDQCD
2) Fermi scale and 2) Fermi scale and fermionfermion masses ~ unification masses ~ unification scalescale3) Fermi scale varies more rapidly than 3) Fermi scale varies more rapidly than ΛΛQCDQCD
∆α∆α//αα ≈≈ 4 104 10--4 4 allowed for GUT 1 and 3 , larger allowed for GUT 1 and 3 , larger for GUT 2for GUT 2
∆∆ln(Mln(Mnn/M/MPP) ) ≈≈40 40 ∆α∆α//αα ≈≈ 0.015 allowed 0.015 allowed
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Time variation of coupling constants must be tiny –
would be of very high significance !
Possible signal for Quintessence
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SummarySummary
oo ΩΩhh = 0.75= 0.75
oo Q/Q/ΛΛ : dynamical und static dark energy will be : dynamical und static dark energy will be distinguishabledistinguishable
oo growing neutrino mass can explain why now problemgrowing neutrino mass can explain why now problem
oo Q : time varying fundamental coupling Q : time varying fundamental coupling ““constantsconstants””violation of equivalence principleviolation of equivalence principle
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????????????????????????????????????????????????
Are dark energy and dark matter related ?Are dark energy and dark matter related ?Can Quintessence be explained in a fundamental Can Quintessence be explained in a fundamental
unified theory ?unified theory ?
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Quintessence and solution of Quintessence and solution of cosmological constant cosmological constant
problem should be related !problem should be related !
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EndEnd
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A few referencesA few references
C.WetterichC.Wetterich , Nucl.Phys.B302,668(1988) , received 24.9.1987, Nucl.Phys.B302,668(1988) , received 24.9.1987
P.J.E.Peebles,B.RatraP.J.E.Peebles,B.Ratra , Astrophys.J.Lett.325,L17(1988) , received 20.10.1987, Astrophys.J.Lett.325,L17(1988) , received 20.10.1987
B.Ratra,P.J.E.PeeblesB.Ratra,P.J.E.Peebles , Phys.Rev.D37,3406(1988) , received 16.2.1988, Phys.Rev.D37,3406(1988) , received 16.2.1988
J.Frieman,C.T.Hill,A.Stebbins,I.WagaJ.Frieman,C.T.Hill,A.Stebbins,I.Waga , Phys.Rev.Lett.75,2077(1995), Phys.Rev.Lett.75,2077(1995)
P.FerreiraP.Ferreira, , M.JoyceM.Joyce , Phys.Rev.Lett.79,4740(1997), Phys.Rev.Lett.79,4740(1997)
C.WetterichC.Wetterich , Astron.Astrophys.301,321(1995), Astron.Astrophys.301,321(1995)
P.VianaP.Viana, , A.LiddleA.Liddle , Phys.Rev.D57,674(1998), Phys.Rev.D57,674(1998)
E.Copeland,A.Liddle,D.WandsE.Copeland,A.Liddle,D.Wands , Phys.Rev.D57,4686(1998), Phys.Rev.D57,4686(1998)
R.Caldwell,R.Dave,P.SteinhardtR.Caldwell,R.Dave,P.Steinhardt , Phys.Rev.Lett.80,1582(1998), Phys.Rev.Lett.80,1582(1998)
P.Steinhardt,L.Wang,I.ZlatevP.Steinhardt,L.Wang,I.Zlatev , Phys.Rev.Lett.82,896(1999), Phys.Rev.Lett.82,896(1999)