Determining the regimes of cold and warm inflation in the susy hybrid model

0.78 MB·English

by  Mar Bastero-Gil

Determining the regimes of cold and warm inflation in the SUSY hybrid model
Mar Bastero-Gil1,∗ and Arjun Berera2,†
1Departamento de F´ısica Te´orica y del Cosmos, Universidad de Granada, Granada-18071, Spain
2 School of Physics, University of Edinburgh, Edinburgh, EH9 3JZ, United Kingdom
The SUSY hybrid inflation model is found to dissipate radiation during the inflationary period.
Analysis is made of parameter regimes in which these dissipative effects are significant. The scalar
spectral index,its running,and thetensor-scalar ratio are computed in theentire parameter range
of the model. A clear prediction for strong dissipative warm inflation is found for nS −1 ≃ 0.98
and a low tensor-scalar ratio much below 10−6. The strong dissipative warm inflation regime also
is found to have no η-problem and the field amplitude much below the Planck scale. As will be
discussed,thishasimportanttheoreticalimplicationsinpermittingamuchwidervarietyofSUGRA
extensions tothe basic model.
5 keywords: cosmology, inflation
0
0 PACSnumbers: 98.80.Cq,11.30.Pb,12.60.Jv
2

n
a
J
I. INTRODUCTION
1
3
The success of the inflationary paradigm has motivated in recent times more serious efforts in building realistic

2 particlephysicsmodelsthatincorporatecosmology[1,2,3]. The objectiveofthissortofmodelbuilding istoaccount
v for various cosmological features, central being inflation, but also leptogenesis, dark matter etc... to constrain the
4
high energy properties of the model, and such that in the low energy regime the model reduces to the Standard
4
Model. Supersymmetry (SUSY) plays a central role here, since aside from its attractive features for particle physics,
1
1 italsoallowsstabilizing veryflatscalarpotentials,whichareessentialininflationmodelsdue to density perturbation
1 constraints. In this respect, a widely studied SUSY model of inflation has been the hybrid model,
4
0 W =κS(Φ1Φ2 µ2), (1)
−
/
h where Φ , Φ are a pair of chargedfields1 under some gaugegroupG, and S is the singlet whichplays the role of the
1 2
p
inflaton.
-
p AnimportantfeatureaboutthemodelEq. (1)anditsvariousembeddingsintomorerealisticparticlephysicsmodels
e [2, 5] is that the inflaton field generally interacts with other fields, with coupling strengths that can be fairly large.
h
Eventhough the nonzero vacuum energy necessaryto drive inflation will break SUSY, this underlying symmetry can
:
v stillprotecttheveryflatinflatonpotentialfromradiativecorrectionsarisingfromtheseperturbativelylargecouplings
i [6, 7]. It has been observed in recent works [6, 8] that the effect of interactions of the inflaton with other fields
X
does not simply affect the local contributions to the inflaton effective potential, but also induces temporally nonlocal
r
a terms in the inflaton evolution equation, that in the moderate to large perturbative regime yield sizable dissipative
effects. Although SUSY cancels the large local quantum effects, for the dynamical problem the nonlocal quantum
effects can not be canceled by SUSY. These dissipative effects in general can lead to warm inflationary regimes [9].
Thus the conclusion of the works [6, 7, 8] is that in general, models in which the inflaton has interactions with
other fields with moderate to strong perturbative coupling, inflation divides into two different dynamical regimes,
cold [10, 11, 12] and warm [9]. This finding is very important, since these two types of inflationary dynamics are
qualitatively muchdifferent. Thus one should expect different observablesignaturesin the two cases,as well as other
theoretical differences in the treatment of inflation.
ThepurposeofthispaperistoapplytheserecentfindingsaboutdissipativedynamicsduringinflationtotheSUSY
hybrid model Eq. (1) and to common extensions of this model. In particular, two models will be studied in this
paper, Eq. (1) and this model with a matter field ∆ ∆¯ coupled to it as
W =κS(Φ Φ µ2)+gΦ ∆∆¯ . (2)
1 2 2
−
∗Electronicaddress: [email protected]
†Electronicaddress: [email protected]
1 OnecouldalsoconsiderthefieldsΦ1,2 beinggaugesinglets. However,inthiscasethegravitinoconstraintonthereheatingtemperature
translatesintoκbeingatmostoftheorderof10−5 [4]. ThatconstraintisavoidedwheninsteadΦ1,2 arenon-singlets.
2
The above is a toy model representingan example of how the basic hybridmodel Eq. (1) is embedded within a more
complete particle physics model, in this case through the ∆ fields.
Inthis paper we willstudy inflationfor bothmodels Eqs. (1) and(2). We will showthat inthe abovemodels both
cold and warm inflation exist and we will determine the parameter regime for them. This will then explicitly verify
the conclusions from the recent papers on dissipation [6, 8], that showed both types of inflationary dynamics could
exist. In both inflationary regimes, we will calculate the scalar spectral index n 1, and its running dn /dlnk.
S S
−
With this information, we will then identify the qualitative andquantitative differences arisingfromthe warmversus
cold regimes.
We emphasize here that the main objective of this paper is to determine in an explicit and well-known model how
these two dynamically very different inflationary regimes emerge. This result departs radically from current wisdom,
in which it is tacitly always assumed that all regimes in any model are cold inflationary. In light of our result, many
other particle physics model building issues emerge in the warm inflationary regimes that we identify. Although we
make some effort in this paper to discuss these issues, it is not the purpose here to dwell on them. In cold inflation,
these issues have been the subject of many yearsof study, and likewise a complete understanding ofsimilar issues for
warm inflationary regimes will take focused effort in future work.
The paper is organized as follows. Sect. II reviews the effective potential for the SUSY hybrid model, as well as
some of the basic results based on this model for cold inflation. Sect. III reviews the main results of dissipative
dynamics during inflation based on [6, 8]. Included here are the main formulas for density perturbations and the
scalar spectral index in the presence of dissipation and a thermal bath. Subsects. IIIA and IIIB compute the effect
thatdissipationhasoninflatonevolutioninthetwomodelsEqs. (1)and(2)respectively. Theoutcomeoftheanalysis
in these two subsections is a graph that divides the parameter space of the model into cold and warm inflationary
regimes, and associated predictions for the scalar spectral index, its running and the tensor-scalar ratio. Sect. IV
addressessomemodelbuildingissuesthatemergeinthenewlyfoundwarminflationaryregimes,suchasthegravitino
abundances and the constraint on the reheating temperature. Finally Sec. V states our conclusions.
II. SUSY HYBRID MODEL
We briefly review first some well known results about standard supersymmetric hybrid inflation [13, 14, 15], in
order to study later what are the main modifications introduced when taking into account the dissipative dynamics
present during inflation [6, 8]. We consider the standard superpotential for the supersymmetric hybrid inflationary
model, Eq. (1). Without taking into account SUSY breaking, the zero-energy global minimum in the model Eq.
(1) is located at the vacuum expectation values (VEV) S=0, Φ = Φ = µ. If the gauge group G of Φ and Φ is
1 2 1 2
identified with a GUT symmetry, the scale µ would be the GUT symmetry breaking scale. On the other hand, for
S > µ, there is a local minimum at Φ = Φ = 0 with potential energy given by the constant term κ2µ4. Inflation
1 2
| |
occurs while the system is located in this false vacuum. Here, the inflaton scalar field S and its fermionic partner
remainmasslessattreelevel,while thescalarsΦ andΦ combineintoapairofrealscalarandpseudoscalarparticles
1 2
with mass m2 = κ2(S 2+µ2), and another pair with mass m2 = κ2(S 2 µ2); their fermionic superpartners are
+ | | − | | −
degenerate with mass m =κS .
F
| |
Duetothesplittinginthemasses,thereisanon-vanishingoneloopradiativecorrectiontothepotential,∆V,which
provides the necessary slope and mass correction2 to the inflaton potential to drive slow-roll inflation. In particular,
the first and second derivatives of the effective inflaton potential are given respectively by:
√2κ4µ3 (x2 1)(x2+1) x2+1 √2κ4µ3
∆V′ = 16π2N x3ln − x4 +xlnx2 1 = 16π2NF1[x], (3)
(cid:18) − (cid:19)
κ4µ2 (x2 1)(x2+1) x2+1 κ4µ2
∆V′′ = N 3x2ln − +ln = NF [x], (4)
16π2 x4 x2 1 16π2 2
(cid:18) − (cid:19)
where is the dimensionality3 ofthe Φ representations,x φ /(√2µ), φ is the realpartof the complex field S,
1,2 S S
N ≡
andwearesettingtheimaginarycomponentsofallthe fieldstozeroforsimplicity. Forlargex,wehave: F [x] 1/x,
1
F [x] 1/x2. ∼
2
∼−
2 We will not add any additional SUSY breaking mass term for the inflaton during inflation, so that its mass is given purely by the
radiativecorrections. GiventhattheµscaleistypicallyoftheorderoftheGUTscale,SUSYbreakingmassesoftheorderofO(1)TeV
arenegligibleunlessthecouplingκ<O(10−5).
3 Wetake =1throughout thispaperunlessotherwiseexplicitlystated.
N
3
Standard(cold)“slow-roll”inflationischaracterizedbyhavingsmallslow-rollparameterǫ 1andη 1,with
H H
≪ ≪
m2 V′ 2 κ2 κm 2 κ2 κm 2 2
ǫH = 2P V = (4π)2 4πµP (NF1[x])2 ≈ (4π)2 4πµP Nx2 , (5)
(cid:18) (cid:19) (cid:18) (cid:19) (cid:18) (cid:19)
V′′ κm 2 κm 2
ηH = m2P V = 4πµP NF2[x]≈− 4πµP xN2 , (6)
(cid:18) (cid:19) (cid:18) (cid:19)
wherem =2.4 1018 GeVisthe reducedPlanckmass. Therefore,duringinflationthe evolutionofthe inflatonfield
P
×
is well approximated by
3Hφ˙ +V′ 0. (7)
S
≃
At this point one should worryabout supergravity(SUGRA) corrections to the inflaton potential. Generically, those
give rise to mass correctionsfor the scalars during inflation of the order of O(H2), with η O(1), spoiling inflation
H
∼
(the so-calledη problem [13, 16]). However,such corrections are not present if we take the minimal Kahler potential
for the fields with a superpotential like Eqs.(1) and (2), and this is the choice we adopt in this paper. Nevertheless,
they will induce a quartic term (plus some higher order corrections) in the inflaton potential [2, 13, 17, 18], with
φ4
V κ2µ4(1+ S + )+∆V . (8)
≃ 8m4 ···
P
The quartic term dominates the inflationary dynamics when φ m , which happens for κ O(1).
S P
∼ ∼
The values of the coupling κ and the scale µ consistent with the inflationary dynamics are obtained by demanding
that (a) we have “enough” inflation (at least 60 e-folds), and (b) that the amplitude of the primordial spectrum
generated by the inflaton vacuum fluctuations are in the range given by COBE observations. The former constraint
gives the value of the inflaton field N ( 60) e-folds before the end of inflation,
e
≃
κm
P
x 2N , (9)
N e
≈ 4πµ
(cid:18) (cid:19)
p
which is then used to evaluate the amplitude of the primordial curvature spectrum,
H H 2 κ 2 4πµ 3 1 4N µ 2
P1/2 = = e . (10)
R (cid:18)φ˙S(cid:19)(cid:18)2π(cid:19) r3(cid:16)4π(cid:17) (cid:18)κmP(cid:19) F1[xN] ≈r 3 (cid:18)mP(cid:19)
Therefore,usingtheCOBEnormalization[19,20]P1/2 =5 10−5atN 60,wehave4thatµ 2 10−3m 5 1015
R × e ≃ ≃ × P ≃ ×
GeV.
Given that implicitly we are working with a SUGRA model, at most the VEV of the inflaton field could be of the
orderofthePlanckscale,preferablybelowthatscale. FromEq. (9)onecanseethatφ>m forvaluesofκ>0.8and
P
so are excluded [17]. Moreover, taking into account the quartic SUGRA correction in Eq.(8), the spectrum becomes
blue tilted(n >1)[2,17, 18,21]alreadyforκ 0.05,whichisnotfavoredbythe observationaldata onthe spectral
S
index from WMAP5, n =0.93 0.03 [20]. ≃
S
±
III. DISSIPATIVE DYNAMICS DURING INFLATION
Dissipativeeffects canbe importantalreadyduringinflation,modifying the inflationarydynamicsdescribedby Eq.
(7). These are related to the quantum corrections in the effective potential of the background field. When neither
the decay of the inflaton nor that of the fields coupled to the inflaton are kinematically allowed, loop corrections
to the propagators are real, and they are absorbed into the renormalized masses and couplings, order by order in
perturbationtheory. Onthe otherhand, whenthe inflaton(orthe fields coupledto the inflaton) candecayinto other
4 Correctionstothisestimationappearforsmallvaluesofκ<0.01,forwhichxN O(1).
5 From the WMAP data only, the best fit value without running of the spectr∼al index is nS = 0.99 0.04. A recent analysis of
±
the combined Lyman-α forest spectra + WMAP [22] also gives nS = 0.99 0.03 with no running, and nS = 0.959 0.036 with
± ±
dnS/dlnk= 0.033 0.025. However,asimilaranalysisinRef. [23]givesnS =0.98 0.02withdnS/dlnk= 0.003 0.01.
− ± ± − ±
4
particles, the propagators in the loop have the standard Breit-Wigner form, with an imaginary contribution related
to the decay rate Γ. Therefore, when computing the 1-loop effective potential for the inflaton field, the contributions
associated to the decay rate lead to dissipative effects [6, 8]. In general this reflects itself in the form of temporally
nonlocal terms in the inflaton evolution equation. Under certain approximations this translate into a simple effective
friction term Υ in the equation of motion for the background inflaton field [6, 8],
S
φ¨ +(3H +Υ )φ˙ +∆V′ =0. (11)
S S S
The emergence of this friction term due to these underlying decay channels implies the dynamics of the system is
suchthat partofthe inflaton energyis dissipated into the lighter particlesproduced inthe decays,i.e., into radiation
ρ , with
R
ρ˙ +4Hρ =Υ φ˙2 . (12)
R R S S
Although the basic idea of interactions leading to dissipative effects during inflation is generally valid, the above set
of equationshas strictly been derivedin [6, 8] only in the adiabatic-Markovianlimit, i.e., when the fields involvedare
moving slowly, which requires
φ˙
S
<H <Γ, (13)
φ
S
with Γ being the decay rate. The secondinequality,H <Γ is alsothe condition for the radiation(decay products)to
thermalize.
Thus in general any inflation model could have two very distinct types of inflationary dynamics, which have
been termed cold and warm [8, 9]. The cold inflationary regime is synonymous with the standard inflation picture
[10, 11, 12], in which dissipative effects are completely ignoredduring the inflation period. On the other hand, in the
warminflationaryregimedissipativeeffectsplayasignificantroleinthedynamicsofthesystem. Aroughquantitative
1/4 1/4 1/4 <
measure that divides these two regimes is ρ H, where ρ > H is the warm inflation regime and ρ H
R ≈ R R ∼
is the cold inflation regime. This criteria is independent of thermalization, but if such were to occur, one sees this
criteria basically amounts to the warm inflation regime corresponding to when T > H. This is easy to understand
since the typical inflaton mass during inflation is m H and so when T > H, thermal fluctuations of the inflaton
φ
≈
field will become important. This criteria for entering the warm inflation regime turns out to require the dissipation
of a very tiny fraction of the inflaton vacuum energy during inflation. For example, for inflation with vacuum (i.e.
potential)energyattheGUTscale 1015−16GeV,inordertoproduceradiationatthescaleoftheHubbleparameter,
which is 1010−11GeV, it just req∼uires dissipating one part in 1020 of this vacuum energy density into radiation.
≈
Thus energetically not a very significant amount of radiation production is required to move into the warm inflation
regime. In fact the levels are so small, and their eventual effects on density perturbations and inflaton evolution are
so significant, that care must be taken to account for these effects in the analysis of any inflation models.
The conditions for slow-rollinflation (φ˙2 V, φ¨ Hφ˙ ) are modified in the presence of the extra friction term
S ≪ S ≪ S
Υ , and we have now:
S
ǫ
H
ǫ = , (14)
Υ (1+r)2
η
H
η = , (15)
Υ (1+r)2
wherer =Υ /(3H),andǫ ,η aretheslow-rollparameterswithoutdissipationgiveninEqs. (5)and(6). Inaddition,
S H H
when the friction term Υ depends on the value of the inflaton field, we can define a third slow-roll parameter
S
r
ǫ = β , (16)
HΥ (1+r)3 Υ
with
V′ Υ′
β = S . (17)
Υ 3H2Υ
S
Similarly to the slow-rollregime without dissipation, when η <1, ǫ <1, and ǫ <1, Eqs. (11) and (12) are well
Υ Υ HΥ
approximated by:
∆V′ 1
φ˙ , (18)
S
≃ − 3H 1+r
Υ 1 r
ρ Sφ˙2 ǫ V , (19)
R ≃ 4H S ≃ 2(1+r)2 H
5
and the number of e-folds is given by:
φSe 3H2
N (1+r)dφ. (20)
e ≃− ∆V′
ZφSi
Obviously, when Υ 1 we recover the standard “cold” hybrid inflation (CHI) scenario.
S
≪
The effect of the dissipative term is twofold: on one hand, dissipation of the vacuum energy into radiation acts
as an extra friction term and slows down the motion of the inflaton field, so that inflation last longer. That means
that when Υ is non negligible,we wouldrequirein generalsmaller initial values of the inflatonfield in orderto have
S
“enough” (at least 60 e-folds) inflation, Eq. (20). On the other hand, fluctuations in the radiation backgroundaffect
those of the inflaton field through the interactions, and this in turn will affect the primordial spectrum generated
during inflation. Approximately, one can say that when T > H the fluctuations of the inflaton field are induced by
the thermal fluctuations, instead of being vacuum fluctuations, with a spectrum proportional to the temperature of
the thermal bath. We notice that having T > H does not necessarily require Υ > 3H. Dissipation may not be
S
strongenoughtoalterthedynamicsofthe backgroundinflatonfield, butitcanbe enougheveninthe weakregimeto
affect its fluctuations, and therefore the spectrum. Depending on the different regimes, the spectrum of the inflaton
fluctuations P1/2 is given for cold inflation [24], weak dissipative warm inflation [25, 26] and strong dissipative warm
δφ
inflation [27] respectively by
H
1/2
T <H : P , (21)
δφ |T=0 ≃ 2π
T
Υ <H <T : P1/2 √TH P1/2 , (22)
S δφ |T ≃ ∼ H δφ |T=0
r
1/4 1/4
πΥ πΥ T
Υ >H : P1/2 S √TH S P1/2 , , (23)
S δφ |Υ ≃ 4H ∼ 4H H δφ |T=0
(cid:18) (cid:19) (cid:18) (cid:19) r
with the amplitude of the primordial spectrum of the curvature perturbation given by:
H 3H2
P1/2 = P1/2 (1+r)P1/2. (24)
R φ˙ δφ ≃ ∆V′ δφ
(cid:12) S(cid:12) (cid:12) (cid:12)
(cid:12) (cid:12) (cid:12) (cid:12)
(cid:12) (cid:12) (cid:12) (cid:12)
Giventhe different“thermal”originofspectru(cid:12)m, t(cid:12)he spectr(cid:12)alind(cid:12)ex alsochangeswithrespectto the coldinflationary
scenario[28, 29, 30, 31], even in the weak dissipative warminflation regime when the evolutionof the inflaton field is
practically unchanged. Again, for the different regimes, it is obtained:
T <H : n 1= 6ǫ +2η , (25)
S H H
− −
17 3 1
Υ <H <T : n 1= ǫ + η β , (26)
S S H H Υ
− − 4 2 − 4
9 3 9 1
Υ >H : n 1=( ǫ + η β ) . (27)
S S H H Υ
− −4 2 − 4 (1+r)
In the latter case there could be appreciable departures from scale invariance in the spectrum; we notice again than
in the strong dissipative case, slow-roll only demands ǫ (1+r)2 and η (1+r)2, whereas the spectral index
H H
≪ ≪
depends on the ratios ǫ /(1+r) and η /(1+r), which not necessarily are much smaller than 1.
H H
The question then is not whether there is dissipation during inflation, but whether this will affect the inflationary
predictions. First, how large can Υ be in a realistic set-up. In the calculations in [6, 7, 8] a robust mechanism for
S
dissipation during inflation has been identified. The basic interaction structure for this mechanism is
1
= g2φ2χ2 g′φψ¯ ψ hχψ¯ ψ , (28)
I χ χ d d
L −2 − −
where φ is the inflaton field, χ and ψ are additional fields to which the inflaton couples, and ψ are light fermions
χ d
into which the scalar χ-particles can decay m > 2m . This interaction structure can be identified in both models
χ ψd
we are studying in this paper Eqs. (1) and (2). In the next two subsections, the dissipative properties of these two
models will be computed based on the results on [6, 8] and then the effect of this dissipation to inflation will be
studied.
6
A. Decay into massive fermions:
First consider the model Eq. (1), which has only the minimal matter content. In this model, the scalar with the
largest mass m can decay into its fermionic superpartner Φ˜ and a massless inflatino, with decay rate6:
+ +
κ2 1 2
Γ = m , (29)
+ 16π + x2 +1
(cid:18) N (cid:19)
where again x is the value of the inflaton field (normalized by µ) N efolds before the end of inflation. This decay
N e
rate is always smaller than the rate of expansion during inflation:
Γ κ2 m /µ
+ =√3 P 1, (30)
H 16π(x2 +1)3/2 ≪
N
and strictly speaking the adiabatic-Markovian approximation would not apply. Nevertheless, in order to get some
numbers, let us proceedand estimate the dissipative coefficientand the amountof radiationproduced. The formeris
given by:
√2(κ4/4)(Γ /m ) φ2
Υ (φ ) = + + S
S S
m
64π 1+(Γ /m )2 1+(Γ /m )2+1 +
+ + + +
π3 pκ 5 x2 qp π3 κ 5 µ
N µ , (31)
≃ 2 4π (x2 +1)5/2 ≃ 2 4π x3
N N
(cid:16) (cid:17) (cid:16) (cid:17)
which is always suppressed with respect to the expansion rate during inflation, H κµ2/(√3m ):
P
≃
Υ π2 κ 4 m x2
S P N 1. (32)
3H ≃ 8√3 4π µ (x2 +1)5/2 ≪
N
(cid:16) (cid:17)
Nevertheless,theamountof“radiation”produced,i.e.,theenergydensitydissipatedfromtheinflaton,couldbelarger
than H4,
ρ 9Υ m4 9 κ 6 m 7 x2
R Sǫ P P N F [x ]2. (33)
H4 ≃ 23H Hκ2µ4 ≃ 256√3 4π µ (x2 +1)5/2 1 N
(cid:16) (cid:17) (cid:18) (cid:19) N
Given that the ratio ρ /H4 goes like the inverse of x5 , the ratio increases as the value of the inflaton field decreases
R N
during inflation. However, it only becomes larger than one for κ 0.1 toward the end of inflation, well after the 60
∼
e-foldsbeforetheend. Wecanconcludethenthatdissipationinthisexampleistooweaktoaffecteitherthespectrum
of the primordial perturbations or the dynamics of the inflaton field.
B. Decay into massless fermions:
As we have seen, dissipation through the decay into massive fermions does not have much effect during inflation.
However, in more realistic models, one would expect the presence of other fields, which in principle are not directly
relevant during inflation but can play a rˆole during/after reheating. For example, fields coupled to either Φ or Φ
1 2
are massless during inflation, and become massive at the global minimum. Thus the model Eq. (2), where we have
introduced a pair of matter fields, ∆ and ∆¯, coupled to Φ . Because they are massless during inflation, they do not
2
contribute to the 1-loop effective potential, and radiative corrections are the same as in the previous case, with the
slope and curvature of the effective potential given by Eqs. (3) and (4). But now the heaviest field with mass m
+
can decay into the massless fermionic partners of ∆ and ∆¯, with decay rate:
g2
Γ = m . (34)
+ +
16π
6 TheinteractionLagrangianisgivenby = (κ/√2)φ+S¯˜Φ˜+.
L −
7
Since nowthereisnophasespacesuppressionfactorinthe decayrate,wehaveΓ φ , andthis canbe muchlarger
+ S
∝
than the Hubble rate during inflation:
Γ g2 m
+ =√3 P (x2 +1)1/2. (35)
H 16π µ N
(cid:18) (cid:19)
Having Γ /H >1, all the way up to the end of inflation, only requiresg >0.16for κ<0.001 ( g >0.01 for κ=0.5).
+
This allows us to apply the adiabatic-Markovianlimit in the effective equation of motion for the inflaton background
field, Eq. (11), with the dissipative coefficient given now by:
π2 κ 3 g2 x2
Υ N µ, (36)
S ≃ 2 4π 16π (1+x2 )1/2
(cid:16) (cid:17) (cid:18) (cid:19) N
and the ratio to the Hubble rate is given by:
Υ κ2 g2 x2 m
S N P , (37)
3H ≃ 128√3π 16π (1+x2 )1/2 µ
(cid:18) (cid:19) N
which behaves like Υ /(3H) x φ , and so decreases during inflation. That is, the evolution of the inflaton
S N S
∝ ∝
fieldmaychangefrombeing dominatedby the frictiontermΥ to be dominatedbythe Hubble rateH. Whether the
S
transitionbetween these two regimes happens before or after 60 e-folds will depend on the value of the parametersof
the model like κ and g. The amount of “radiation” obtained through the dissipative term, is given by:
ρ 9 r m4
R ǫ P , (38)
H4 ≃ 2(1+r)2 Hκ2µ4
which even when Υ <H could give rise to a thermal bath with T >H. In particular, we can have:
S
(a) Υ >3H, and T >H (φ˙ V /Υ ):
S S φ S
≃−
ρ 36√3 1 m 5 1
R P
, (39)
H4 ≃ π2 g2 µ x3
(cid:18) (cid:19) N
(b) Υ <H (φ˙ V /(3H)):
S S φ
≃−
ρ 9 κ 4 g2 m 7 1
R P
. (40)
H4 ≃ 256√3π (cid:16)4π(cid:17) (cid:18)16π(cid:19)(cid:18) µ (cid:19) xN
The values of the couplings κ and g for which we could havecold or warminflation, and strongor weak dissipative
dynamics, are plotted in Fig. (1). In order to get the different regions, we have proceeded as follow: for each pair of
values in the plane κ g, the value of the inflaton field at the end of inflation is determined. This is done in the cold
and weak dissipative−regimes by the condition7 η = 1, Eq.(15). In the strong dissipative regime inflation can end
Υ
either with η =1 or itmay alsohappen thatmost ofthe vacuumenergyis alreadytransferredinto radiationduring
Υ
inflation, and then inflation will end when ρ κ2µ4 instead. In this case, whichever occurs first fixes the value of
R
≃
the inflaton field atthe end of inflation. The value of the inflaton field at 60 e-folds of inflation is then obtained from
Eq. (20). This in turn fixes the value of the dissipative coefficient Υ , Eq. (36), the temperature of thermal bath,
S
Eq. (38), and therefore the amplitude of the spectrum Eq. (24). The COBE normalization is then used to fix the
value of the scale µ. In order to match the expressions for the spectrum across the different regimes, we have used a
simple expression with :
3H2 T πΥ 1/4 H
P1/2 = (1+r) 1+ 1+ S . (41)
R ∆V′ H 4H 2π
(cid:12) (cid:12) r ! (cid:18) (cid:19) !(cid:18) (cid:19)
(cid:12) (cid:12)
(cid:12) (cid:12)
We can see in Fig. (1) that the s(cid:12)trong(cid:12)dissipative regime Υ >3H requires large values of the couplings, κ g
S
∼ ∼
O(1); for values κ g 0.1 we are in the weak dissipative regime; and for values κ g 0.01 we recover the cold
≃ ≃ ≃ ≃
inflationaryscenario. Typically,forafixedvalueofthescaleµtheamplitudeofthespectruminthestrongdissipative
7 ThevalueofηΥ becomes largerthan1beforetheothertwoslow-rollparameters.
8
1
µ=0.001 m Υ> 3H
P
T>H
0.1 Γ=H
g
µ=0.0015 m
0.01 P
T<H
0.001 a
r
g
µ=0.002 m u
P S
0.0001
0.0001 0.001 0.01 0.1 1
κ
FIG. 1: Regions of cold (T <H),and warm (T >H)SUSYhybrid inflation in theκ−g plane. The warm inflation region is
divided into the weak dissipative regime with T >H and ΥS <3H (lighter shaded region), and the strong dissipative regime
with ΥS > 3H (darker shaded region). Included are also the contour plots of constant µ, and the adiabatic-Markovian limit
Γ+ = H. The black region on the right of the plot is excluded because φS >mP. In addition, when SUGRA corrections are
taking into account, valuesto theleft and down thewide dot-dashed line are excluded.
regime would be larger than the one generated at zero T. The COBE normalization implies then a smaller value of
the inflationary scale µ. For example, for κ = g = 1 we have µ 1013 GeV, whereas pushing the coupling toward
its perturbative limit, κ =g =√4π we would get µ 2 1010 G≃eV. On the other hand, going from the cold to the
≃ ×
weak dissipative regime, the value of µ only varies by a factor of 2 or 3, and it is still in the range of the GUT scale
O(1015) GeV.
As mentioned before, the quartic term in the inflaton potential induced by SUGRA corrections becomes non
negligible for not very small values of κ. In the CHI scenario, the value of the inflaton field becomes larger than
m for κ 0.15, and consequently that region is excluded. The same constraint applies also in the weak dissipative
P
≥
scenario. However, in the strong dissipative regime, with Υ > 3H, the extra friction term keeps the value of the
S
inflaton field below the Planck scale, and the constraint on κ can be avoided.
In Fig. (2) we have comparedthe prediction for the spectral index of the scalar spectrum of perturbations in both
the CHIscenario,andwarmhybridinflation(WHI).Fromthe warminflationscenariowecanalwaysrecoverthe CHI
predictionby takingg 1. InstandardSUSY GUT hybridinflation, forsmallvalues ofthe couplingκ the spectrum
≪
is practically scale invariant, it reaches a minimum around κ 0.01, and then rises due to SUGRA corrections up
≃
to positive values, which are disfavoured by WMAP results. But in the weak and the strong dissipative regime, due
to the different origin of the spectrum, we get that the spectral index is still below 1 even for values of the coupling
κ>0.01. This is especially true in the strong dissipative regime, where the dynamic is such that the inflaton field is
wellbelowthePlanckscaleandSUGRAcorrectionsarenegligible. Inthatregimethe departurefromscaleinvariance
is within the observational value, with n 1 0.022.
S
− ≃−
In Fig. (3) we have also compared the running of the spectral index, dn /dlnk in both scenarios. The running
S
although negative is much smaller than the value preferred by the WMAP data, dn /dlnk 0.031+0.016. Again,
S ≃ − −0.015
in the strong dissipative regime we can have largervalues of the couplings κ and g compatible with observations,but
the predicted running of the spectral index is still small, with dn /dlnk 4 10−4. Nevertheless, it is not yet
S
≃ − ×
clear the statistical relevance of this result, which in any case would be finally confirmed or excluded by the Planck
Satellite experiment.
Concerning the primordial spectrum of tensor perturbations, as they do not couple strongly to the thermal back-
ground, the amplitude is the same than in CHI, with
2
2 H
P = . (42)
tensor m2 2π
P (cid:18) (cid:19)
9
0.03
WHI: T>H, Y < 3H
S
0.02 WHI: Y > 3H
S
CHI
0.01
1
− 0
S WHI
n
−0.01
−0.02
10−5 10−4 10−3 10−2 10−1 100
κ
FIG. 2: Spectral index for cold SUSY hybrid inflation (solid line, CHI), and warm inflation (gray region, WHI). The weak
dissipative regime (T > H but ΥS < 3H) is given by the darker gray region (triangle down);the strong dissipative regime
(ΥS >3H) is given bythe light gray region (triangle up).
0
CHI
WHI
WHI
−0.0005
k WHI: T> H, Y < 3H
n S
dl WHI: Y > 3H
/ S
S
n
d
−0.001
10−5 10−4 10−3 κ10−2 10−1 100
FIG.3: RunningofthespectralindexforcoldSUSYhybridinflation(solidline,CHI),andwarmhybridinflation(grayregion,
WHI). The weak dissipative regime (T > H but ΥS < 3H) is given by the darker gray region (triangle down); the strong
dissipative regime (ΥS >3H) is given bythe light gray region (triangle up).
As we have seen, strong dissipation (κ O(1)) translates into a smaller inflationary scale µ compared to that of
∼
standard CHI, therefore a lower value of H and a smaller contribution of the gravitational waves to the spectrum.
However,thesamelevelofprimordialtensorperturbationscanbeobtaineddecreasingthevalueofκandnodissipation.
This can be seen in Fig. (4), where we have plotted the prediction for the tensor-to-scalarratio, defined as
P
tensor
R = , (43)
g
P
R
versusthe predictionfor the scalarspectralindexn 1,for the differentregimes(cold, weakdissipation,andstrong
S
−
dissipation). The smallest values of κ correspond to a practically scale invariant spectrum. At present, from the
10
10−5
10−6 T<H
10−7
10−8
10−9 WHI: T>H, YS<3H
Rg10−10
10−11
10−12
10−13
WHI: Y >3H
S
10−14
10−15
−0.03 −0.02 −0.01 0 0.01 0.02 0.03
n −1
S
FIG.4: Tensor-to-scalarratioversusthepredictedscalar spectralindexnS−1. Thecold regime,T <H,isgivenbythedark
grey areas; the weak dissipative regime, T >H but ΥS <3H, is given by the striped area; and the strong dissipative regime,
ΥS >3H,is given by thelight gray region.
Cosmic Microwave Background polarization measurements the tensor-to-scalarratio is poorly constraint (R <0.4),
g
although in the future ratios as low as 10−6 could be probed [32]. Still, such a gravitational background can be
achieved(but notlarger)inthiskindofmodels onlyinthe coldorweakdissipativeregime,andtypicallyforvaluesof
the coupling κ close to the maximum allowed by SUGRA corrections (blue tilted spectrum). On the other hand, in
thestrongdissipativeregimeweobtainaclearpredictionthatdistinguishesthisregimesfromtheothers: noexpected
tensor signal, with R <10−9, and a red tilted spectrum with n 0.98.
g S
≃
IV. REHEATING TEMPERATURE
One of the main constraints on model building of inflationary supersymmetric particle physics models comes from
the gravitino constraint on the reheating T after inflation. Gravitinos with a typical mass of the order of O(1 100)
−
TeVcanbethermallyproducedduringtheradiationdominatederathatfollowsinflation. IfT istoohigh,wewillhave
too many of them, and their subsequent decay will interfere with the predictions of the abundances of light elements
at the time of big bang nucleosyntheses (BBN) [33]. This puts an upper bound onthe reheatingT typically of the
RH
order of 109 GeV [33], and a more recent analysis on BBN has lowered this bound to T < 107GeV for a gravitino
RH
∼
mass m O(1) TeV [34, 35]. In cold inflation, the reheating T after inflation can be well approximated by:
3/2
≃
1/4
90
T Γ m , (44)
RH ≃ π2g φ P
(cid:18) ∗(cid:19)
p
where Γ is the decay rate of the inflaton field, and g the effective number of degrees of freedom (typically of the
φ ∗
order of O(100) in a SUSY model). Therefore, the reheating constraint translates in the inflaton not decaying too
fast after inflation, which may implies some further constraint on the couplings8.
In this letter we have just minimally extended the inflationary sector by adding a pair of extra matter fields ∆,
∆¯, with generic coupling g. This allows the decay of the Φ fields already during inflation, and the possibility of
i
having a warm regime of hybrid inflation, when the couplings are not very small, say κ,g > 0.1. The question then
is whether this large coupling g could give rise to a large decay rate, and therefore a too large T . From the S, Φ
RH i
sector we would have scalars and pseudoscalars with masses m = √2κµ (plus a massless state if the minimum is
S
8 Thiscanbeavoidedifthegravitinoabundance isdilutedbytheentropyproducedduringthelate-decay ofsomeotherparticle[36].