1 Introduction

Starobinsky-like inflation and soft-SUSY breaking

[12mm] Stephen F. King111E-mail: king@soton.ac.uk, Elena Perdomo222E-mail: e.perdomo-mendez@soton.ac.uk

[-2mm]

School of Physics and Astronomy, University of Southampton,

SO17 1BJ Southampton, United Kingdom

We study a version of Starobinsky-like inflation in no-scale supergravity (SUGRA) where a Polonyi term in the hidden sector breaks supersymmetry (SUSY) after inflation, providing a link between the gravitino mass and inflation. We extend the theory to the visible sector and calculate the soft-SUSY breaking parameters depending on the modular weights in the superpotential and choice of Kähler potential. We are led to either no-scale SUGRA or pure gravity mediated SUSY breaking patterns, but with inflationary constraints on the Polonyi term setting a strict upper bound on the gravitino mass TeV. Since gaugino masses are significantly lighter than , this suggests that SUSY may be discovered at the LHC or FCC.

## 1 Introduction

Inflation [1, 2, 3, 4, 5, 6] is well known to solve the flatness and horizon problems, diluting cosmological relics and providing an origin of cosmological fluctuations. In slow-roll inflation [7, 8], the inflaton rolls along a quite flat potential and inflation end as it falls into some basin. Inflation is supported and constrained by current observational data [9], which measures a spectral index and low tensor-to-scalar ratio , excluding the simplest chaotic models based on polynomial potentials such as or [10]. Surviving models include Starobinsky inflation [11], Higgs inflation [12] and related models [13], and low scale hybrid inflation [14].

Supersymmetry (SUSY) may be naturally combined with inflation since it allows better control over the high energy dynamics of scalars [16, 15, 17]. SUSY inflation is also motivated by the Lyth bound [18] on the low tensor-to-scalar ratio, which prefers a scale of inflation below the Planck scale. Since inflation is sensitive to UV scales, it is necessary to consider supergravity (SUGRA) inflation, as in e.g. [19, 20, 21]. In no-scale SUGRA [22], the Kähler potential takes a logarithmic form which circumvents the problem. Alternatives to no-scale SUGRA have also been proposed which also address the problem based on a Heisenberg symmetry [23, 24] or a shift symmetry [25, 26, 27] (see also [28]).

It has been shown by Ellis, Nanopoulos, Olive (ENO) that no-scale SUGRA can behave like a Starobinsky inflationary model [29, 30, 31]. However, in this approach, a term with constant modular weight is used to break SUSY, and there is no connection between inflation and SUSY breaking. Recently we considered the above ENO model, but with a linear Polonyi term added to the superpotential [32]. The purpose of adding this term was to provide an explicit mechanism for breaking SUSY in order to provide a link between inflation and SUSY breaking. Indeed we showed that inflation requires a strict upper bound for the gravitino mass TeV [32].

In the present paper we show how the Polonyi-extended ENO model may be generalised to include the fields in the visible sector of the minimal supersymmetric standard model (MSSM). Such a generalisation has been done for the ENO model [29, 30, 31] and we perform a similar analysis for the Polonyi-extended ENO model. We calculate the soft-SUSY breaking parameters depending on the modular weights in the superpotential and choice of Kähler potential and we are led to new phenomenological possibilities for supersymmetry (SUSY) breaking, based on generalisations of no-scale SUSY breaking and pure gravity mediated SUSY breaking. The Polonyi-extended ENO model is especially interesting to consider because of the upper bound on the gravitino mass discussed in the previous paragraph which allows the much lighter gauginos to be discovered in future collider experiments. This motivates the present investigation of the soft SUSY breaking parameters, which could form the basis for future phenomenological studies.

The layout of the remainder of the paper is as follows. In section 2 we discuss the hidden sector of the supergravity theory where inflation takes place. In section 3 we discuss the visible sector of the supergravity theory and show how the MSSM matter and Higgs fields may be included. In section 4 we discuss the supergravity scalar potential, showing how inflation emerges from the hidden sector and soft-SUSY breaking parameters emerge from the full theory including the visible sector, leading to new examples of no-scale SUSY breaking and pure gravity mediated SUSY breaking. Section 5 concludes the paper.

## 2 The Hidden Sector

In general supergravity theory, the tree-level supergravity scalar potential can be found using the Kähler function , which is given in terms of the Kähler potential and the superpotential as,

 G=KM2P+ln|WM3P|+ln|WM3P|∗. (1)

The effective scalar potential is then given by,

 V=eG[∂G∂ϕiKij∗∂G∂ϕj∗−3]M4P, (2)

where is the inverse of the Kähler metric . When, at the minimum of the scalar potential, some of the hidden sector fields acquire VEVs in such a way that at least one of their auxiliary fields, , is non-vanishing, then SUSY is spontaneously broken and soft SUSY-breaking terms are generated in the observable sector. The gravitino becomes massive and its mass

 m23/2=eG=eK/M2P|W|2M4P (3)

sets the overall scale of the soft parameters. In general, the Kähler potential and the superpotential involve superfields in the hidden and visible sectors. The hidden sector superfields are gauge singlets and do not have Yukawa couplings to the charged fields in the visible sector, coupling only indirectly to them via Planck suppressed operators.

The simplest no-scale Kähler potential in the hidden sector is given by two complex fields , where T is a modulus field while is the field responsible for inflation and SUSY breaking. The Kähler potential in the hidden sector takes the form

 Khid(ϕ,T)=−3M2Pln(T+T∗MP−|ϕ|23M2P), (4)

where is the reduced Planck scale.

It was found in [29] this Kähler potential together with the Wess-Zumino superpotential [33, 34] can lead to the Starobinsky-like inflationary potential. When the modulus field is fixed with a vacuum expectation value of and , the no-scale Kähler potential together with the Wess-Zumino superpotential is equivalent of an model of gravity, in which Starobinsky inflation emerges at a particular point in parameter space [30]. A simple modification to this superpotential has been done in [32], adding the Polonyi term to provide an explicit and simple mechanism for supersymmetry breaking at the end of inflation. The Wess-Zumino superpotential [33] in the hidden sector, with quadratic and trilinear terms, together with a linear Polonyi term looks like

 Whid(ϕ)=m2ϕ+μ2ϕ2−λ3ϕ3. (5)

In the following, it is convenient to introduce the change of variables [35]

 T=MP2⎛⎜⎝1−y2√3MP1+y2√3MP⎞⎟⎠,ϕ=⎛⎜⎝y11+y2√3MP⎞⎟⎠, (6)

with the inverse relations

 y1=(2ϕ1+2T/MP),y2=√3MP(1−2T/MP1+2T/MP). (7)

After this change of variables, the hidden sector superpotential becomes

 Whid(y1,y2)=(1+y2√3MP)−3˜Whid(y1,y2), (8)

where the rescaled superpotential is

 ˜Whid(y1,y2)=m2y1(1+y2√3MP)2+μ2y21(1+y2√3MP)−λ3y31. (9)

The Kähler potential in the hidden sector becomes

 Khid(y1,y2)=˜Khid(y1,y2)+3ln(|1+y2√3MP|2) (10)

where

 ˜Khid(y1,y2)=−3M2Pln(1−|y1|2+|y2|23M2P), (11)

Note that the combination of and is equivalent to using and , since the physical quantities are given by the Kähler function  1 which is the same in both cases (the extra term in the Kähler potential cancels with an opposite term coming from the superpotential). Therefore, we use the symmetric representation of the Kähler in Eq. 11 and the rescaled superpotential in Eq.9 in the following.

This superpotential can reproduce the Starobinsky model for the real part of and fixed , when a suitable stabilizing term is added to the no-scale Kähler potential [30, 35, 36]:

 ˜Khid(y1,y2)=−3M2Pln(1−|y1|2+|y2|23M2P+|y2|4Λ2M2P), (12)

with , as discussed in [30]. In section 3, we ignore the term for simplicity, but it should be kept in mind that it is necessary to stabilize the field .

The exact Starobinsky potential is obtained when dropping the Polonyi term, , fixing and using the relationship [30]. To quantify how much the Starobinsky limit deviates when including the Polonyi term, we use the parameter while keeping the relation , which gives

 μ−1˜Whid(y1,y2)=√3bMPy1(1+y2√3MP)2+y212(1+y2√3MP)−y313√3MP. (13)

For non-zero , SUSY is broken and the gravitino mass in Eq.3 becomes non-zero at the end of inflation, as was shown in [32]. As discussed in [32], there is an upper limit on the parameter in order to have a viable inflationary scenario, suggesting a gravitino mass TeV with favoured values of TeV. A more quantitative discussion (which we do not repeat here) can be found in [32], where it is shown that this limit comes from the two crucial dimensionless observables: the tensor-to-scalar ratio, , and the scalar tilt, , given by the Planck satellite [9]. Furthermore, the scalar amplitude observable, , is sensitive to the overall scale of the potential, to the parameter in Eq. 13. It is shown there [32] that, in the Starobinsky limit when , the bilinear mass term parameter becomes and we use these values in the following computations.

## 3 The Visible Sector

We now extend the hidden sector inflation model in the previous section to include the matter fields in the visible sector, such as those of the minimal supersymmetric standard model (MSSM), which includes the Standard Model (SM) quarks and leptons together with their supersymmetric partners, written generically in terms of matter and Higgs superfields . The visible sector superfields carry gauge charges under the SM gauge group, unlike the hidden sector supefields which are gauge singlets. We consider two possibilities for extending the hidden sector supergravity theory of the previous section to include such visible sector superfields.

Motivated by the no-scale approach [37], the first possibility (Case I) is to embed the visible sector matter superfields within the logarithm in the Kähler potential (Case I), such that

 KI=−3M2Pln(1−|y1|2+|y2|2+|yvis|23M2P),Case I. (14)

Another possibility (Case II) we also explore is to have the visible sector superfields outside the logarithm in the Kähler potential via minimal kinetic terms

 KII=−3M2Pln(1−|y1|2+|y2|23M2P)+|yvis|2,Case II. (15)

Furthermore, in the same spirit as in [31], we assume that the superpotential for the visible sector superfields has the form

 Wvis=W2(yvis)(1+y2√3MP)β+W3(yvis)(1+y2√3MP)α, (16)

where and are modular weights and are bi/trilinear parts of the superpotential of the MSSM in terms of the visible sector superfields . The total superpotential is then given by

 W=˜Whid+Wvis, (17)

where was given in Eq.13 and is given in Eq.16.

We want to make the connection between the Wess-Zumino-Polonyi superpotential 13, which has a parameter space in which the Starobinsky inflation is recovered, and the soft supersymmetry-breaking parameters after the MSSM superfields are included. The main difference between the model of [32] which we are developing here, and that proposed in [31] is that, in the present case, supersymmetry is broken through the Polonyi term while in [31] a term with constant modular weight 3 term was used to break SUSY. In the present model there is a constraint from inflation in how big the parameter (accounting for the Polonyi term) can be, leading to an upper bound on the gravitino mass, which sets the SUSY breaking scale. The present model therefore suggests a more constrained region of parameter space which may be confronted with LHC, Higgs and dark matter constraints.

The main difference between the two cases I and II is that in the pure no-scale case 14, the soft supersymmetry-breaking mass squared is zero while in the latter case 15, is different from zero and equal to the gravitino mass, as we will show in section 4.

## 4 Potential and soft-SUSY breaking parameters

We can compute the supergravity scalar potential from Eqs. 1 and 2, using either Eq.14 (case I) or Eq.15 (case II), with the total superpotential in Eq.17. At the minimum of the potential some of the hidden sector fields, and , acquire VEVs such that the F term is non-vanishing, then supersymmetry is spontaneously broken and soft supersymmetry-breaking terms are generated in the observable sector, . This is just the usual gravity mediated SUSY breaking mechanism. However the special forms of superpotential and Kähler potential here lead to a special form of SUSY breaking, referred to as either no-scale SUSY breaking (case I) or pure gravity mediated SUSY breaking (case II).

### 4.1 Hidden sector potential and inflation

We begin by computing the supergravity scalar potential from Eqs. 1 and 2, in the hidden sector using  13 and  11 only. We follow the same treatment as in [29] and assume that the field is fixed with a vacuum expectation value of and , corresponding to 333The modulus field is stabilized when including a term as in Eq. 12, for a better understanding see [30].. The minimum of the potential is always given by , for both cases I and II, is found for

 y1=√32(1±√1+4b)MP, (18)

such that supersymmetry is spontaneously broken in the hidden sector. For , only if we have the minus sign and we restrict ourselves to this case in the following. This model reproduces the effective potential of the Starobinsky model for . The dynamical field can be converted into a canonically-normalized inflaton field by the transformation [29, 30]

 y1=±√3MPtanh(χ√3MP)=±√3MPtanh(x√6MP), (19)

where and the latter equality holds for . The imaginary part of the inflaton is fixed to by the potential [29, 32] since the potential is always minimized by in the range of interest of the inflaton field . We use the positive sign in Eq. 19 and write the potential in terms of the inflaton field

 V=34μ2M2P[1+b+(b−1)cosh(√23x√MP)+sinh(√23x√MP)]2, (20)

where we have fixed . In terms of the inflaton field , the minimum of the potential is found for

 x0=√6MPtanh−1(12(1−√1+4b)). (21)

The exact Starobinsky limit is realized for , while small values for represents a small deviation from the Starobinsky limit as shown in Fig. 1.

As deviates from zero, the value of the field at the global minimum shifts away from zero, while maintaining . Although the scalar potential vanishes, the superpotential and the Kähler function is different from zero, generating explicit soft supersymmetry-breaking terms of the required form in the effective low-energy Lagrangian. The gravitino becomes massive, see Eq. 3, and sets the overall scale of the soft parameters

 m3/2=−32μb2+O(b3), (22)

where we have expanded at lowest order in . The exact analytical expression can be found in Appendix A.

As explained in [32], the limits from inflation suggest that the parameters GeV and . For fixed (where is the value of the field when inflation starts) we see that there is an approximate quadratic dependence of the gravitino mass on the parameter , as shown in Fig. 2, where we have rescaled the results around the origin as in [32]. For , we see that , so supersymmetry is unbroken and we are left with the Wess-Zumino superpotential limit leading to Starobinsky inflation. However, from Fig. 1, we see that for small values of , the potential retains a plateau where inflation will happen and the corresponding limit on the gravitino mass may be read off from Fig. 2 as TeV.

### 4.2 Visible sector potential and SUSY breaking

We now compute the supergravity scalar potential from Eqs. 1 and 2, including the visible sector superfields, using either Eq.14 (case I) or Eq.15 (case II), with the total superpotential in Eq.17. With the addition of the visible sector superpotential in Eq. 16, we are now able to compute the soft supersymmetry breaking mass-squared, bilinear, and trilinear parameters, respectively.

#### 4.2.1 Case I: no-scale SUSY breaking

For the Case I, where the SM superfields are inside the Log of the Kähler potential, the soft supersymmetry breaking parameters become

 m0=0,A0m3/2=−6α−3(4+α)b2+O(b3), Case I B0m3/2=2(1−β)−(1+β)b2+O(b3). (23)

The prediction for is the familiar result of no-scale SUSY breaking. The exact analytical functions are given in Appendix A, while the expressions in Eq. 23 are found when expanding in powers of and hold for our range of interest . The mass-squared term is zero while the bilinear and trilinear parameters will depend on the choice of the modular weights and , as shown in Fig. 3. The main effect of switching on is to increase the gravitino mass, since the terms proportional to are negligible. The special choice of and , corresponds to the pure no-scale option where for , in which case the supersymmetry breaking in the low scale energy can be produced via a non-minimal gauge kinetic term generating non-zero gaugino masses .

For the rest of cases, where and , we can set some limits in the bilinear and trilinear couplings due to the constraint on the parameter coming from inflation such that TeV and TeV. We assume the condition to avoid constraints from Big Bang nucleosynthesis on gravitino decays. In this case, we cannot find a viable phenomenological region due to the relation between the trilinear coupling and the gravitino mass in Eq. 23, implying which leads to tachyonic sfermion masses. Furthermore, for , there is no value of which minimizes the Higgs potential and which could give the correct Higgs Mass GeV. Therefore, the only case we can further explore is the case and , corresponding to .

It has been proven in [38] the no-scale boundary conditions when becoming universal at some unification scale above the GUT scale, are compatible with low-energy constraints. They show a scenario based on model where the superpotential contains terms , where and are and Higgs representations. For different values of and , the region of , and has been studied, taking into account phenomenological constraints on supersymmetric particles and the cosmological LSP density. Although, the LHC has imposed additional constraints, via the measurement of the Higgs Mass and the decay , the model is still consistent with the LHC data [31, 39]. For example, for the values and , the region with GeV and GeV is consistent with the relic cold dark matter density, a Higgs mass of GeV and the experimental measurements of .

#### 4.2.2 Case II: pure gravity SUSY breaking

As an alternative to the no-scale possibility, we can have the Standard Model superfields outside the logarithm. This is called Case II in Eq. 15. For small , where inflation works, we find that the soft supersymmetry breaking parameters are

 m0=m3/2,A0m3/2=−6α−3(4+α)b2+O(b3), Case II B0m3/2=2(1−β)−(1+β)b2+O(b3), (24)

where the relations for and are kept the same as in Eq. 23 while the universal soft scalar mass term is now different from zero and equal to the gravitino mass . Note that the soft scalar mass is equal to the gravitino mass, while the soft gaugino mass will be assumed to be much smaller, as in anomaly mediated SUSY breaking. As before, the main effect of switching on is to increase the gravitino mass, since the terms proportional to are negligible.

For the same reasons as before, the general cases and are not viable phenomenological choices. As mentioned, we impose , meaning (see Eq. 24). This will lead to tachyonic sfermion masses. Similarly, for we cannot find a value of which reproduces the correct Higgs Mass. Therefore, we will focus in the case and on the following, corresponding to and .

The special case and , meaning , is called pure gravity-mediated (PGM) models [40, 41, 42, 43, 44, 45, 46] where the gaugino masses, and terms are determined by anomaly mediation [47] leaving only the gravitino mass as a free parameter. Note that in this case since , Eq.24 gives to excellent approximation. The main phenomenological effect of the Polonyi term is then to set a limit on the gravitino mass from the requirement of successful inflation. These PGM models with GUT scale universality [41] are phenomenologically viable when including a Giudice-Masiero term in the Kähler potential [48], which allows to choose as a second free parameter. For successful electroweak symmetry breaking (EWSB), is restricted to a narrow range from about  [42, 46]. Then, the Higgs mass GeV is obtained when the gravitino mass is in the range TeV. In our case we have the additional constraint from inflation requiring TeV, see Fig. 2. Therefore, the Case II, in which , for and has an allowed parameter space when including the Giudice-Masiero term which is also compatible with inflation and corresponds to .

Recently, PGM models have been studied in an SU(5) GUT model [49], allowing two new parameters, a high energy scale above the GUT scale, and a new coupling , where is an adjoint Higgs . They find a viable parameter space as long as the Higgs coupling is relatively large, for a relaxed , away from , opening up the parameter space considerably. In the case where higher dimensional operators involving are included, proton decay can be within reach of future experiments. Moreover, in some regions of parameter space the bino can be degenerate with the wino or gluino, giving an acceptable dark matter relic density.

## 5 Conclusion

In this paper we have studied a version of Starobinsky-like inflation in no-scale SUGRA where a Polonyi term in the hidden sector breaks SUSY after inflation, providing a link between the gravitino mass and inflation. The linear Polonyi term provides a simple way to break SUSY after inflation, with the requirement of successful inflation leading to an upper bound on the gravitino mass TeV, with gaugino masses considerably less than this.

The progress made in this paper is to extend the previous hidden sector Polonyi theory (proposed by one of us) to include the visible sector and to calculate the resulting soft-SUSY breaking parameters in terms of the modular weights and for the bilinear and trilinear parts of the superpotential and a choice of Kähler potential. In this case, we can write the soft-SUSY breaking parameters in terms of , and the parameter accounting for the Polonyi term. In case I we included the MSSM matter and Higgs superfields inside the Log of the Kähler potential following a no-scale approach. In the second case, Case II, these superfields are added via minimal kinetic terms.

We were thereby led to familiar phenomenological possibilities for supersymmetry (SUSY) breaking, based on no-scale SUSY breaking and pure gravity mediated SUSY breaking, but with the strict bound coming from our Polonyi model that TeV. However we found that the only phenomenological viable choices for both cases I and II, are the ones with and , corresponding to .

In case I, in addition to , the scalar soft scalar mass term is zero , as in the no-scale SUSY breaking approach, in which case SUSY breaking at low energies is produced via non-zero gaugino masses . Models like this one had been discussed by ENO and have been shown to be compatible with LHC data, with all superpartners potentially observable at LHC or the FCC.

In case II, in addition to , the scalar mass is equal to the gravitino mass , with as in anomaly mediation models, with such a scenario referred to as PGM. Such PGM models are viable models after the inclusion of a Giudice-Masiero term in the Kähler potential, for a large gravitino mass of order 100-1000 TeV, compatible with our inflation bound, and can evade LHC searches while still providing a good dark matter candidate and gauge coupling unification, with squarks and sleptons very heavy, while the gauginos remain light and observable at the LHC or the FCC.

In conclusion, Starobinsky-like inflation in no-scale SUGRA models with a Polonyi term provides a promising setting for both inflation and SUSY breaking within a well motivated particle physics framework. The Polonyi term provides a link between the gravitino mass and inflation leading to a strict upper bound on the gravitino mass TeV. We have seen that under reasonable assumptions, the soft-SUSY breaking parameters can be calculated, leading to either no-scale SUGRA or PGM patterns, where the results presented here could form the basis of future phenomenological studies. In particular, since gauginos are significantly lighter than , this suggests that SUSY could be discovered at the LHC or FCC.

## Acknowledgments

SFK thanks the CERN Theory group for hospitality and acknowledges the STFC Consolidated Grant ST/L000296/1. SFK and EP acknowledge the European Union’s Horizon 2020 Research and Innovation programme under Marie Skłodowska-Curie grant agreements Elusives ITN No. 674896 and InvisiblesPlus RISE No. 690575.

## Appendix A Soft-supersymmetry breaking parameters

We present the analytic results for the gravitino mass and the soft-supersymmetry breaking parameters as a function of the modular weights and and the parameter , which takes into account the contribution from the Polonyi term in the superpotential. For both cases I and II, in which we include the Standard Model superfields inside or outside the logarithm in the Kähler potential, see Eqs. 14 and 15, the bilinear, and trilinear parameters are the same and the only difference is in the soft scalar mass term , vanishing in case I while being equal to the gravitino mass in case II.

 m3/2=−μ−1+√1+4b+b(−6+4√1+4b)√2(1−2b+√1+4b)3/2m0=0 (Case I)orm0=m3/2 (Case II) ,A0=−μ3(√4b+1−1)2(−8b+√4b+1−1)√2(−2b+√4b+1+1)3(b(α−8(α−2)b+5α√4b+1−10√4b+1+14)−2√4b+1+2)√(−√4b+1+2b(−5√4b+1+b(16b−12√4b+1+21)+6)+1),B0=−μ(√4b+1−1)2(−8b+√4b+1−1)(−2b+√4b+1+1)3(b(−8b(β−2)+5β√4b+1+β−10√4b+1+6)−√4b+1+1)√−2√4b+1+4b(−5√4b+1+b(16b−12√4b+1+21)+6)+2. (25)

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