1 Introduction

KANAZAWA-15-06

May, 2015

Constrained inflaton due to a complex scalar

Romy H. S. Budhi 111e-mail:  romyhanang@hep.s.kanazawa-u.ac.jp,   Shoichi Kashiwase 222e-mail:  shoichi@hep.s.kanazawa-u.ac.jp,

and

Daijiro Suematsu 333e-mail:  suematsu@hep.s.kanazawa-u.ac.jp


Physics Department, Gadjah Mada University, Yogyakarta 55281, Indonesia

Institute for Theoretical Physics, Kanazawa University, Kanazawa 920-1192, Japan

Abstract
We reexamine inflation due to a constrained inflaton in the model of a complex scalar. Inflaton evolves along a spiral-like valley of special scalar potential in the scalar field space just like single field inflation. Sub-Planckian inflaton can induce sufficient -foldings because of a long slow-roll path. In a special limit, the scalar spectral index and the tensor-to-scalar ratio has equivalent expressions to the inflation with monomial potential . The favorable values for them could be obtained by varying parameters in the potential. This model could be embedded in a certain radiative neutrino mass model.

1 Introduction

Inflationary expansion of the Universe is now believed to have existed before the radiation dominated era in the early Universe [1, 2]. Although a lot of inflation models have been proposed by now [3], we do not know which model can describe this phenomenon correctly. The relation between inflation and particle physics is also unclear. However, recent results of the CMB observations seem to have ruled out many of them already [2]. This has been done by comparing both values of the scalar spectral index and the tensor-to-scalar ratio obtained from the CMB observations and predicted values for them by each model.

If we take a large inflaton scenario in the slow-roll inflation framework, trans-Planckian values are required for realization of sufficient -foldings. In that case, we cannot answer the question why higher non-renormalizable terms do not contribute to the inflaton potential. If we include such terms in inflaton potential, slow-roll conditions cannot be satisfied. However, such kind of difficulty can be reconciled by compactifying the inflaton trajectory into a winding trajectory in the higher dimensional fields space. In that case, sufficient -foldings along the trajectory can be obtained even if each field is kept in sub-Planckian regions. That possibility was studied in [4] by introducing an idea about a spiralized inflation in two-dimensional field space as a possible solution of the multifield slow-roll inflation. Its realizations have been proposed in the several frameworks, such as in string models [5], SUSY models [6], axions-based models [7, 10, 11, 8, 9] and a complex scalar model which has similar features with axions-based models [12, 13]. The higher order corrections to the potential realizing the spiralized inflation are found to affect significantly the predicted tensor-to-scalar ratio without changing the spectral index substantially [14].

In this paper we study an inflation model based on large but sub-Planckian inflaton. The model considered here has been proposed in [15]. It could have an intimate connection to neutrino mass generation. Although the required number for -foldings is found to be realized in this model, the predicted tensor-to-scalar ratio by the model is too large compared with a central value of the up-dated observational results [2, 16]. Our main purpose is to study whether the favorable values for them can be obtained in this model. We also discuss a possible connection to a certain particle physics model.

2 A sub-Planckian inflaton model

The model studied here is defined by a complex scalar which has odd parity. Its invariant potential is assumed to be given such as [15]

If we use the polar coordinate , this potential can be written as

(1)

where is assumed to satisfy . As shown in Fig. 1, has local minima with a potential barrier in the radial direction. These minima form a spiral-like valley whose slope in the angular direction could be extremely small. As a result, if we use the field evolution along this valley, slow-roll inflation is expected to be caused even for sub-Planckian values of [15, 13].

Fig. 1: Potential at a fixed for case. Other parameters are fixed at , and .

The evolution of the scalar field in this potential is dictated by the following equation of motion:

(2)

where the Hubble parameter of the system is now written as and denotes partial derivative of the potential in the direction of field component . Taking , the terms could be simply written for any number of as follows,

(3)
(4)

We may solve eq. (2) numerically to see the evolution of . The initial value of each component cannot be selected arbitrarily since the slow-roll behavior could be ruined depending on it. If the initial position of the inflaton is located at a point higher than its next potential barrier, the inflaton could cross over it without realizing the slow-roll motion along the angular direction. The most simple setting for the initial value to realize the slow-roll is to take it at a potential minimum. An example of the evolution of the scalar field components is illustrated in Fig. 2.

(a)
(b)
Fig. 2: Inflaton evolution for case. Parameters in the potential are fixed at the same values as the ones used in Fig. 1. Inflaton is assumed to be at a potential minimum initially. In this case, it is numerically proven that the end of single field inflation signed as turning point in the panel (a) is mostly realized much before , such that it is illustrated in the panel (b).

Now we describe features of the inflation induced by this field evolution in detail. The radial component is assumed to take a large initial value on a local minimum in the radial direction. Even if is not just on this minimum initially, it converges to a minimum point within a certain period of time as long as it starts to roll from the neighborhood of a minimum point of the valley initially. In that case, as shown in [15], the model could cause sufficient -foldings through the inflaton evolution along this spiral-like valley even for sub-Planckian values of . An inflaton field could be identified with

(5)

where the subscript of the fields stands for the field value at the end of single field inflation. The field is defined by using as

(6)

The number of e-foldings caused by during its slow-roll is given as

(7)

where and is represented by using the hypergeometric function as

(8)

Slow-roll parameters and for single field inflation can be represented by using the model parameters as

(9)

If the term is neglected in these formulas, we can find very simple formulas for these slow-roll parameters at the time characterized by the inflaton value . They can be represented by using the -foldings , which is defined for in eq. (7), as

(10)

Thus, the scalar index and the tensor-to-scalar ratio can be derived as [15]

(11)

In order to see the features of this model, it may be useful to compare the model with single field inflation with monomial potential . Since the -foldings in this model is written as , the sufficient -foldings require a trans-Planckian value for the inflaton . We note that the contribution of is negligible in this case. If we use this number of -foldings , the slow roll parameters are expressed as

(12)

and then and can be written as

(13)

It is easily found that and in both models have the same expression for in the limit . However, we should remind that the present model works well only for the non-negligible since this term causes the potential barrier in the radial direction. makes the inflaton evolve along the spiral-like trajectory formed by the potential minima like a single field inflation. This brings about a different feature for the model from the inflation scenario.

In this model,the single field inflation is expected to end at the time when is realized. If we apply the slow-roll approximation to the slow-roll parameter , the inflation is found to end at . Since is satisfied, the end of inflation could happen much before the time when is realized. In such a case, is not satisfied and then has a substantial contribution to determine the number of -foldings in eq. (7). Thus, the smaller could be enough to realize the same values for and in comparison with the inflation.*** Although this becomes clear especially in the small case, could be well approximated as the value at in other cases.. We should also note that the values of and in this model could deviate largely from ones predicted in the inflation model due to the non-negligible contribution from the term. Illustration given in Fig. 1(b) justifies this argument numerically when whole contributions, including non-negligible term, are taken in to account. As it is expected, the end of inflation at which inflaton starts to oscillate around global minimum of the potential takes place much before . After this time, the inflaton falls in the reheating process and produces lighter particles.

3 Spectral index

We estimate the scalar spectral index and the tensor-to-scalar ratio by taking account of the effect. Before it, we constrain parameters in the potential by using the normalization for the scalar perturbation found in the CMB. The normalization for the scalar perturbation found in the CMB observations gives the constraint on the inflaton potential at the time when the scale characterized by a certain wave number exits the horizon. The observation of CMB requires the spectrum of scalar perturbation to take at [1], should satisfy

(14)

where we use . If the term does not dominate the potential, we can represent the condition from this normalization constraint as where is a value of at the time when the -foldings is .

On the other hand, the -foldings expected after the scale exits the horizon is dependent on the reheating phenomena and others in such a way as [3]

(15)

This suggests that should be considered to have a value in the range 50 - 60. Taking these constraints into account, we estimate both and for the case where is in this range.

3 1.00 1.5 0.05 0.417 6.528 60.0 0.967 0.070 -0.00047
9.84 1.7 0.05 0.411 5.914 60.0 0.964 0.056 -0.00043
8.62 1.9 0.05 0.406 5.399 60.0 0.959 0.040 -0.00032
2 1.32 1.1 0.05 0.394 7.019 60.0 0.973 0.058 -0.00043
1.76 1.1 0.05 0.384 6.725 50.0 0.968 0.072 -0.00061
1.22 1.6 0.05 0.383 5.931 60.0 0.969 0.039 -0.00040
1.71 1.6 0.05 0.374 5.767 50.0 0.964 0.052 -0.00059
1.03 1.9 0.05 0.374 5.318 60.0 0.963 0.026 -0.00035
1 1.36 0.5 0.05 0.349 5.079 50.0 0.975 0.041 -0.00046
7.45 1.6 0.05 0.333 4.146 60.0 0.970 0.015 -0.00036
1.02 1.6 0.05 0.326 4.102 50.0 0.966 0.019 -0.00052
6.15 1.8 0.05 0.327 3.976 60.0 0.966 0.011 -0.00035
8.77 1.8 0.05 0.320 3.944 50.0 0.962 0.016 -0.00052

Table 1 Examples of the predicted values for the spectral index and the tensor-to-scalar ratio in this scenario with .

Numerical examples are shown in Table 1 for the cases with a fixed . We note that the first term of becomes and for and 2, respectively. For given values of , the values of and are fixed so that the normalization condition given in eq. (14) is satisfied and also takes its value in the imposed range 50 - 60. Both and are estimated for them. If we apply the value of at  Mpc [2] to the present analysis using the same values of and , and are changed. This effect on is found to be for the fixed values of and which give and at Mpc. In Fig. 3, we plot the predicted points in the plane by red and green circles, which correspond to and 60 respectively for every 0.1 of starting from on the right-hand side while is fixed as . We show the boundary values of by the red and black stars, for which either red or green circles are inside of the region of CL and CL of the latest Planck TT+lowP+ BKP+lensing+ext combined data for the and panels, respectively. They show that the present model with included in this interval are favored by the latest Planck data combined with others. The best fit result is obtained for the case.

As discussed above, the present model shows the similar behavior to the monomial inflation models at least for the spectral index and the tensor-to-scalar ratio in the limiting case with the negligible . However, if is not negligible, this feature could be changed and these values largely deviate from the monomial inflation models. Since the predicted region in the plane could be distinctive from other inflation models, the model might be tested through future CMB observations. One of the promising CMB observations would be LiteBIRD which is expected to detect the signal of the gravitational wave with at more than [17]. Thus the whole of the predicted region could be verified in near future.

Recent CMB results suggest that the running of the spectral index is consistent with zero at level. Thus, this can be an another useful test of the model. The running of the spectral index is known to be expressed by using the slow-roll parameters as

(16)

where is defined as . In the present model, it is written by using the model parameters as

(17)

If we use the parameters given in Table 1, the running of the spectral index can be estimated in each case by using these formulas. The results are shown in the last column of Table 1. Although they are consistent with the latest Planck data, they take very small negative values. We might be able to use it for the verification of the model in future.

(a)
(b)
(c)
Fig. 3:   Predicted regions in the plane are presented in panel (a) for , in panel (b) for , and in panel (c) for . is fixed as in all cases. The values of and are given in Table 1 for representative values of . Contours given in the right panel of Fig. 21 in Planck 2015 results.XIII.[2] are used here. Horizontal black lines represent a possible limit detected by LiteBIRD in near future.

4 Relation with particle physics

Finally, we discuss the relation of the model with particle physics. Although we cannot clarify the origin of potential (2) at the present stage, we expect it might be produced through some non-perturbative effects of Planck scale physics. The complex scalar can play an important role in particle physics if we embed it in an extended standard model. As such an interesting example, we consider the radiative neutrino mass model proposed by Ma [18]. This model is given by the following Lagrangian for the neutrino sector:

(18)

where and are the doublet leptons and the ordinary doublet Higgs scalar in the standard model. Two types new fields are introduced in this model, that is, an inert double scalar and singlet fermions . All their masses are assumed to be of  TeV. New fields and are assigned odd parity of imposed symmetry, although all the standard model contents have its even parity. Since is assumed to have no vacuum expectation value, this symmetry is exact and then neutrino masses cannot be generated at tree level. Neutrinos get masses through a one-loop diagram which has and in the internal lines as shown in the left-hand diagram of Fig.4. Moreover, the lightest neutral odd field is stable to be a good dark matter (DM) candidate. Thus, DM is an inevitable ingredient for the neutrino mass generation in this model. The model has been clarified quantitatively to have interesting features through a lot of studies [19, 20].

We can relate the present model to the Ma model by identifying the symmetry in the present model with that in the Ma model. We assign its odd parity to the complex scalar . If we take account of these symmetry, new terms which are subdominant during the inflation period are introduced as invariant ones,

(19)

Here we note that the term in eq. (18) is also allowed under the imposed symmetry. However, since its -function is proportional to itself if an interaction in the last line of eq. (19) is neglected, is stable for radiative corrections. On the other hand, if it is included in the Lagrangian, the term can be induced through this interaction as the effective one at low energy regions after integrating out the heavy field.

This can be easily seen through the neutrino mass generation. In the present extended model, the neutrino masses can be generated through the right-hand diagram of Fig. 4. The neutrino masses obtained through this diagram can be described by the formula

(20)

where and represents the mass of the real and imaginary component of which can be expressed as and . stands for and , respectively. The function is defined as

(21)

If is satisfied and it corresponds to the present case, this formula is found to be reduced to

(22)

which is equivalent to the neutrino mass formula obtained through the left-hand diagram of Fig. 4 for the Ma model. This shows that can be identified with as the effective coupling obtained at the low energy regions much smaller than . The key coupling for the neutrino mass generation in the Ma model could be closely related to the inflaton interaction term in this extension.

Fig. 4:  One-loop diagrams contributing to the neutrino mass generation. The left-hand diagram is the one in the Ma model. Lepton number is violated through the Majorama mass of . The right-hand diagram is the one in the present extended model. represents the real and imaginary part of the singlet scalar defined by . is a dimensional coupling for which is expressed as and .

We should also note that the interesting feature for DM in the Ma model is completely kept in this extended model. We suppose that the odd lightest field is the neutral real component of the inert doublet . Its stability is guaranteed by the imposed symmetry. Since its relic abundance is determined by the coannihilations among the components of which are controlled by the coupling constants in eq. (18), the results obtained in [23, 24] can be applied to the present model without affecting the analysis in this paper. They shows the required relic abundance could be easily realized if either or takes a value of for the with the mass of  TeV. Thus, this extended model could give a simple explanation not only for the inflation but also for the neutrino masses and the DM abundance, simultaneously.

5 Summary

We have considered an inflation scenario based on a complex singlet scalar. Special potential of this scalar constrains the inflaton evolution along a spiral-like trajectory in the space of two degrees of freedom. This makes the model behave like a single field inflation scenario. However, since the slop along this constrained direction is flat enough, inflaton can travel through trans-Planckian path. As a result, the sufficient -foldings can be realized even for sub-Planckian inflaton values. Serious potential problem in the large field inflaton could be solved in this model. Both the spectral index and the tensor-to-scalar ratio predicted in this model can be consistent with recently up-dated CMB observational results. Since these could take values in distinctive regions from other inflation scenario, the model might be tested through future CMB observations.

The inflaton in this model might be embedded into the extended standard model as an important ingredient. As such an example, we have discussed a possibility that the inflaton is an indispensable element in the radiative neutrino mass model, where a certain quartic scalar coupling plays a crucial role in the neutrino mass generation. Since the inflaton causes this coupling as an effective one at low energy regions, it could have a close relation with particle physics in this extension. The model might have another interesting feature. Reheating through the inflaton decay might give the origin of baryon number asymmetry through the generation of the lepton number asymmetry in a non-thermal way. Detailed study of this subject will be presented in future publication [22]. If it could be shown through explicit analysis, the problems in the standard model might be solved in a compact way in this extended model.

Acknowledgement

R.  H.  S.  Budhi is supported by the Directorate General of Higher Education (DGHE) of Indonesia (Grant Number 1245/E4.4/K/2012). S. K. is supported by Grant-in-Aid for JSPS fellows (265862). D. S. is supported by JSPS Grant-in-Aid for Scientific Research (C) (Grant Number 24540263) and MEXT Grant-in-Aid for Scientific Research on Innovative Areas (Grant Number 26104009).

References

  • [1] WMAP Collaboration, D. N. Spergel, et al., First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters, Astrophys. J. Suppl. 148 (2003) 175 [ astro-ph/0302209];
    E. Komatsu, et al., Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation, Astrophys. J. Suppl. 180 (2009) 330 [arXiv:0803.0547 [astro-ph]];
    E. Komatsu, et al., Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation, Astrophys. J. Suppl. 192 (2011) 18 [arXiv:1001.4538[astro-ph.CO]];
    G. Hinshaw, et al., Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Parameter Results,Astrophys. J. Suppl. 208 (2013) 19 [arXiv:1212.5226 [astro-ph.CO]];
    Planck Collaboration, P. A. R. Ade, et al., Planck 2013 results. XXII. Constraints on inflation, Astron. Astrophys. 571 (2014) A22 [arXiv:1303.5082 [astro-ph.CO]].
  • [2] Planck Collaboration, P. A. R. Ade, et al., Planck 2015 results. XIII. Cosmological parameters, [arXiv:1502.01589 [astro-ph.CO]];
    Planck Collaboration, P. A. R. Ade, et al., Planck 2015 results. XX. Constraints on inflation, [arXiv:1502.02114 [astro-ph.CO]].
  • [3] For reviews, D. H. Lyth and A. Riotto, Particle physics models of inflation and the cosmological density perturbation, Phys. Rept. 314 (1999) 1 [hep-ph/9807278];
    A. R. Liddle and D. H. Lyth, Cosmological inflation and Large-Scale Structure, Cambridge University Press, Cambridge U.K, (2000).
  • [4] ] I. S.  Yang, The Strong Multifield Slowroll Condition and Spiral Inflation, Phys.Rev. D85 (2012) 123532 [arXiv:1202.3388 [hep-th]]
  • [5] Pontus Ahlqvist, Brian Greene1, and David Kagan, Exploring Spiral Inflation in String Theory, [arXiv:1308.0538 [hep-th]].
  • [6] T. Li, Z. Li, D. V. Nanopoulos, Helical Phase Inflation, Phys. Rev. D91 (2015) 061303 [arXiv:1409.3267[hep-th]];
    T. Li, Z. Li, D. V. Nanopoulos, Helical Phase Inflation and Monodromy in Supergravity Theory, [arXiv:1412.5093[hep-th]].
  • [7] J. McDonald, A Minimal Sub-Planckian Axion Inflation Model with Large Tensor-to-Scalar Ratio, JCAP 1501 (2015) 018 [arXiv:1407.7471 [hep-th]]
  • [8] C. D. Carone, J. Erlich, A. Sensharma, Z. Wang, Dante’s Waterfall, Phys. Rev. D91 (2015) 043512 [arXiv:1410.2593[hep-ph]].
  • [9] Marcus Berg, Enrico Pajer, and Stefan Sjors, Dante’s Inferno, Phys.Rev. D81 (2010) 103535, [ arXiv:0912.1341 [hep-th]]
  • [10] Jihn E. Kim, , Hans Peter Nilles, and Marco Peloso Completing Natural Inflation, JCAP 0501 (2005) 005, [arXiv:hep-ph/0409138]
  • [11] Rolf Kappl, Sven Krippendorf and Hans Peter Nilles , Aligned Natural Inflation: Monodromies of two Axions, Phys.Lett. B737 (2014) 124-128 , [arXiv:1404.7127v3 [hep-th]]
  • [12] G. Barenboim, W.-II Park, Spiral Inflation, Phys. Lett. B741 (2015) 252 [arXiv:1412.2724[hep-ph]]
    Gabriela Barenboim and Wan-Il Park, Spiral Inflation with Coleman-Weinberg Potential, Phys.Rev. D91 (2015) 063511, [arXiv:1501.00484 [hep-ph]].
  • [13] J. McDonald, Sub-Planckian Two-Field Inflation Consistent with the Lyth Bound, JCAP 09 (2014) 027 [ arXiv:1404.4620 [hep-ph]].
  • [14] J. McDonald, Signatures of Planck Corrections in a Spiralling Axion Inflation Model, JCAP 1505 (2015) 014 [arXiv:1412.6943[hep-ph]].
  • [15] R. H. S. Budhi, S. Kashiwase and D. Suematsu, Inflation in a modified radiative seesaw model, Phys. Rev. D90 (2014) 113013 [arXiv:1409.6889 [hep-ph]].
  • [16] BICEP2/Keck and Planck Collaborations, P. A. R. Ade, et al., Joint Analysis of BICEP2/Keck Array and Planck Data, Phys. Rev. Lett. 114 (2015) 101301 [arXiv:1502.00612 [astro-ph.CO]].
  • [17] M. Hazumi, Future CMB polarization measurements and Japanese contributions, Prog. Theor. Phys. Suppl. 190 (2011) 75.
  • [18] E. Ma, Verifiable radiative seesaw mechanism of neutrino mass and dark matter, Phys. Rev. D73 (2006) 077301 [hep-ph/0601225].
  • [19] J. Kubo, E. Ma and D. Suematsu, Cold Dark Matter, Radiative Neutrino Mass, , and Neutrinoless Double Beta Decay, Phys. Lett. B642 (2006) 18 [hep-ph/0604114];
    J. Kubo and D. Suematsu, Neutrino masses and CDM in a non-supersymmetric model, Phys. Lett. B643 (2006) 336 [hep-ph/0610006]; D. Aristizabal Sierra, J. Kubo, D. Suematsu, D. Restrepo and O. Zapata, Radiative seesaw: Warm dark matter, collider and lepton flavour violating signals, Phys. Rev. D79 (2009) 013011 [arXiv:0808.3340 [hep-ph]];
    D. Suematsu, T. Toma and T. Yoshida, Reconciliation of CDM abundance and in a radiative seesaw model , Phys. Rev. D79 (2009) 093004 [arXiv:0903.0287 [hep-ph]];
    D. Suematsu, T. Toma and T. Yoshida, Enhancement of the annihilation of dark matter in a radiative seesaw model, Phys. Rev. D82 (2010) 013012 [arXiv:1002.3225 [hep-ph]].
  • [20] D. Suematsu, Leptogenesis and dark matter unified in a non-SUSY model for neutrino masses, Eur. Phys. J. C56 (2008) 379 [arXiv:0706.2401 [hep-ph] ];
    D. Suematsu, Thermal Leptogenesis in a TeV Scale Model for Neutrino Masses, Eur. Phys. J. C72 (2012) 1951 [arXiv:1103.0857 [hep-ph]].
  • [21] D. Suematsu, Extension of a radiative neutrino mass model based on a cosmological view point, Phys. Rev. D85 (2012) 073008 [ arXiv:1202.0656 [hep-ph]].
  • [22] S. Kashiwase and D. Suematsu, in preparation.
  • [23] T. Hambye, F.-S. Ling, L. L. Honorez and J. Roche, Scalar Multiplet Dark Matter, JHEP 07 (2009) 090 [arXiv:0903.4010 [hep-ph]].
  • [24] S. Kashiwase and D. Suematsu, Baryon number asymmetry and dark matter in the neutrino mass model with an inert doublet, Phys. Rev. D86 (2012) 053001 [ arXiv:1207.2594 [hep-ph]];
    S. Kashiwase and D. Suematsu, Leptogenesis and dark matter detection in a TeV scale neutrino mass model with inverted mass hierarchy, Eur. Phys. J. C73 (2013) 2484 [arXiv:1301.2087 [hep-ph]].
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