Running non-minimal inflation with stabilized inflaton potential
Abstract
In the context of the Higgs model involving gauge and Yukawa interactions with the spontaneous gauge symmetry breaking, we consider \(\lambda \phi ^4\) inflation with non-minimal gravitational coupling, where the Higgs field is identified as the inflaton. Since the inflaton quartic coupling is very small, once quantum corrections through the gauge and Yukawa interactions are taken into account, the inflaton effective potential most likely becomes unstable. In order to avoid this problem, we need to impose stability conditions on the effective inflaton potential, which lead to not only non-trivial relations amongst the particle mass spectrum of the model, but also correlations between the inflationary predictions and the mass spectrum. For concrete discussion, we investigate the minimal \(B-L\) extension of the standard model with identification of the \(B-L\) Higgs field as the inflaton. The stability conditions for the inflaton effective potential fix the mass ratio amongst the \(B-L\) gauge boson, the right-handed neutrinos and the inflaton. This mass ratio also correlates with the inflationary predictions. In other words, if the \(B-L\) gauge boson and the right-handed neutrinos are discovered in the future, their observed mass ratio provides constraints on the inflationary predictions.
1 Introduction
Current understanding about the origin of our universe is that, for a very brief moment at the beginning, our universe went through a period of rapid accelerated expansion known as inflation. Inflation scenario [1, 2, 3, 4] was originally proposed to solve serious problems in the Standard Big-Bang Cosmology, namely, the horizon, flatness and monopole problems. In addition and more importantly from the view point of the current cosmological observations, inflation provides a mechanism to create primordial density fluctuations of the early universe which seed the formation of large scale structure of the universe that we see today. In a simple inflation scenario, inflation is driven by a single scalar field (inflaton) that slowly rolls down to its potential minimum (slow-roll inflation). During the slow-roll era, the inflaton energy is dominated by a slowly varying potential, which causes the universe to undergo a phase of an accelerated expansion. Quantum fluctuations of the inflaton field are stretched to macroscopic scales by inflation to yield the primordial density fluctuations. After inflation, the inflaton decays to the Standard Model (SM) particles and the decay products heat up the universe (reheating). The success of big bang nucleosynthesis scenario requires the reheating temperature to be \(T_{\mathrm{R}} \gtrsim 1\) MeV.
Recently the Planck 2015 results [5] have set an upper bound on the tensor-to-scalar ratio as \(r \lesssim 0.11\) while the best fit value for the spectral index (\(n_\mathrm{s}\)) is \(0.9655 \pm 0.0062\) at \(68\%\) CL. Hence, the simple chaotic inflationary scenario with the inflaton potentials \(V \propto \phi ^4\) and \(V \propto \phi ^2\) are disfavored because their predictions for r are too large. Among many inflation models, \(\lambda \phi ^4\) inflation with non-minimal gravitational coupling (\(\xi \phi ^2 \mathcal{R}\), where \(\phi \) is inflaton, \(\mathcal{R}\) is the scalar curvature, and \(\xi \) is a dimensionless coupling) is a very simple model, which can satisfy the constraints by the Planck 2015 with \(\xi \gtrsim 0.001\) [6, 7, 8].
Given that we need interactions between SM particles and inflaton for a successful reheating of the universe, a more compelling inflation scenario would be where the inflaton field plays another important role in particle physics. As an example of such a scenario, we may consider the (general) Higgs model, where a scalar (Higgs) field plays the crucial role to spontaneously break the gauge symmetry of the model, and we identify the Higgs field as inflation. The SM Higgs inflation [9, 10, 11, 12, 13, 14, 15, 16, 17, 18] is nothing but this scenario, where the SM Higgs boson plays the role of inflaton with non-minimal gravitational coupling. For the observed Higgs boson mass of around 125 GeV, the stability of SM Higgs potential is very sensitive to the initial value of top quark pole mass. Hence, we need more precise measurements for top quark pole mass [19] to obtain a conclusion about the SM Higgs potential stability.^{1} For a large top quark pole mass, for example, \(M_\mathrm{t}=173.34\) GeV [24], the SM Higgs potential turns out to be unstable, and some extension of the SM is necessary to realize the SM Higgs inflation [25, 26].^{2} It is interesting to apply the same idea as the SM Higgs inflation to the general Higgs model and identify the Higgs field of the model (not the SM Higgs field) as the inflaton in the presence of non-minimal gravitational coupling. For a simple example, see [37].
A simple way to avoid this problem is to require the beta function to vanish at the initial inflaton value (the stationary condition of \(\lambda \) with respect to \(\phi \)), namely, \(C_g g^4 - C_Y Y^4 = 0 \).^{3} This condition leads to a relation between g and Y, equivalently, a mass relation between the gauge boson and fermion in the Higgs model. Since the Higgs quartic coupling at low energy is evaluated by solving the RG equation, in which the gauge and Yukawa couplings dominate, the resultant Higgs mass also has a relation to the gauge and fermion masses. The stability of the effective potential also requires the positivity of the second derivative of the potential, which leads to another constraint on the gauge and Yukawa couplings. In the slow-roll inflation, the inflationary predictions are determined by the slow-roll parameters defined with the potential and its derivatives, and therefore, the inflationary predictions have a correlation with the mass spectrum of the Higgs model.
In order to explicitly show the mass relation and the correlation between the particle mass spectrum and inflationary predictions, we take the minimal \(B-L\) model as an example. This model is a very simple, well-motivated extension of the SM, where the global \(B-L\) (baryon number minus lepton number) in the SM is gauged. Three right-handed neutrinos and the \(B-L\) Higgs field (which is identified as the inflaton) are introduced for the cancellation of the gauge and gravitational anomaly and the \(B-L\) gauge symmetry breaking, respectively. Associated with the \(B-L\) gauge symmetry breaking, the \(B-L\) gauge boson and the right-handed neutrinos acquire their masses. With the generation of the Majorana right-handed neutrino masses, the seesaw mechanism [40, 41, 42, 43, 44, 45] for the light neutrino mass generation is automatically implemented in this model. Analyzing the RG evolutions of the \(B-L\) sector and the effective inflaton (\(B-L\) Higgs) potential, we show the particle mass spectrum and its correlation to the inflationary predictions. Through the correlation, the Planck 2015 results provide us with constraints on the particle mass spectrum.
This paper is organized as follows. In the next section, we briefly review the \(\lambda \phi ^4\) inflation with non-minimal gravitational coupling at the tree level, and discuss the inflationary predictions in the light of the Planck 2015 results. In Sect. 3, we introduce the minimal \(B-L\) extension of the SM and calculate the RG improved effective Higgs potential. We show the particle mass spectrum derived from the stability conditions of the effective potential and its correlation to the inflationary predictions. We then compare our results for various values of the non-minimal gravitational coupling \(\xi \) with the Planck 2015 results. In Sect. 5, we discuss reheating scenario in the \(B-L\) Higgs inflation for the completion of our inflationary scenario. Section 6 is devoted to conclusions.
2 Non-minimal \(\lambda \phi ^4\) inflation at tree level
Figure 1 shows inflationary predictions for the non-minimal \(\lambda \phi ^4\) inflation at the tree level for \(N=50\) (dashed–dotted) and \(N=60\) (solid). Top panels show r vs. \(\xi \) (left) and \(n_\mathrm{s}\) vs. \(\xi \) (right). Both r and \(n_\mathrm{s}\) show asymptotic behavior for both small and large \(\xi \) values. In the minimal \(\lambda \phi ^4\) inflation limit with \(\xi = 0\), we obtain \(r \simeq 0.31\) (0.26) and \(n_\mathrm{s} \simeq 0.942\) (0.951) for \(N=50\) (60). The plots also show that, for a larger e-holding number, we obtain a larger \(n_\mathrm{s}\) while a smaller r. The bottom-left panel shows the tree-level quartic coupling \(\lambda \) as a function of \(\xi \). Note that \(\lambda \) is very small unless \(\xi \gg 1\). The inflationary predictions for \(n_\mathrm{s}\) and r for various values of \(\xi \) are depicted in the bottom-right panel along with the results from the measurements by Planck 2015 and Planck+BICEP2/Keck Array [5]. We see that the inflationary predictions for \(\xi \gtrsim 0.001\) are consistent with the observations.
3 Running \(B-L\) Higgs inflation and stability of inflaton potential
Particle contents of the minimal \(B-L\) model. In addition to the SM particle contents, the right-handed neutrino \(N\!R^i\) (\(i=1,2,3\) denotes the generation index) and a complex scalar \(\varphi \) are introduced
SU(3)\(_c\) | SU(2)\(_L\) | U(1)\(_Y\) | U(1)\(_{B-L}\) | |
---|---|---|---|---|
\( q_\mathrm{L}^i \) | 3 | 2 | \(+1/6\) | \(+1/3\) |
\( u_\mathrm{R}^i \) | 3 | 1 | \(+2/3\) | \(+1/3\) |
\( d_\mathrm{R}^i \) | 3 | 1 | \(-1/3\) | \(+1/3\) |
\( \ell ^i_\mathrm{L}\) | 1 | 2 | \(-1/2\) | \(-1\) |
\( \mathrm{NR}^i\) | 1 | 1 | 0 | \(-1\) |
\( e_\mathrm{R}^i \) | 1 | 1 | \(-1\) | \(-1\) |
H | 1 | 2 | \(-1/2\) | 0 |
\( \varphi \) | 1 | 1 | 0 | \(+2\) |
Let us now investigate the stability of the effective inflaton potential. In our analysis throughout this paper, we set the initial values of \(\lambda \) to be the one obtained in the tree-level analysis at the initial inflaton value \(\phi =\phi _\mathrm{I}\), equivalently, \(\Phi _\mathrm{I}= \phi _\mathrm{I}/\sqrt{1+\xi \phi _\mathrm{I}^2} \). Then, we consider the RG improved effective inflaton potential by taking into account the RG evolution of the quartic coupling with the initial condition at \(\Phi _\mathrm{I}\).
In order to avoid this instability, we impose not only the condition of \(\beta _\lambda =0\) but also \(\mathrm{d} \beta _\lambda /\mathrm{d} \Phi > 0\) at \(\Phi _\mathrm{I}\).^{8} From the first condition, the Yukawa coupling Y is determined by the gauge coupling, which we take as a free parameter in our analysis, along with the others, \(\xi \) and \(v_{BL}\). The second condition ensures that the effective potential is monotonically increasing in the vicinity of \(\Phi _\mathrm{I}\), and yields a lower bound on \(g > g_{\mathrm{min}}\).^{9} When we analyze the global structure of the effective potential, we can notice that there exists an upper bound on \(g< g_{\mathrm{max}}\). For a large \(g > g_{\mathrm{max}}\), the effective potential develops a local minimum at \(\Phi < \Phi _\mathrm{I}\), so that the inflaton field will be trapped in this minimum after inflation.^{10} A second inflation then takes place until the vacuum transition from this local minimum to the true \(B-L\) symmetry breaking vacuum. To avoid this problem, the parameter region is restricted to be in the range of \(g_{\mathrm{min}}< g < g_{\mathrm{max}}\). Figure 3 shows the effective potential for various values of the gauge coupling (g) for fixed \(\xi =0.1\). In the left panel, the solid line depicts the effective potential for \(g=0.041\), while the dot-dashed line is for \(g=0.046\). In this example, we find the upper bound as \(g_{\mathrm{max}}=0.0425\). We can see that the effective potential develops a local minimum for \(g=0.046 > g_{\mathrm{max}}\). For various values of \(g < g_{\mathrm{max}}\), the effective potentials are shown in the right panel.
4 Inflationary predictions and low energy observables
Under the stability conditions, \(g_{\mathrm{min}}< g < g_{\mathrm{max}}\) with various value of \(\xi \), we now calculate the inflationary predictions with the effective inflaton potential. Since we refer the results in the tree-level analysis for \(\lambda (\Phi _\mathrm{I})\) for a fixed \(\xi \) and impose the stability condition \(\beta _\lambda (\Phi _\mathrm{I}) =0\), our prediction for the tensor-to-scalar ratio r is the same as the one obtained in the tree-level analysis. However, the RG evolution of the inflaton quartic coupling alters the other inflationary predictions, \(n_\mathrm{s}\) and \(\alpha \), from those obtained in the tree-level analysis, because they are calculated by the second and third derivatives of the effective potential (see Eqs. (2.5) and (2.9)).
In order to see the inflationary predictions as a function of g, we show our results in Fig. 5 for \(\xi =0.0029\), 0.01 and 0.1, with \(N=60\). The top-left and top-right panels show the inflationary predictions of \(n_\mathrm{s}\) and \(\alpha =\mathrm{d}n_\mathrm{s}/\mathrm{d} \ln k\) as a function of g in the range of \(g_{\mathrm{min}}< g < g_{\mathrm{max}}\). The prediction for r is the same in the tree-level analysis, and \(r \simeq 0.108, 0.045\) and 0.008, respectively, for \(\xi =0.0029\), 0.01 and 0.1. For a larger value of \(\xi \), \(g_{\mathrm{max}}\) becomes larger. As g is lowered, the predicted \(n_\mathrm{s}\) value approaches the tree-level prediction. By numerically solving the RG equations for the couplings in Eq. (3.6) for a fixed g, we obtain the particle mass spectrum with \(m_{Z^\prime }=3\) TeV. The mass ratio \(m_N/m_{Z^\prime }\) is shown in the bottom-left panel, while the bottom-right panel shows the inflaton mass.^{12} In both panels, the solid lines from left to right correspond to the results for \(\xi =0.0029\), 0.01 and 0.1, respectively. The resultant mass ratio is almost independent of \(\xi \), but shows a splitting for \(g \lesssim 5 \times 10^{-4}\). For such a very small g, its corresponding Y determined by the stability condition is also very small, and hence both g and Y are almost RG invariant and the mass ratio is determined by \(Y(\Phi _\mathrm{I})/g(\Phi _\mathrm{I})\). However, in this case, the condition \(g^2, Y^2 \gg \lambda \) is no longer valid, and Y determined by \(\beta _\lambda (\Phi _\mathrm{I})=0\) depends on the input \(\lambda \) values. This is the reason why the bottom-left panel shows the splitting among three solid lines for \(g \lesssim 5 \times 10^{-4}\). For \(g \gtrsim 0.005\), the RG evolution of \(\lambda \) is mainly determined by g and Y in its beta function, since \(\lambda (\Phi _\mathrm{I})\) is extremely small. For a very small g value \(\lesssim 0.005\), the effect of g and Y on the RG evolution of \(\lambda \) becomes negligible, and \(\lambda (v_{BL}) \simeq \lambda (\Phi _\mathrm{I})\). Since we have fixed \(m_{Z^\prime }=2 g(v_{BL}) v_{BL}=3\) TeV, \(v_{BL} = 1.5 \;\mathrm{TeV}/g(v_{BL}) \simeq 1.5 \;\mathrm{TeV}/g(\Phi _\mathrm{I})\), and the inflaton mass becomes larger proportionally to \(1/g(\Phi _\mathrm{I})\) as shown in the bottom-right panel.
Same as Fig. 5 but for \(N=50\) and 60 with \(\xi =0.1\) is depicted in Fig. 6. The dashed lines denote the results for \(N=50\), while the solid lines for \(N=60\). The inflationary predictions show a sizable deference for the two different N values, as shown in the tree-level analysis in Sect. 2. On the other hand, the particle mass spectrum weakly depends on N.
We show the results for the mass spectrum for large \(\xi \) values and \(N=60\) in Fig. 7. The solid lines from left to right corresponds to the results for \(\xi =1\), 10, 50, 150, 500 and 1000. For \(g\lesssim 0.05\), the resultant mass ratio in the left panel shows \(\xi \)-dependence. This is because \(g^2, Y^2 \gg \lambda \) is no longer valid for such a small g value, and the Y value determined by \(\beta _\lambda (\Phi _\mathrm{I})\) depends on \(\lambda (\Phi _\mathrm{I})\). We also show the inflation mass spectrum in the right panel, which show a similar behavior to the result in the bottom-right panel in Fig. 5. As we have seen in Fig. 4, the inflationary predictions for \(\xi \gtrsim 1\) are close to those obtained in the tree-level analysis, \(n_\mathrm{s} \simeq 0.968\) and \(r \simeq 0.003\).
5 Reheating after inflation
The left panel in Fig. 9 shows the mass eigenvalue \(m_{\phi _2}\) as a function of \(\sin \theta \) for various \(m_\phi \) values with \(m_h=125\) GeV. In the \(\theta =0\) limit, \(m_{\phi _2}=m_\phi \), while \(m_{\phi }=m_h\) for \(\theta =\pi /2\). Although in this plot we show the results by using Eq. (5.5), we only consider the case with \(\theta \ll 1\) as mentioned above, otherwise our results obtained in the previous sections are changed in the presence of a sizable \(\lambda ^\prime \). For \(\theta \ll 1\), the mass eigenstate \(\phi _2\) (\(\phi _1\)) is almost identical to \(\phi \) (h).
6 Conclusions
The inflationary universe is the standard paradigm in modern cosmology, which not only solves the problems in the Standard Big Bang Cosmology, but also provide the primordial density fluctuations necessary for generating the large scale structure of the present universe. As a simple and successful inflationary scenario, we have considered the \(\lambda \phi ^4\) inflation with non-minimal gravitational coupling. With a suitable strength of the non-minimal coupling, the inflationary predictions of this scenario becomes perfectly consistent with the Planck 2015 results.
It is more interesting if the inflaton can also play some crucial role in particle physics. We have considered the general Higgs model with the gauge and Yukawa interactions with the spontaneous gauge symmetry breaking. In the presence of the non-minimal gravitational coupling, the Higgs field can also play the role of inflaton. The analysis with the Higgs potential at the tree-level leads to the inflationary predictions consistent with the cosmological observations. However, once we take quantum corrections, the effective inflaton potential most likely becomes unstable. This is because the inflaton quartic coupling is extremely small in a large portion of the parameters space and the effective potential is controlled by the gauge and Yukawa couplings independently of the quartic coupling. In the renormalization group improved effective potential, we see that the running quartic coupling becomes negative in the vicinity of the initial inflaton value, indicating the instability of the effective potential. In order to avoid this problem, we have imposed the stability condition of vanishing the beta function of the inflation quartic coupling. This condition leads to a non-trivial relation between the gauge and fermion masses. Since the renormalization group evolution of the inflaton quartic coupling is mainly controlled by the gauge and Yukawa coupling, the inflation mass at low energy is determined by the couplings. Therefore, the mass spectrum of the gauge boson, fermion and inflation shows a non-trivial relation.
Since the inflaton potential is modified from the tree-level one, the inflationary predictions are altered from those obtained by the tree-level analysis. Although the prediction of the tensor-to-scalar ratio remains the same under the condition of the vanishing beta function, the predictions for the scalar spectral index and the running of the spectral index can be significantly altered. The fact that the effective potential is controlled by the gauge and Yukawa couplings implies a correlation between the inflationary predictions and the particle mass spectrum. Therefore, the observables at the gauge symmetry breaking scale correlate with the inflationary predictions which determined by physics at an extremely high energy compared to the gauge symmetry breaking scale.
By taking the minimal \(B-L\) extension of the Standard Model as a simple example, we have shown such a non-trivial relation in the particle mass spectrum driven by the stability condition of the effective inflaton potential. We also have calculated the inflationary predictions from the effective potential and found their dependence of the \(B-L\) gauge coupling. Therefore, the new particle mass spectrum of the \(B-L\) model, once observed, has an implication to the inflationary predictions. On the other hand, more precise measurements of the inflationary predictions yield a constraint on the \(B-L\) particle mass spectrum.
For completeness, we have also investigated reheating after inflation. Since the inflation is lighter than the \(Z^\prime \) boson and the right-handed neutrinos, its reheating process through the heavy particles are not efficient, and the resultant reheating temperature is too low to be consistent with the bound from big bang nucleosynthesis. We then introduce a coupling between the inflaton and the Standard Model Higgs doublet. Through the mixing with the Standard Model Higgs boson, the inflaton can decay into the Standard Model particles and the universe can be heated up with a sufficiently high reheating temperature. We have found that this happens with a sufficiently small coupling between the inflaton and the Higgs doublet and such a small has essentially no effect on our analysis for the particle mass spectrum and the inflationary predictions.
Footnotes
- 1.
- 2.
- 3.
- 4.
For a small \(\xi \lesssim 1\), the inflaton is very light and its potential is approximately given by \(\lambda \phi ^4\). In this case the inflaton energy density behaves like the energy density of the radiation, and the e-folding number N can be determined unambiguously [46]. In this case we find \(N\simeq 60\).
- 5.
In this RG improved effective potential, we have identified the renormalization scale with \(\Phi \) according to the prescription proposed in [47, 48, 49], where it has been shown that the effective potential is frame-independent with this choice. In fact, we are especially interested in the parameter region of \(\xi \ll 1\) in this paper, so that \(\Phi \simeq \phi \) and the identification reduces to the usual one.
- 6.
- 7.
In this paper, we are interested in this case, otherwise the beta function is so small that the inflaton quartic coupling is almost RG invariant. Although the tree-level analysis is valid in this case, the gauge and Yukawa couplings are too small to yield any impacts in the experimental point of view.
- 8.
To be precise, \(\beta _\lambda \) is not necessary to be exactly zero to stabilize the inflaton potential. We may consider a more general condition \(96 g^4- 3 Y^4 \lesssim \lambda ^2\). Since \(\lambda \ll 1\), \(\beta _\lambda =0\) is a good approximation. In addition, although \(g, Y \lesssim \lambda \) can approximately satisfy this condition, we are not interested in such very small couplings for which RG evolutions are negligible.
- 9.
From Eq. (3.9) we find \(g_{\mathrm{min}}^2 \sim \lambda \). The discussion here is applicable only for \(g^2 \gtrsim \lambda \), and \(g_{\mathrm{min}}\) is not the general lower bound on the gauge coupling. For \(g^2, Y^2 \ll \lambda \), the running effect on all the couplings is negligible and hence the inflaton potential is stable.
- 10.
- 11.
In the same way, we can express the running of the spectral index, \(\alpha \), in terms of \(\xi \), \(\Phi _\mathrm{I}\), \(\lambda \) and g. However, as we will see in the following numeral analysis, the predicted \(\alpha \) values are found to be very small and always consistent with the Planck 2015 results. Thus, we omit the expression for \(\alpha \).
- 12.
Note that although the resultant mass ratios are shown at a very high precision level, our RG analysis at the one-loop level has an uncertainty of \(\mathcal{O}(g^2)\)% from quantum corrections at the next order. At this level of precision, different lines are virtually indistinguishable, so we have shown Figs. 5 and 6 at such a very high precision level.
- 13.
In general, reheating can occur through the parametric resonance more effectively than the perturbative decay of the inflaton. For a detailed discussion of “preheating” in the Higgs inflation, see [54, 55]. In our analysis we do not consider the preheating and estimate the reheating temperature using Eq. (5.1). The true reheating temperature could be much higher than our result.
Notes
Acknowledgements
This work is supported in part by the United States Department of Energy Grant, No. DE-SC 0013680.
References
- 1.A.A. Starobinsky, A new type of isotropic cosmological models without singularity. Phys. Lett. B 91, 99 (1980)ADSCrossRefGoogle Scholar
- 2.A.H. Guth, The inflationary universe: a possible solution to the horizon and flatness problems. Phys. Rev. D 23, 347 (1981)ADSCrossRefGoogle Scholar
- 3.A.D. Linde, Chaotic inflation. Phys. Lett. B 129, 177 (1983)ADSCrossRefGoogle Scholar
- 4.A. Albrecht, P.J. Steinhardt, Cosmology for grand unified theories with radiatively induced symmetry breaking. Phys. Rev. Lett. 48, 1220 (1982)ADSCrossRefGoogle Scholar
- 5.P.A.R. Ade et al. [Planck Collaboration], Planck 2015 results. XIII. Cosmological parameters. arXiv:1502.01589 [astro-ph.CO]
- 6.N. Okada, M.U. Rehman, Q. Shafi, Tensor to scalar ratio in non-minimal \(\phi ^4\) inflation. Phys. Rev. D 82, 043502 (2010). arXiv:1005.5161 [hep-ph]
- 7.N. Okada, V.N. Senoguz, Q. Shafi, The observational status of simple inflationary models: an update. arXiv:1403.6403 [hep-ph];
- 8.T. Inagaki, R. Nakanishi, S.D. Odintsov, Non-minimal two-loop inflation. Phys. Lett. B 745, 105 (2015). arXiv:1502.06301 [hep-ph]ADSCrossRefMATHGoogle Scholar
- 9.F.L. Bezrukov, M. Shaposhnikov, The standard model Higgs boson as the inflaton. Phys. Lett. B 659, 703 (2008). arXiv:0710.3755 [hep-th]ADSCrossRefGoogle Scholar
- 10.F.L. Bezrukov, A. Magnin, M. Shaposhnikov, Standard model Higgs boson mass from inflation. Phys. Lett. B 675, 88 (2009). arXiv:0812.4950 [hep-ph]ADSCrossRefGoogle Scholar
- 11.F. Bezrukov, D. Gorbunov, M. Shaposhnikov, On initial conditions for the Hot Big Bang. JCAP 0906, 029 (2009). arXiv:0812.3622 [hep-ph]ADSCrossRefGoogle Scholar
- 12.F. Bezrukov, M. Shaposhnikov, Standard model Higgs boson mass from inflation: two loop analysis. JHEP 0907, 089 (2009). arXiv:0904.1537 [hep-ph]ADSCrossRefGoogle Scholar
- 13.F. Bezrukov, A. Magnin, M. Shaposhnikov, S. Sibiryakov, Higgs inflation: consistency and generalisations. JHEP 1101, 016 (2011). arXiv:1008.5157 [hep-ph]ADSCrossRefMATHGoogle Scholar
- 14.A.O. Barvinsky, A.Y. Kamenshchik, A.A. Starobinsky, Inflation scenario via the Standard model Higgs boson and LHC. JCAP 0811, 021 (2008). arXiv:0809.2104 [hep-ph]ADSCrossRefGoogle Scholar
- 15.A.O. Barvinsky, A.Y. Kamenshchik, C. Kiefer, A.A. Starobinsky, C. Steinwachs, Asymptotic freedom in inflationary cosmology with a non-minimally coupled Higgs field. JCAP 0912, 003 (2009). arXiv:0904.1698 [hep-ph]ADSCrossRefGoogle Scholar
- 16.A.O. Barvinsky, A.Y. Kamenshchik, C. Kiefer, A.A. Starobinsky, C. Steinwachs, Higgs boson, renormalization group, and naturalness in cosmology. Eur. Phys. J. C 72, 2219 (2012). arXiv:0910.1041 [hep-ph]ADSCrossRefGoogle Scholar
- 17.A. De Simone, M.P. Hertzberg, F. Wilczek, Running inflation in the standard model. Phys. Lett. B 678, 1 (2009). arXiv:0812.4946 [hep-ph]ADSCrossRefGoogle Scholar
- 18.T.E. Clark, B. Liu, S.T. Love, T. ter Veldhuis, The standard model Higgs Boson-inflaton and dark matter. Phys. Rev. D 80, 075019 (2009). arXiv:0906.5595 [hep-ph]ADSCrossRefGoogle Scholar
- 19.A.V. Bednyakov, B.A. Kniehl, A.F. Pikelner, O.L. Veretin, Stability of the electroweak vacuum: gauge independence and advanced precision. arXiv:1507.08833 [hep-ph]
- 20.V. Branchina, E. Messina, Stability, Higgs boson mass and new physics. Phys. Rev. Lett. 111, 241801 (2013). arXiv:1307.5193 [hep-ph]ADSCrossRefGoogle Scholar
- 21.V. Branchina, E. Messina, Stability and UV completion of the standard model. arXiv:1507.08812 [hep-ph]
- 22.V. Branchina, E. Messina, A. Platania, Top mass determination, Higgs inflation, and vacuum stability. JHEP 1409, 182 (2014). arXiv:1407.4112 [hep-ph]ADSCrossRefGoogle Scholar
- 23.V. Branchina, E. Messina, M. Sher, Lifetime of the electroweak vacuum and sensitivity to Planck scale physics. Phys. Rev. D 91, 013003 (2015). arXiv:1408.5302 [hep-ph]ADSCrossRefGoogle Scholar
- 24.[ATLAS and CDF and CMS and D0 Collaborations], First combination of Tevatron and LHC measurements of the top-quark mass. arXiv:1403.4427 [hep-ex]
- 25.N. Okada, Q. Shafi, Higgs inflation, seesaw physics and fermion dark matter. Phys. Lett. B 747, 223 (2015). arXiv:1501.05375 [hep-ph]
- 26.S. Di Vita, C. Germani, Electroweak vacuum stability and inflation via non-minimal derivative couplings to gravity. arXiv:1508.04777 [hep-ph]
- 27.M.B. Einhorn, D.R.T. Jones, Inflation with non-minimal gravitational couplings in supergravity. JHEP 1003, 026 (2010). arXiv:0912.2718 [hep-ph]ADSCrossRefMATHGoogle Scholar
- 28.M.B. Einhorn, D.R.T. Jones, GUT scalar potentials for Higgs inflation. JCAP 1211, 049 (2012). arXiv:1207.1710 [hep-ph]ADSCrossRefGoogle Scholar
- 29.S. Ferrara, R. Kallosh, A. Linde, A. Marrani, A. Van Proeyen, Jordan frame supergravity and inflation in NMSSM. Phys. Rev. D 82, 045003 (2010). arXiv:1004.0712 [hep-th]ADSCrossRefGoogle Scholar
- 30.S. Ferrara, R. Kallosh, A. Linde, A. Marrani, A. Van Proeyen, Superconformal symmetry, NMSSM, and inflation. Phys. Rev. D 83, 025008 (2011). arXiv:1008.2942 [hep-th]ADSCrossRefGoogle Scholar
- 31.M. Arai, S. Kawai, N. Okada, Higgs inflation in minimal supersymmetric SU(5) GUT. Phys. Rev. D 84, 123515 (2011). arXiv:1107.4767 [hep-ph]ADSCrossRefGoogle Scholar
- 32.M. Arai, S. Kawai, N. Okada, Supersymmetric standard model inflation in the Planck era. Phys. Rev. D 86, 063507 (2012). arXiv:1112.2391 [hep-ph]ADSCrossRefGoogle Scholar
- 33.M. Arai, S. Kawai, N. Okada, Higgs-lepton inflation in the supersymmetric minimal seesaw model. Phys. Rev. D 87(6), 065009 (2013). arXiv:1212.6828 [hep-ph]
- 34.S. Kawai, N. Okada, TeV scale seesaw from supersymmetric Higgs-lepton inflation and BICEP2. Phys. Lett. B 735, 186 (2014). arXiv:1404.1450 [hep-ph]ADSCrossRefGoogle Scholar
- 35.C. Pallis, N. Toumbas, Non-minimal Higgs inflation and non-thermal leptogenesis in a supersymmetric Pati-Salam model. JCAP 1112, 002 (2011). arXiv:1108.1771 [hep-ph]ADSCrossRefGoogle Scholar
- 36.S. Kawai, J. Kim, Testing supersymmetric Higgs inflation with non-Gaussianity. Phys. Rev. D 91(4), 045021 (2015). arXiv:1411.5188 [hep-ph]
- 37.N. Okada, M.U. Rehman, Q. Shafi, Non-minimal B-L inflation with observable gravity waves. Phys. Lett. B 701, 520 (2011). arXiv:1102.4747 [hep-ph]
- 38.Y. Hamada, H. Kawai, K.Y. Oda, S.C. Park, Higgs inflation is still alive after the results from BICEP2. Phys. Rev. Lett. 112(24), 241301 (2014). doi:10.1103/PhysRevLett.112.241301. arXiv:1403.5043 [hep-ph]
- 39.F. Bezrukov, M. Shaposhnikov, Higgs inflation at the critical point. Phys. Lett. B 734, 249 (2014). arXiv:1403.6078 [hep-ph]ADSCrossRefGoogle Scholar
- 40.P. Minkowski, Phys. Lett. B 67, 421 (1977)ADSCrossRefGoogle Scholar
- 41.T. Yanagida, in Proceedings of the Workshop on the Unified Theory and the Baryon Number in the Universe eds. by O. Sawada, A. Sugamoto (KEK, Tsukuba, 1979), p. 95Google Scholar
- 42.M. Gell-Mann, P. Ramond, R. Slansky, Supergravity ed. by P. van Nieuwenhuizen et al. (North Holland, Amsterdam, 1979), p. 315Google Scholar
- 43.S.L. Glashow, The future of elementary particle physics, in Proceedings of the 1979 Cargèse Summer Institute on Quarks and Leptons ed. by M. Lévy et al. (Plenum Press, New York, 1980) p. 687Google Scholar
- 44.R.N. Mohapatra, G. Senjanović, Neutrino mass and spontaneous parity violation. Phys. Rev. Lett. 44, 912 (1980)ADSCrossRefGoogle Scholar
- 45.J. Schechter, J.W.F. Valle, Neutrino masses in SU(2) x U(1) theories. Phys. Rev. D 22, 2227 (1980)ADSCrossRefGoogle Scholar
- 46.F. Bezrukov, D. Gorbunov, Light inflaton after LHC8 and WMAP9 results. JHEP 1307, 140 (2013). arXiv:1303.4395 [hep-ph]ADSCrossRefGoogle Scholar
- 47.D.P. George, S. Mooij, M. Postma, Quantum corrections in Higgs inflation: the real scalar case. JCAP 1402, 024 (2014). arXiv:1310.2157 [hep-th]ADSMathSciNetCrossRefGoogle Scholar
- 48.D.P. George, S. Mooij, M. Postma, Top-Goldstone coupling spoils renormalization of Higgs inflation. arXiv:1408.7079 [hep-th]
- 49.D.P. George, S. Mooij, M. Postma, Quantum corrections in Higgs inflation: the standard model case. arXiv:1508.04660 [hep-th]
- 50.F. Bezrukov, J. Rubio, M. Shaposhnikov, Living beyond the edge: Higgs inflation and vacuum metastability. Phys. Rev. D 92(8), 083512 (2015). doi:10.1103/PhysRevD.92.083512. arXiv:1412.3811 [hep-ph]
- 51.G. Aad et al. [ATLAS Collaboration], Search for high-mass dilepton resonances in pp collisions at \(\sqrt{s}=8\) TeV with the ATLAS detector. Phys. Rev. D 90(5), 052005 (2014). arXiv:1405.4123 [hep-ex]
- 52.CMS Collaboration [CMS Collaboration], Search for resonances in the dilepton mass distribution in pp collisions at sqrt(s) = 8 TeV. CMS-PAS-EXO-12-061Google Scholar
- 53.V. Khachatryan et al. [CMS Collaboration], Search for physics beyond the standard model in dilepton mass spectra in proton-proton collisions at \( \sqrt{s}=8 \) TeV. JHEP 1504, 025 (2015). arXiv:1412.6302 [hep-ex]
- 54.F. Bezrukov, D. Gorbunov, M. Shaposhnikov, On initial conditions for the Hot Big Bang. JCAP 0906, 029 (2009). doi:10.1088/1475-7516/2009/06/029. arXiv:0812.3622 [hep-ph];
- 55.J. Garcia-Bellido, D.G. Figueroa, J. Rubio, Preheating in the standard model with the Higgs-inflaton coupled to gravity. Phys. Rev. D 79, 063531 (2009). doi:10.1103/PhysRevD.79.063531. arXiv:0812.4624 [hep-ph]
- 56.A. Anisimov, Y. Bartocci, F.L. Bezrukov, Inflaton mass in the nuMSM inflation. Phys. Lett. B 671, 211 (2009). arXiv:0809.1097 [hep-ph]ADSCrossRefGoogle Scholar
- 57.F. Bezrukov, D. Gorbunov, Light inflaton Hunter’s guide. JHEP 1005, 010 (2010). arXiv:0912.0390 [hep-ph]ADSCrossRefMATHGoogle Scholar
Copyright information
Open AccessThis article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.
Funded by SCOAP^{3}.