1 Introduction
Abstract

We present a new approach for generating tiny neutrino masses. The Dirac neutrino mass matrix gets contributions from two new Higgs doublets with their vevs at the electroweak (EW) scale. Neutrino masses are tiny not because of tiny Yukawa couplings, or very heavy () right handed neutrinos. They are tiny because of a cancelation in the Dirac neutrino mass matrix (fine tuning). After fine tuning to make the Dirac neutrino mass matrix at the GeV scale, light neutrino masses are obtained in the correct scale via the see-saw mechanism with the right handed neutrino at the EW scale. The proposal links neutrino physics to collider physics. The Higgs search strategy is completely altered. For a wide range of Higgs masses, the Standard Model Higgs decays dominantly to mode giving rise to the final state , or . This can be tested at the LHC, and possibly at the Tevatron.

OSU-HEP-10-03

Neutrino Masses from Fine Tuning

B. N. Grossmann111Email address: benjamin.grossmann@okstate.edu, Z. Murdock222Email address: zeke.murdock@okstate.edu, and S. Nandi333Email address: s.nandi@okstate.edu

Department of Physics and Oklahoma Center for High Energy Physics,

Oklahoma State University, Stillwater, Oklahoma, 74078




1 Introduction

In the past decade, the existence of tiny neutrino masses of the order of one hundredth to one tenth of an electron volt has been firmly established through atmospheric, solar and reactor neutrino experiments [1][2][3]. These masses are a million or more times smaller than the corresponding charged lepton masses. While the quark and charged lepton masses span many orders of magnitude, the neutrino masses do not. The square roots of the neutrino mass square differences, as obtained from the neutrino oscillation experiments, lie within a factor of six of each other. Also the quark mixing angles are very small, whereas two of the neutrino mixing angles are large [4]. These observations have led to several unanswered questions. Why are the neutrino masses so small compared to the corresponding charged lepton or quark masses? Why is there such a large hierarchy among the charged fermion masses, while there is practically no hierarchy among the neutrino masses? Also, unlike the quark sector why are the mixing angles in the neutrino sector large? Another related fundamental question is whether neutrinos are Majorana or Dirac particles, and whether the light neutrino spectrum exhibit a normal hierarchy or an inverted hierarchy.

The most popular idea proposed so far for understanding the tiny neutrino mass is the famous see-saw mechanism [5]. One postulates the existence of very massive Standard Model (SM) singlet right handed neutrinos with Majorana masses of the order of . The Yukawa couplings of the left-handed (LH) neutrino to these heavy right-handed (RH) neutrinos then gives a Dirac mass of the order of the charged lepton masses, . As a result, the left-handed neutrino obtains a tiny mass of the order of . Although there are several indirect benefits for its existence, there is no direct experimental evidence for such a heavy particle. The mass scale is so high that no connection can be made with the physics to be explored at the high energy colliders such as the Tevatron and the LHC. It is important to explore other possibilities to explain the tiny neutrino masses. Also, the see-saw mechanism does not naturally lead to close values of the neutrino masses as observed experimentally, though such close masses can be arranged with the appropriate choice of the right handed Majorana sector.

Recent astrophysical observation requires a tiny but non-zero value of the cosmological constant, eV). This value is surprisingly close to the value of the light neutrino masses required from the neutrino oscillation experiments, eV. It has been exceedingly difficult to derive such a tiny value of the cosmological constant, and there is some acceptance that it may be fine tuned. The idea of Higgs mass also being fine tuned has been explored leading to the so called “Split Supersymmetry” [6] with interesting implications at the TeV scale that can be explored at the LHC. Neutrino masses being in the same ballpark as the cosmological constant, it is not unreasonable to assume that their values are also fine tuned. The objective in this project is to adopt this philosophy, build a concrete model realizing this scenario, and explore its phenomenological implications, especially for the LHC.

In this work, we present a model in which the light neutrinos get their masses from the usual see-saw mechanism, except the right handed neutrino masses are at the EW scale. The neutrino Dirac masses get contributions from two different Higgs doublets with their vacuum expectation values (vevs) at the electroweak scale. The neutrino masses are small not because of tiny Yukawa couplings or a tiny vev of a new Higgs doublet [7]. In fact, we take the Yukawa couplings to be of order one. The smallness of the light neutrino masses are due to the cancellation in the Dirac neutrino mass matrix, making and giving rise to light neutrino masses where is the RH Majorana neutrino mass. Thus with in the EW scale, we get the light neutrino masses in the correct range of eV.

Our work is presented as follows: In section 2, we present the model and the formalism. In section 3, we discuss the phenomenological implications of the model, especially how it alters the usual SM Higgs decay modes, and its implications for the Higgs search at the LHC. Section 4 contains our conclusions.

2 Model and Formalism

2.1 Our model

Our model is based on the SM gauge symmetry supplemented by a discrete symmetry. In addition to the SM fermions and the Higgs doublet , we introduce three RH neutrinos , where , and two additional Higgs doublets and , with vevs at the EW scale. All the SM particles are even under the symmetry, while the three RH neutrinos and the two new Higgs doublets and are odd under . The symmetry is softly broken by the bilinear Higgs terms. With this symmetry, the Yukawa interactions are given by

(1)

where the fermion fields represent three families, and , , and represent three corresponding Yukawa coupling matrices.

(2)
(3)

Note that from the above equations, the neutrino mass matrix is obtained to be

(4)

The Dirac mass matrix is given by

(5)

Here and are the vevs of the new Higgs fields and . For the mass scales in which , the light neutrino mass matrix is given by

(6)

Note that experimentally masses of the light neutrinos are in the eV range. Thus with in the EW scale, the matrix needs to be in the scale of GeV. Since the vevs and are in the EW scale, we can get in the GeV scale by assuming the Yukawa couplings to be very tiny, of order . Such a path, similar to the usual see-saw, will not lead to any interesting implications for neutrino physics in the TeV scale. Instead we assume that the Yukawa couplings and are , and these Yukawa couplings and vevs and are fined tuned to get in the GeV. This is our approach to the smallness of the light neutrino mass scale. As we will see, this gives interesting implication for neutrino physics at the TeV scale, and can be explored at the LHC.

2.2 Higgs potential

Now we discuss the Higgs sector of the model. In addition to the usual SM Higgs two other Higgs doublets , are required in this model. These two new Higgs doublets couple only to the neutrinos, and this is imposed using the symmetry. It is the cancelation of contributions to the Dirac neutrino mass from these two new doublets that enable the use of fine tuning.

We assume that the symmetry is softly broken by the bilinear terms in the Higgs Potential. The two new doublets will mix with the SM Higgs doublet, and as we will see, this will produce entirely new signals for the SM Higgs boson decays. The Higgs potential is given by

(7)
(8)
(9)

Note that the odd part of the potential breaks the symmetry softly. This will have interesting implications for the SM Higgs boson decays.

(10)

Since there are three Higgs doublets, after EW symmetry breaking, there will remain a pair of charged Higgs (), five neutral scalar Higgses (), and two neutral pseudoscalar Higgses (). Due to the breaking of the symmetry, there is mixing within each of these three groups of Higgses (but not between groups). We denote the mass eigenstates of the five neutral Higgses by , , , , and .

2.3 Mixing between the light and heavy neutrinos

In our model, we are considering a scenario in which the three RH neutrinos have masses in the EW scale with Yukawa couplings with the light LH neutrinos. They will also mix with the light neutrinos, and thus will participate in the gauge interactions. LEP has searched for such RH neutrinos. Before we discuss these constraints, let us first consider the mixing between the light neutrinos and the RH neutrinos. Using the observed values of the light neutrino masses and mixings, we can make a reasonable estimate of the mixing between the LH and RH neutrinos as follows. We use the normal hierarchy for the light neutrino masses with the values

(11)

The mixing matrix follows the standard parametrization. The angles are the central values, and is the maximal value allowed by current experiment [8].

(12)
(13)

The three possible CP-violating phases are assumed to be zero. From the above mass eigenvalues and the mixing matrix, we can calculate the light neutrino mass matrix using

(14)

For simplicity, we assume that the RH Majorana mass matrix to be proportional to the unit matrix,

(15)

As a consequence of this choice for and having a symmetric , the mixing matrix among only the generations of heavy neutrinos is equivalent to the mixing matrix among only the generations of light neutrinos . Using the above numbers and choosing , we can now calculate numerically the Dirac neutrino mass matrix from the equation

(16)

There are four sets of real solutions for . Only two sets of solutions are shown in Eqs. (17) and (18). The other two are just the negatives of these two sets.

(17)
(18)

Using the solutions for and , we can now use the full neutrino mass matrix and calculate the full mixing matrix and the mixing angles between the heavy and light neutrinos.

(19)

It turns out that

(20)

For solution set 1, the full rotation matrix is

(21)

For solution set 2, the full rotation matrix is

(22)
Set 1
Set 2
Table 1: Mixing angles between the light neutrinos (subscripts ) and the heavy neutrinos (subscripts ).

As can be seen on Table 1, the mixing between the heavy and light neutrinos is extremely small.

3 Phenomenological implications

In this section, we discuss the phenomenological implications of our model. We are considering RH neutrinos at the EW scale. Their mass can be below the boson mass. Thus they can be searched for at LEP, Tevatron, and at the LHC. First we discuss the constraints that already exist from the search at LEP.

3.1 LEP constraints

Searches for have been conducted at LEP in the channel , with subsequently decaying to or . This experiment puts limits on the mixing angle between the heavy and the light neutrinos for GeV GeV, and for GeV [9]. As we discussed in previous section, the mixing angles between the light and heavy neutrinos are extremely small, ranging between to . Thus, in our model, LEP constraints allow small masses for the heavy Majorana neutrinos.

3.2 Higgs decays and Higgs signals

In our model, the Yukawa couplings between the light neutrinos, the heavy Majorana neutrinos and the new Higgs fields and are . The SM Higgs mixes with the new Higgses, and these mixings are naturally large. Thus, for , the SM Higgs will dominantly decay to a light and , as soon as this decay mode becomes kinematically allowed, because the coupling for this decay mode is much larger than the usually dominant mode, or even the mode. The branching ratios for the various Higgs decay modes are shown in Fig. 1 for GeV, for the Yukawa couplings, and . As can be seen from the plot, as soon as the decay mode becomes kinematically allowed, this mode totally dominates over the usual mode, and is larger than the usually dominant mode even beyond the threshold. Thus in our model, the SM Higgs decay mode is greatly altered. A second plot is shown for Yukawa couplings equal to in Fig. 2

Figure 1: Branching ratios of with the coupling between and , .
Figure 2: Branching ratios of with .

At hadron colliders, the SM Higgs boson is dominantly produced via gluon fusion with the top quark in the loop. In our model, because of the mixing of with and , the lightest mass neutral scalar Higgs decays dominantly as .

Figure 3: Decay modes of .

The final state signal will depend on the decay modes of . Two of the allowed decay modes of are shown in Fig. 3. The 3-body decay mode is completely dominant over the 2-body decay mode or . This is because the 2-body decay is suppressed by the tiny mixing angle, or smaller. Thus the final state signals for the Higgs bosons at the LHC, in our model, is . Collider signals will include large missing energy and 2 hard b-jets.

Using Madgraph, we generated events for in the SM for LHC at 14 TeV, 7 TeV, and Tevatron. Using the cuts GeV, and the for each b-jet to be greater than GeV, we find the cross section to be pb, for the LHC at 14 TeV. This provides a reasonable estimate of the background. The cross section for Higgs production at the LHC at TeV is pb for a 120 GeV Higgs. For a large mass range of the Higgs boson in our model, the branching ratio, . Thus, prior to any cuts on the signal, this mode is observable at the LHC, and stands out over the SM background. A summary for different energies is given in Table 2. The Higgs production at the Tevatron is taken from [10]. For the LHC we used [11].

Collider Energy Background Signal
LHC 14 TeV 13 pb 50 pb
LHC 7 TeV 2.4 pb 30 pb
Tevatron 2 TeV 240 fb 1 pb
Table 2: Collider Searches for .

3.3 Search at Tevatron

The D0 collaboration at the Tevatron has searched for the SM Higgs boson in the channel using 5.2 of data. With both ’s being tagged and a and for the b-jets, they expect about 5 events for the mode. However, there is a large SM background arising mainly from + jets, + jets, and . The estimated background with these cuts is about events, while they observe 514 events. Thus the SM signal from production for this mode is not observable with the current Tevatron data. However in our model, depending on the , this signal is much larger and may be observable, especially as luminosity accumulates in the coming year. Other possibilities for our model are that the RH neutrinos could decay via a charged Higgs.

3.4 Decays via Charged Higgs

For a sufficiently light , the decay via a charged Higgs becomes important. Taking the Yukawa couplings to be order one, and the mixing to be maximal between the three Higgs doublets, the decay rates for the decays are shown in Table 3. Taking the tau and , the cross section for at the Tevatron is 45 fb (123 fb at the LHC for 7 TeV collisions). This background is much smaller than background, as it is a leptonic (not QCD) process. This signature, two high taus plus missing energy, may be easier to see.

Figure 4: Decay modes of through a charged Higgs .
Decay Mode (GeV) (GeV) BR
200 43.8%
200 37.0%
200 16.3%
200 1.85%
200 1.12%
250 63.6%
250 22.9%
250 9.21%
250 2.69%
250 1.65%
Table 3: Decay Rates of for , .

4 Conclusions

We have proposed a new approach for understanding of the tininess of the light neutrino masses. We extend the SM gauge symmetry by a discrete symmetry, and the particle content by adding three right handed neutrinos and two additional Higgs doublets. These new Higgs doublets couple only to the neutrinos. The tiny neutrino masses are generated via the see-saw mechanism with the right handed neutrino mass matrix at the EW scale, and the Dirac neutrino mass matrix at the GeV scale. The Dirac neutrino mass matrix gets contribution from the two new EW Higgs doublets with vevs at the EW scale. The Yukawa couplings are of order one, and the two EW contributions are fine tuned to achieve the Dirac neutrino mass matrix at the GeV level. The model links neutrino physics to collider physics at the TeV scale. The SM Higgs decays are drastically altered. For a wide range of the Higgs mass, it decays dominantly to giving rise to the final state , or . This can be tested a at the LHC and possibly at the Tevatron.

Acknowledgments

We thank K. S. Babu, W.A. Bardeen, B. Dobrescu, C. T. Hill and A. Khanov for useful discussions. Part of this work was done during our visit to Fermilab in Fall, 2009. We thank the Fermilab Theory Group for warm hospitality and support during this visit. This work is supported in part by the United States Department of Energy, Grant Numbers DE-FG02-04ER41306 and DE-FG02-04ER46140.

References

  • [1] Super-Kamiokande Collaboration, Y. Ashie et al., Phys. Rev. D 71 (2005) 11205; Super-Kamiokande Collaboration, Y. Ashie et al., Phys. Rev. Lett. 93 (2004) 101801.
  • [2] SNO Collaboration, S.N. Ahmed et al.,nucl-ex/0309004; SNO Collaboration, Q.R. Ahmad et al., Phys. Rev. Lett. 89 (2002) 011301; Super-Kamiokande Collaboration, S. Fukuda et al., Phys. Lett. B 539 (2002) 179; Super-Kamiokande Collaboration, M.B. Smy et al., Phys. Rev. D 69 (2004) 011104.
  • [3] For a recent comprehensive review, see for example, R.N. Mohapatra et al., hep-ph/0510213.
  • [4] C. Amsler et al. (Particle Data Group), Physics Letters B667, 1 (2008) and 2009 partial update for the 2010 edition.
  • [5] P. Minkowski, Phys. Lett. B 67 (1977) 421, M. Gell-Mann, P. Ramond, and R. Slansky, Supergravity (P. van Nieuwenhuizen et al. eds.), North Holland, Amsterdam, 1980, p. 315; T. Yanagida, in Proceedings of the Workshop on the Unified Theory and the Baryon Number in the Universe (O. Sawada and A. Sugamoto, eds.), KEK, Tsukuba, Japan, 1979, p. 95; S. L. Glashow, The future of elementary particle physics, in Proceedings of the 1979 Carg‘ese Summer Institute on Quarks and Leptons (M. L´evy et al. eds.), Plenum Press, New York, 1980, pp. 687–71 R. N. Mohapatra and G. Senjanovi´c, Phys. Rev. Lett. 44 (1980) 912.
  • [6] N. Arkani-Hamed and S. Dimopoulos, JHEP 0506, 073 (2005) [arXiv:hep-th/0405159].
  • [7] S. Gabriel and S. Nandi, Phys. Lett. B 655, 141 (2007) [arXiv:hep-ph/0610253]. S. Gabriel, B. Mukhopadhyaya, S. Nandi and S. K. Rai, Phys. Lett. B 669, 180 (2008) [arXiv:0804.1112 [hep-ph]].
  • [8] The CHOOZ Collaboration, Phys. Lett. B420:397-404 (1998).
  • [9] P. Achard et al. [L3 Collaboration], Phys. Lett. B 517, 67 (2001) [arXiv:hep-ex/0107014].
  • [10] J. Baglio and A. Djouadi, arXiv:1003.4266 [hep-ph].
  • [11] F. Stockli and R. Suarez, http://wwweth.cern.ch/HiggsCrossSections/HiggsCrossSection.html
  • [12] V. M. Abazov et al. [D0 Collaboration], Phys. Rev. Lett. 104, 071801 (2010) [arXiv:0912.5285 [hep-ex]].
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
165584
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description