9512.net

甜梦文库

甜梦文库

当前位置：首页 >> >> # Nambu-Goldstone and Massive Modes in Gravitational Theories with Spontaneous Lorentz Breaki

Nambu-Goldstone and Massive Modes in Gravitational Theories with Spontaneous Lorentz Breaking

arXiv:0801.1711v2 [gr-qc] 17 Apr 2008

R. Bluhm Physics Department, Colby College, Waterville, ME 04901, USA E-mail: rtbluhm@colby.edu

Spontaneous breaking of local Lorentz symmetry is of interest as a possible mechanism originating from physics at the Planck scale. If such breaking occurs, however, it raises the questions of what the fate of the Nambu-Goldstone modes is, whether a Higgs mechanism can occur, and whether additional massive modes (analogous to the Higgs particle) can appear. A summary of some recent work looking at these questions is presented here.

1

Introduction

The idea that Lorentz symmetry might be spontaneously broken began to catch on when it was shown that mechanisms in string theory might lead to this form of symmetry breaking.1 Since then, spontaneous Lorentz breaking has been examined in its own right in a number of contexts, including investigating its phenomenological e?ects and its e?ects on gravity. However, as soon as a theory allows spontaneous breaking of a symmetry, well-known consequences from particle physics must be considered and addressed. The ?rst is the Goldstone theorem, which states that when a continuous symmetry is spontaneously broken, massless Nambu-Goldstone (NG) modes appear. The second is the possibility of a Higgs mechanism, resulting in massive gauge ?elds, for the case when the symmetry is local. The third is the possibility that additional massive modes might appear (analogous to the Higgs boson in the case of the electroweak model). Clearly, all three of these can have physical implications and must be accounted for in any theory with spontaneous symmetry breaking. In this work, these processes are examined for the case where it is Lorentz symmetry that is spontaneously broken.1,2,3,4 First, the fate of the NG modes is examined. Then, since Lorentz symmetry is a local symmetry in the context of gravity, the possibility of a Higgs mechanism is considered. Lastly, the possibility of additional massive modes (analogous to the Higgs particle) is considered as well. An explicit illustration of these processes is given for the case of a bumblebee model, in which a vector ?eld acquires a nonzero vacuum value. 1

2

Spontaneous Lorentz Breaking

In a gravitational theory, Lorentz symmetry acts in local frames, transforming tensor components with respect to a local basis, e.g., Tabc (where Latin indices denote components with respect to a local frame). Similarly, di?eomorphisms act in the spacetime manifold, transforming components with respect to the spacetime coordinate system, e.g., Tλ?ν (denoted using Greek indices). These local and spacetime tensor components are linked by a vierbein. For example, the spacetime metric and local Minkowski metric are related by g?ν = e?a eνb ηab . (1)

With a vierbein formalism, spinors can naturally be incorporated into a theory. A vierbein formalism also parallels gauge theory, with Lorentz symmetry acting as a local symmetry group. The spin connection ω?ab enters in covariant derivatives that act on local tensor components and plays the role of the gauge ?eld for the Lorentz symmetry. In contrast, the metric excitations, e.g., h?ν = g?ν ? η?ν , act as the gauge ?elds for the di?eomorphism symmetry. In the context of a vierbein formalism, there are primarily two geometries that can be distinguished. In a Riemannian geometry (with no torsion), the spin connection is nondynamical and does not propagate. However, in a RiemannCartan geometry (with nonzero torsion), the spin connection must be treated as independent degrees of freedom that in principle can propagate. Local Lorentz symmetry is spontaneously broken when a local tensor ?eld acquires a nonzero vacuum expectation value (vev), e.g., for the case of a three-component tensor, < Tabc > = tabc . (2) Spontaneous Lorentz breaking can be introduced into a theory dynamically by adding a potential term V to the Lagrangian. For example, a potential of the form V ? (Tλ?ν g λα g ?β g νγ Tαβγ ± t2 )2 , (3) consisting of a quadratic function of products of the tensor components Tλ?ν , has a minimum when Tλ?ν g λα g ?β g νγ Tαβγ = ? t2 . (4)

Solutions of Eq. (4) span a degenerate space of possible vacuum solutions. Spontaneous Lorentz breaking occurs when a particular vacuum value tabc in the local frame is chosen, obeying ?t2 = tabc η pa η qb η rc tpqr , where the sign depends on the timelike or spacelike nature of the tensor. 2

3

Nambu-Goldstone Modes

Consider a theory with a tensor vev in a local Lorentz frame, < Tabc > = tabc , which spontaneously breaks Lorentz symmetry. Since the vacuum value for the vierbein is also a constant or ?xed function, e.g., < e?a > = δ?a , the spacetime tensor therefore has a vev as well, < Tλ?ν > = tλ?ν . (5)

This means that when Lorentz symmetry is spontaneously broken, di?eomorphisms are spontaneously broken as well. This implies that NG modes should appear (in the absence of a Higgs mechanism) for both of these broken symmetries. In general, the NG modes consist of ?eld excitations that stay within the minimum of the potential V . They therefore obey the condition (4). A solution of this condition is given in terms of the vierbein and the local vev, Tλ?ν = eλa e?b eνc tabc . (6)

As a general rule, there can be up to as many NG modes as there are broken symmetries. Since the maximal case corresponds to six broken Lorentz generators and four broken di?eomorphisms, there can therefore be up to ten NG modes. Where do the NG modes reside? In general, the answer depends on the choices of gauge. However, one natural choice is to put all of the NG modes into the vierbein. A counting argument shows this is possible. The vierbein e?a has 16 components. With no spontaneous Lorentz violation, typically the six Lorentz and four di?eomorphism degrees are used to gauge away ten components, leaving up to six independent degrees of freedom. (Note that a general gravitational theory can have up to six propagating metric modes, but general relativity is special in that there are only two). In contrast, in a theory with spontaneous Lorentz breaking, up to all ten NG modes can potentially propagate as additional degrees of freedom in the vierbein. 4 Gravitational Higgs Mechanisms

With two sets of broken symmetries, local Lorentz transformations and di?eomorphisms, there are potentially two types of Higgs mechanisms. Furthermore, there is the possibility that additional massive modes can exist as excitations that do not stay in the minimum of the potential V . For the case of the broken di?eomorphisms. it was shown that the conventional Higgs mechanism involving the metric does not occur.1 This is because the mass term that is generated by covariant derivatives involves the connection, which consists of derivatives of the metric and not the metric itself. As a 3

result, no mass term for the metric is generated according to the usual Higgs mechanism. However, it was also shown that because of the form of the potential, e.g., as in Eq. (3), quadratic terms involving the metric can arise. This results in an alternative form of the Higgs mechanism1 that has no direct analogue in nonabelian gauge theory. (In nonabelian gauge theory, the potential V involves only the scalar Higgs ?elds and not the gauge ?elds. In contrast here, both the metric and tensor ?elds enter in the massive-?eld excitations). The additional mass terms that arise in this alternative Higgs mechanism can potentially modify gravity in a way that avoids the van Dam, Veltmann, and Zakharov discontinuity.5 They are therefore potentially interesting in studies of modi?ed gravity theory. In contrast, for the case of the broken Lorentz symmetry, it is found that a conventional Higgs mechanism can occur.3 In this case, the relevant gauge ?eld is the spin connection. This ?eld appears directly in covariant derivatives acting on local tensor components, and for the case where the local tensors acquire a vev, quadratic mass terms for the spin connection can be generated. However, a viable Higgs mechanism involving the spin connection can occur only if the spin connection is a dynamical (i.e., propagating) ?eld. This then requires that there is nonzero torsion and that the geometry is Riemann-Cartan. As a result, a conventional Higgs mechanism for the spin connection is possible, but only in a Riemann-Cartan geometry. However, even if torsion is permitted, constructing a viable model with a massive propagating spin connection that is ghost- and tachyon-free remains a challenging and open problem.3 Therefore, for simplicity in the remainder of this work, a Riemann spacetime (with no torsion) is assumed. In this restricted context, the only possible process giving rise to massive modes is the alternative Higgs mechanism, in which massive modes are due to excitations that do not stay in the minimum of the potential V. 5 Bumblebee Models

To investigate further the e?ects of NG and massive modes in theories with spontaneous Lorentz violation, it is useful to work in the context of a de?nite model. The simplest example involves a vector ?eld with a nonzero vev. Models of this type are known as bumblebee models.1,2 Examples have been studied in various forms by a number of authors.1,2,3,4,6,7,8,9,10,11,12,13,14,15,16,17 Bumblebee models are de?ned as ?eld theories with a vector ?eld B? that acquires a nonzero vev, < B? > = b? . The vev is induced by a potential V in the Lagrangian that has a minimum when the vacuum solution holds. Bumblebee models can be de?ned with generalized kinetic terms for the vector 4

and gravitational ?elds. However, for brevity, an example with a Maxwell kinetic term is considered here. The Lagrangian then has the form L = LG + LB + LM , where LG describes the pure-gravity sector, LM describes the matter sector (including possible interactions with B? ), and LB = ? 1 B?ν B ?ν ? V (B? B ? ± b2 ), 4 (7)

describes the bumblebee ?eld. (For simplicity, additional possible interactions between the curvature tensor and B? are neglected here as well). The bumblebee ?eld strength in Riemann spacetime is B?ν = ?? Bν ? ?ν B? . A noteworthy feature of all bumblebee models is that they do not have local U (1) gauge symmetry. This symmetry is broken explicitly by the presence of the potential V . However, it is common to include couplings to matter that involve the notion of charge in the matter sector. For example, terms involving current couplings with charged matter can be included by de?ning, LM = B? J ? with D? J ? = 0. In this case, the theory has a global U (1) symmetry that gives rise to charge conservation in the matter sector. This assumption also implies that initial values can be chosen that maintain stability of the Hamiltonian.4 Di?erent forms of the potential V can be considered. One example is a smooth quadratic potential,

1 V = 2 κ(B? B ? ± b2 )2 ,

(8)

where κ is a constant (of mass dimension zero). This type of potential allows both NG excitations (that stay within the potential minimum) as well as massive excitations (that do not). An alternative would be to consider a linear Lagrange-multiplier potential V = λ(B? B ? ± b2 ), (9)

where the Lagrange-multiplier ?eld λ imposes a constraint that only allows NG excitations in B? and excludes massive-mode excitations. However, for de?niteness here, the smooth potential (8) is chosen, which allows a massivemode excitation. For such a bumblebee model, three Lorentz symmetries and one di?eomorphism are broken. Therefore, up to four NG modes can appear. However, the di?eomorphism NG mode is found not to propagate.3 It drops out of the kinetic terms and is purely an auxiliary ?eld. In contrast, the Lorentz NG modes do appear in the form of two massless transverse modes and one auxiliary mode. These have properties similar to the photon in electrodynamics, which raises the interesting possibility that photons might be described as NG modes in theories with spontaneous Lorentz violation.3 Previous links between 5

QED gauge ?elds, fermion composites, and NG modes have been uncovered in ?at spacetime (with global Lorentz symmetry).18 However, bumblebee models are di?erent. They consist of theories with a noncomposite vector ?eld, have no local U(1) gauge symmetry, and give rise to photons as NG modes in the presence of gravity. Note that bumblebee models also include possible couplings between the vacuum value b? and a matter current J ? . Such an interaction can provide an unmistakable signature of physical Lorentz violation that would distinguish it from any gauge-?xed form of QED. Note as well that any such signal would be contained in the Standard-Model Extension(SME).19 Thus, on-going investigations of Lorentz breaking using the SME have sensitivity to all signals of spontaneous Lorentz breaking involving couplings between matter and the background vevs. To determine more thoroughly whether conventional Einstein-Maxwell solutions can emerge from bumblebee models, the role of the massive mode must be investigated.4 This mode constitutes an additional degree of freedom beyond those of the NG modes. It also alters the form of the initial-value problem. For simplicity, only the case of a purely timelike vacuum vector b? = (b, 0, 0, 0) is considered here. In this case, in the weak-?eld limit, it is found that the massive mode does not propagate as a free ?eld. Instead, it remains purely an auxiliary ?eld that has no time dependence. As a result, its value is ?xed by the initial conditions at t = 0. Although it does not propagate, the massive mode can nevertheless alter the form of the static potentials. An example of this can be seen by solving for the modi?ed static potentials in the presence of a point particle with mass m and charge q. It is found that both the electromagnetic and gravitational potentials are modi?ed by the presence of the massive mode, where the speci?c forms of the modi?ed potentials depend on the assumed initial value of the static massive mode. There are therefore numerous cases that could be explored, including examples that might be relevant in considering alternative explanations of dark matter. However, in the large-mass limit (e.g., approaching the Planck scale), excitation of the massive mode is highly suppressed, and the static potentials approach the conventional Coulomb and Newtonian forms. In the limit of a vanishing massive mode, these become exact expressions. As a result, it is found that the usual Einstein-Maxwell solutions (describing both propagating photons and the usual static potentials) can emerge from a bumblebee model (without local U(1) symmetry), in which local Lorentz symmetry is spontaneously broken. Acknowledgments This work was supported by NSF grant PHY-0554663. 6

1. V.A. Kosteleck? and S. Samuel, Phys. Rev. D 40, 1886 (1989); Phys. y Rev. D 39, 683 (1989); Phys. Rev. Lett. 63, 224 (1989). 2. V.A. Kosteleck?, Phys. Rev. D 69, 105009 (2004). y 3. R. Bluhm and V.A. Kosteleck?, Phys. Rev. D 71, 065008 (2005). y 4. R. Bluhm, S.-H. Fung. and V.A. Kosteleck?, arXiv:0712.4119. y 5. H. van Dam and M. Veltman, Nucl. Phys. B 22, 397 (1970); V.I. Zakharov, JEPT Lett. 12, 312 (1970). 6. V.A. Kosteleck? and R. Lehnert, Phys. Rev. D 63, 065008 (2001). y 7. B. Altschul and V.A. Kosteleck?, Phys. Lett. B 628, 106 (2005). y 8. V.A. Kosteleck? and Q.G. Bailey, Phys. Rev. D 74, 045001 (2006). y 9. C. Eling, T. Jacobson, and D. Mattingly, gr-qc/0410001. 10. P. Kraus and E.T. Tomboulis, Phys. Rev. D 66, 045015 (2002). 11. J.W. Mo?at, Intl. J. Mod. Phys. D 12, 1279 (2003). 12. B.M. Gripaios, JHEP 0410, 069 (2004). 13. S.M. Carroll and E.A. Lim, Phys. Rev. D 70, 123525 (2004). 14. O. Bertolami and J. Paramos, Phys. Rev. D 72, 044001 (2005). 15. J.W. Elliott, G.D. Moore, and H. Stoica, JHEP 0508, 066 (2005). 16. J.L. Chkareuli, C.D. Froggatt, and H.B. Nielsen, hep-th/0610186. 17. H.-C. Cheng, M. Luty, S. Mukohyama, and J. Thaler, JHEP 0605, 076 (2006). 18. J.D. Bjorken, Ann. Phys. 24, 174 (1963); Y. Nambu, Prog. Theor. Phys. Suppl. Extra 190 (1968). 19. For a review of the Standard-Model Extension, see R. Bluhm, in Special Relativity: Will It Survive the Next 101 Years? eds., J. Ehlers and C. L¨mmerzahl, (Springer, Berlin, 2006), hep-ph/0506054. a

7

赞助商链接

- Spontaneous Lorentz and Diffeomorphism Violation, Massive Modes, and Gravity
- Spontaneous Nambu-Goldstone Currents Generation Driven by Mismatch
- Baryogenesis from Gravitational Decay of TeV-Particles in Theories with Low Scale Gravity
- Prepotentials of N=2 SU(2) Yang-Mills theories coupled with massive matter multiplets
- Strings on type IIB pp-wave backgrounds with interacting massive theories on the worldsheet
- Nambu-Goldstone Modes in Gravitational Theories with Spontaneous Lorentz Breaking
- Spontaneous Lorentz Violation, Gravity, and Nambu-Goldstone Modes
- Spontaneous Lorentz Violation, Nambu-Goldstone Modes, and Gravity
- Spontaneous Lorentz and Diffeomorphism Violation, Massive Modes, and Gravity
- Spontaneous Breakdown of the Lorentz Invariance in Three-Dimensional Gauge Theories
- Q-stars in scalar-tensor gravitational theories
- Spontaneous Breakdown of the Lorentz Invariance and the Nambu-Goldstone Theorem
- EYM equations in the presence of q-stars is scalar-tensor gravitational theories
- Neutrino Masses and Interactions in a Model with Nambu-Goldstone Bosons
- The Higgs sector of gravitational gauge theories

更多相关文章：
更多相关标签：