Propagating Degrees of Freedom in <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-4.5269pt" id="M1" height="16.7875pt" version="1.1" viewBox="-0.0657574 -12.2606 33.9084 16.7875" width="33.9084pt"><g transform="matrix(.017,0,0,-0.017,0,0)"><path id="g113-103" d="M619 670C619 686 593 712 555 712S459 686 410 634S335 504 320 430H250L219 400L222 388H312L258 73C223 -133 201 -166 187 -180C175 -191 158 -199 140 -199C123 -199 88 -188 74 -172C68 -166 63 -164 54 -171C38 -185 23 -201 23 -215C23 -236 60 -261 93 -261C122 -261 161 -247 207 -200C268 -138 300 -71 337 94C365 220 376 277 394 387L501 399L521 430H401C432 623 464 665 501 665C524 665 544 651 567 627C577 617 583 618 592 625C601 631 619 651 619 670Z"/></g><g transform="matrix(.017,0,0,-0.017,11.025,0)"><path id="g113-41" d="M300 -147C201 -63 143 98 143 270S200 602 300 686L282 710C136 610 70 450 70 271V270C70 89 136 -72 282 -170L300 -147Z"/></g><g transform="matrix(.017,0,0,-0.017,16.962,0)"><path id="g113-83" d="M610 18C585 26 567 34 540 68C517 97 499 128 476 171C452 215 425 276 413 304C496 332 570 394 570 494C570 555 545 595 509 619S419 650 364 650H139L133 622C216 615 219 612 203 527L129 132C112 40 105 36 23 28L17 0H279L285 28C199 34 194 40 211 132L239 284H284C320 284 334 275 351 236C374 182 394 140 420 93C459 23 495 -1 592 -8H600L610 18ZM480 485C480 424 449 372 403 342C374 323 338 316 293 316H245L291 562C296 589 301 601 311 608S337 618 358 618C432 618 480 575 480 485Z"/></g><g transform="matrix(.017,0,0,-0.017,27.721,0)"><path id="g113-42" d="M275 270C275 450 212 609 64 710L45 686C145 604 203 442 203 270S147 -63 45 -147L64 -170C213 -68 275 89 275 270Z"/></g></svg> Gravity

Myung, Yun Soo

doi:https://doi.org/10.1155/2016/3901734

Advances in High Energy Physics

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Research Article | Open Access

Volume 2016 | Article ID 3901734 | https://doi.org/10.1155/2016/3901734

Propagating Degrees of Freedom in Gravity

Yun Soo Myung¹

Academic Editor: George Siopsis

Received22 Sept 2016

Accepted06 Dec 2016

Published21 Dec 2016

Abstract

We have computed the number of polarization modes of gravitational waves propagating in the Minkowski background in gravity. These are three of two from transverse-traceless tensor modes and one from a massive trace mode, which confirms the results found in the literature. There is no massless breathing mode and the massive trace mode corresponds to the Ricci scalar. A newly defined metric tensor in gravity satisfies the transverse-traceless (TT) condition as well as the TT wave equation.

1. Introduction

gravity theory is considered as a representative theory of modified gravities. gravity [1–4] has much attentions as a strong candidate for explaining the current accelerating universe [5, 6]. When choosing the Hu-Sawicki model [7], the theory could give rise to the late time cosmic acceleration without violating the gravity tests in the solar system and without affecting high redshift physics. Very recently, the observational constraints on this model were reported from weal lensing peak abundances [8]. Particularly, gravity [9–11] has shown a strong evidence for inflation to support recent Planck data [12]. An important feature of this model indicates that the inflationary dynamics were driven by the purely gravitational interaction and the scale of inflation is linked to the mass parameter . This theory could thus provide a unified picture of both inflation in the early universe and the accelerated expansion at later times. In addition, black hole [13–15] and traversal wormhole solutions [16, 17] have been found within gravity in recent years. The recent detection of gravitational waves by the LIGO Collaboration [18] is surely a milestone in gravitational waves research and opens new perspectives in the study of Einstein gravity (general relativity) and astrophysics. Hence, it is meaningful to explore gravitational waves in the modified theory of gravity, especially in gravity. The observation of the polarization modes of gravitational waves will be a crucial tool to obtain valuable information about the black holes and the physics of the early universe.

It is well-known that the Einstein gravity with two polarization degrees of freedom (DOF) is distinguished from the metric gravity with three DOF [19]. Importantly, it is worth noting that the Einstein equation derived from gravity contains fourth-order derivative terms. A simple way to avoid a difficulty dealing with the fourth-order equation is to transform gravity into a scalar-tensor theory which is surely a second-order theory.

Very recently, it was reported that a polynomial model could provide two additional scalars of a massive longitudinal mode (perturbed Ricci scalar: ) and a massless transverse mode (breathing mode: ), in addition to the two TT tensor modes () [20]. A breathing mode seems to be overlooked in the literature because of the assumption that the application of the Lorentz gauge implies the TT wave equation. Also, it was insisted that four DOF found in [20] is consistent with the result obtained from the Newman-Penrose (NP) formalism. However, the presence of a breathing mode contradicts the well-known fact in the literature that the gravity involves three DOF of a massive longitudinal mode and two spin-2 modes. Hereafter, we wish to call this the issue of DOF in theories.

In this work, we wish to point out that gravity still involves three DOF by investigating the fourth-order equation composed of a second-order tensor and a fourth-order scalar.

It seems that there is no breathing mode because the perturbed Ricci scalar is related closely to the trace “” of perturbed metric tensor. Hence, the allocation of the Ricci scalar as a newly scalar represents the trace of metric tensor. Also, we wish to remind the reader that the Ricci scalar equation is not an independent equation and is not separated from the perturbed Einstein equation because it comes out just from taking the trace of the latter equation. This implies that the Ricci scalar is an emergent mode from . Furthermore, it is instructive to note that, in the TT gauge, there is a close connection between the metric perturbation and the linearized Riemann tensor, implying that [21]. This gauge is very convenient because it fixes all local gauge freedoms. But it might be unclear that there exists a close relation between the metric perturbation and the NP formalism unless one chooses the TT gauge. One could not naively choose the TT gauge in the perturbed gravity because of , whereas the Lorentz gauge is easily implemented to eliminate the gauge DOF. However, one might choose the TT gauge to obtain a massless spin-2 in the perturbed gravity when one introduces a newly metric perturbation .

The organization of our work is as follows. In Section 2, we briefly describe gravity and its scalar-tensor theory and derive two sets of perturbed equations around the Minkowski background in Section 3. Section 4 is focused on obtaining the number of propagating DOF when one chooses the Lorentz gauge. Finally, we will discuss our result which shows that there is no breathing mode in Section 5.

2. Gravity and Its Scalar-Tensor Theory

Instead of a polynomial model of [20, 22], we start with a specific gravity (Starobinsky model [9])where the -term was originally motivated by one-loop correction to Einstein gravity. Here the mass parameter is chosen to be a positive value, which is consistent with the stability condition of [2]. This model of gravity is enough to find the propagating DOF around the Minkowski background. The Einstein equation takes the formwhere the prime () denotes the differentiation with respect to its argument.

On the other hand, one might represent (1) as a scalar-tensor theory by introducing an auxiliary field [10]:where the superscript means the Jordan frame. Varying with respect to provideswhich means that the Ricci scalar is treated as an independent scalar degree of freedom. Plugging (4) into again leads to the original gravity (1) exactly.

Making use of the conformal transformation and redefining the scalar field ()one arrives at the Starobinsky model in the Einstein frame [11]with the Starobinsky potentialAt this stage, we note that the conformal transformation (5) is a purely classified transformation of coordinates and results in one frame are classically equivalent to the ones obtained in other frame. Hence, it is plausible that the number of DOF in the scalar-tensor theory (6) is three because of two TT tensor modes and one scalar mode. From (6), the Einstein and scalar equations are derived asThe above describes a process of [] briefly.

3. Two Sets of Perturbed Equations

We introduce the metric perturbation around the Minkowski background to find out the propagating DOF:The Taylor expansions around are employed to define the linearized Ricci scalar as [23]with , , and . We note that will be used here instead of in [20]. The perturbed (linearized) equation to (2) is given by the fourth-order coupled equationwhere the linearized Ricci tensor and scalar are given byWhen using (12), the linearized equation (11) becomes a second (fourth)-order differential equation with respect to . Obviously, it is not a tractable equation. Furthermore, its trace equation leads to the linearized Ricci scalar equationIntroducing the linearized Einstein tensor , (11) takes a compact form:We note that the Bianchi identity is satisfied when acting on (14).

On the other hand, two linearized equations of (8) together with take the simple forms with and :We note that (13) and (16) are the same when replacing by , but the fourth-order coupled equation (11) is quite different from the linearized Einstein equation (15). This indicates that (11) can be reduced to two decoupled second-order equations (15) and (16) if one employs the conformal transformation and redefinition of scalar appropriately after choosing (3), leading to a canonical scalar action with the Starobinsky potential in the Einstein frame. In the scalar-tensor theory approach, one assigns the perturbed Ricci scalar to an independent scalar . Instead, it does not have the trace of metric perturbation .

4. Propagating DOF with the Lorentz Gauge

In order to take into account the propagating DOF in gravity, it is convenient to separate the metric tensor into the traceless part and the trace part aswith . This splitting is meaningful because the issue of DOF in theories is related to the presence of .

First of all, let us choose the Lorentz (harmonic) gauge to eliminate the gauge DOF:Here, we note that the transverse condition of cannot be achieved in gravity because of . Then, the linearized Ricci tensor and scalar are given bywhere the last equation indicates that the linearized Ricci scalar exists iff under the Lorentz gauge. This implies that cannot be defined without . That is, if , .

Now, the fourth-order equation (11) leads toThe other form of (20) takes the form

If , its trace equation takes the formwhich is actually the same equation as in (13). Here, (22) impliesbecause could represent a massive (scalar) graviton mode in gravity. The other case of is not allowed since if , one could not derive the trace equation (22) itself. Importantly, this issue should be carefully treated because the massless mode satisfying may correspond to the breathing mode, which is the main subject of this work. In general, it seems that the solution of (22) is given by the sum of the massive mode and massless mode which are independent of each other. However, the massless mode which is a solution to does not exist in gravity. We stress that plays the role of a propagating massive mode instead of . Here is the additional reason to understand why the massless mode (breathing mode) cannot survive in gravity. If one requires , via (19)], (21) reduces to , which is just the tensor equation in Einstein gravity when choosing the Lorentz gauge. It is worth noting that the last fourth-order term of (21) indicates a feature of the perturbed gravity clearly. If one chooses , this term disappears. Therefore, we clarify that the massless scalar mode does not exist.

Acting on (21) leads to (18), which implies that the Lorentz-gauge condition is satisfied in the perturbed equation level. Plugging (22) into (20), we haveSubstituting (22) into (21) implies a fourth-order equationwhich shows clearly that the traceless metric perturbation is closely coupled to the trace of metric perturbation . It is clear that the trace mode cannot be decoupled from the traceless tensor mode . This is the origin of difficulty met when taking into account DOF which had arisen from the gravity. Interestingly, (25) can be transformed to the Ricci tensor-Ricci scalar equationwhich indicates that the traceless Ricci tensor is coupled to the Ricci scalar.

At this stage, we observe that (25) may become a massless propagating tensor equation for aswhich suggests a way of defining a massless spin-2 in gravity. That is, plugging in (27) into (25) leads to . We find from (17) that differs from by . In particular, the splitting of in is nontrivial, which reflects a feature of gravity. This is compared to that of in Einstein gravity. For this purpose, we may express aswhere is the trace-reversed metric perturbation [21]. Here, the Lorentz gauge is given by . We may rewrite (20) in terms of :which is surely the same equation found in [19]. Substituting defined in (29) into that in (30) arrives at which is the same equation as in (27).

Using the trace equation (23) and the Lorentz gauge (18), we may impose the TT condition for :which indicates that is a newly tensor mode defined in gravity. This may imply that gravity accommodates three DOF of two from and one from . We note that if , reduces to and to finally, leading to Einstein gravity.

Considering a gravitational wave that propagates in direction, (27) together with (31) exhibits the fact that gravitational waves have two polarization components. Explicitly, (31) implies where the last two expressions correspond to the TT gauge. is a valid solution to the TT wave equation . The TT gauge condition of implies is constant and, however, this component should be zero to satisfy a condition of the asymptotic flatness: as . The remaining nonzero components of are given by , , , and . Requiring the symmetry and traceless condition leads to the two independent componentsNow, considering (23), one finds the trace solution [24]where is the group velocity of a massive scalar graviton.

Finally, we obtain as the solution to (24) with (28):The other solution as the solution to (30) with (29) takes the formwhich is the same solution found in [19]. This encodes that three DOF of () are found from gravity.

In order to compare (35) and (36) with the Ricci scalar-like solution [20, 24, 25], we write down its solution by replacing with Even though () are similar to (), the last term of solution (37) differs from that of (35).

On the other side of the scalar-tensor theory, (15) together with reduces toAlso, as was shown in (16), the scalar mode is decoupled completely from . Requiring the transverse condition of (Lorentz condition with ) leads to two DOF of , which describe the general relativity. Hence, it is obvious that the scalar-tensor theory has three DOF (one scalar DOF + two tensor DOF).

5. Discussions

First of all, we note that three DOF of () (35) are found from analyzing the perturbed gravity. Here, we did not introduce the Ricci scalar mode () separately because it is closely related to the trace of metric tensor . We have solved the fourth-order coupled equation (24) together with the trace equation (23) directly.

We have found that there is no breathing mode in gravity. The four DOF including breathing mode have been obtained in [20] by assuming that the traceless condition of cannot be imposed on the perturbed gravity, after counting the Ricci scalar mode. The authors in [20] have discovered the breathing mode () from the condition of when the background space-time is not Minkowski. The approach used in [20] was based on the observation that is considered as a different mode from initially [25]. This might lead to overcounting of DOF. However, noting an expression of (19) in the Lorentz gauge implies that is closely connected to .

One might attempt to argue from (22) that the massless mode satisfying may correspond to the breathing mode. In general, it seems that the solution to the fourth-order equation (22) is given by the sum of the massive mode and massless mode which are independent of each other. However, the massless mode which is a solution to does not exist in gravity since [via (19)] means in the Lorentz gauge.

Consequently, we have clarified the issue of DOF in theories. The number of polarization modes of gravitational waves in gravity is still “three” in Minkowski space-time, which is consistent with the results in the literature (especially for [19]). Also, we would like to mention that the DOF counting of theories should be independent of propagating space-time.

Competing Interests

The author declares no competing interests.

Acknowledgments

This work was supported by the 2016 Inje University research grant.

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Copyright

Copyright © 2016 Yun Soo Myung. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP³.

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