International Centre for Theoretical Physics

" TC/82/T5

INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS

ULTRAVIOLET FIIJITENESS OF N = 8 SUPERGRA.VITY

SPONTANEOUSLY BROKEN BY DIMENSIONAL REDUCTION

E. Sezgin INTERNATIONAL and ATOMIC ENERGY AGENCY P. van Nieuwenhuizen

UNITED NATIONS EDUCATIONAL, SCIENTIFIC AND CULTURAL ORGANIZATION 1982MIRAMARE-TRIESTE

The reuormalisability aspects of extended and simple supergravity IC/62/75 models have so far only been studied in massless models where the one- and two-loop corrections to the S-matrix are finite when no matter Is present, tut

International Atomic Energy Agency where non-fenormalizaibility sets in as soon as matter is added [l]. Using and superspace methods , arguments have been given that N = 8 supergravity is nations Educational Sciei:; ;ic and Cultural. Organization even, finite to six loops [2]. In this letter we consider the finiteness properties of N = 8 supergravity with masses obtained from dimensional TKTEPJNA'IIOHAL CENTRE FOR THEORETICAL PHYSICS reduction. Our main result is that the one-loop divergences cancel, even when all gravitini acquire masses [3].

The model we consider in d = h dimensions is obtained from the N = 8,d = 5 model by generalized dimensional reduction [h]. In d = 5, the action has a global E{6) and a local Usp(8) invariance [5]. The Usp(8) gauge ULTRAVIOLET FIHITEBESS OF H = 8 SUBERGRAVITY, fields are composites of scalar fields which parametrize the E(6) algebra. m SPONTANEOUSLY BBOKEH BY DIMENSIONAL REDUCTION • All fields in d = 5 are massless and consist of: one funfbein e , eight u a A gravitini i|> in the fundamental representation of Usp(8), 2T vectors A™B in the fundamental representation of E(6) and 48 spin — fields xa ° • The E. Sezgin scalar fields are written according to the theory of non-linear representation; International Centre for Theoretical Physics, Trieste, Italy,

and ab Cd ,cdef ^H - (exp 8 (1) P. van Sieuwenhuizen Institute for Theoretical Physics, State Univ. of Hew York at Stony Brook, Stony Brook, N.Y.^USA. where the 36 8 parametrize the Usp(B) subgroup of E(6), while the 1*2 scal&rs ific e are physical and parametrize the coset E(6)/Usp(8). The X and if are totally antisymmetric and symplectic traceless and ABSTRACT ( ) !K , . Usp(8) indices denoted by latin letters, run from one to The one-loop corrections to scalar-scalar scattering in II = 8 eight and are raised and lowered by the Usp(8) metric For further •ab" supergravity with h masses from dimensional reduction, are finite. We details we refer the reader to Hef.3.

discuss various mechanisms that cancel the cosmological constant and The generalized dimensional reduction is carried out by assuming infra-red divergences due to finite tut non-vanishing tadpoles. that all fields are independent of the fifth co-ordinate x , except the , , . C10 , «.^ab photons A and scalarn s V which are assumed to be of the form M dp

MRAMARE - TRIESTE (exp June 1982 (2)

and idem Yag - We shall later take the matrix M as the most general • To be submitted for publication. element in the Cartan subalgebra of E{6), but in order to exclude a cosmological constant, we begin by requiring that M lies in the maximal

-2- compact subgroup of E(6) which is Usp(8). Hence

0 m- - 2

-m, 0 (3) In d = 5 this is a pure Lorentz gauge but in i - h it provides masses for the 2k would-be Goldstone "bosons and it leads to massive ghosts which do not, however, contribute in our calculations. Substituting (2) into the action "breaks all supersymmetries, but the theory We compute the one-loop divergences of graviscalar-graviscalar cannot a priori "be called spontaneously "broken, because there is nothing • • :.3tie scattering. We have chosen this process since it requires the spontaneous about (2): we. postulate: the factorization ansatz in (2). It is smallest nusuber 01 graphs (see however Figs.1,2,3)- Since the massless the aim of this letter to shov that the "broken theory has the same ultraviolet >Tiodel is finite, we only calculate mass-dependent corrections. Although in properties as the unbroken theory and in this sense it deserves the name any (broken or unbroken) theory graviton-graviton scattering is finite, on- spontaneously "broken. shell at one-loop,it woula be presumably even haj-der (if possible at all) After dimensional reduction, from d = 5 to d = li [3], the fiinfbein to prove finiteness of other amplitudes by using symmetry arguments which yields the vierbein and a graviphoton B and the graviscalar , all massless. connect this S-matrix element to other S-matrix elements, "because the (global) The graviphoton has a Pauli coupling when M = O, "but when M 4 0, it has symmetry is broken. We only compute ultraviolet divergences. There are minimal charge couplings as well,and this is a serious problem for fatal infra-red divergences due to the fact that tadpoles with a massive loop phenomenological applications 16]. The eight gravitini eat the eight and a massless external line, though finite, are actually non-vanishing [33- would-be Goldstone spin — fields jir ajid all "become massive with masses This may be due to our expanding^fields about zero. Since the minimum of the Of the 27 photons A only three remain masslests (namely ± m. (i = 1,4J potential is a valley, we could have expanded about other classical values, 3 56 aS A^A \A note that A £1=0) while the remaining 2k get masses and it is conceivable that this freedom could "be used to make the quantum split into (±m. ±m ) , where i < j. The corresponding 27 scalars A vacuum expectation value of all fields vanishing, hence cancelling the tad- 1 12 ) and three massless "bosons which do not get eaten (namely $ > poles. The potential is positive and vanishing at its minimum. A closed 2U would-be Goldstone bosons which get eaten by the corresponding A . /ill result is [3] I48 spin — fields become massive (16 with masses [m. | and 32 with |m. ± m. ± TIL] where i < j < k). Finally, the t's yield 1*0 massive scalars (2l* with masses |m. ± m [ and 16 with |m. 1 m ± HL * m \ where i < j < k < '- ) and v =jre i,. 1 1 " , 123H 1256, two massless bosons which do not get eaten (namely 41 and ). (5) The model is quantized as follows. The spacetime symmetries and the 2 U(l} of the graviphoton are fixed by the usual de Donder and Lorentz gauges. where a is given "by The eight local supersymmetries are fixed in the unitary gauge iji = 0, as

a is the local Usp(8) by the unitary gauge 6 = 0. This introduces m. , 2>abcd _ h_ [abc d] {Z 1 and mT terms in the gravitino propagator. There are still 27 local U(l)'s Vb'c'd ~ 3 *e[a'b'c' (6) associated with A , despite the fact that some have acquired masses, anc we fix these by an 't Hooft gauge fixing term which diagonalizes their kinetic terms

-h- -3- Some unexplained regularities gccux in the spin-one loops. In all Since the M

The calculation is full of details, but these cannot be recorded Let us now take the matrix M in (2) as the most general element here, Hon-local divergences of the form (mass)U times t2 / s2 cancel in the Cartan subalgebra of E(6) rather than Usp{8). This yields two more where s,t and u denote Mandelstam variables. As in other one-loop parameters with the dimension of a mass. The extra two E(6) generators calculations, we expect that all terms with poles in s,t,u should cancel, which coHmute with (3) and each other have the following non-zero entries and ve checked this in a number of cases. There are also divergences proportional to powers of m~ , due to the gravitino propagator but these are gauge artefacts and should cancel. The crucial divergences we are concerned with are of the form (mass) time3 a constant. The contributions from spin 0, j , 1 are given in Figs.1,2,3- All divergences are (10) multiples of 1231* They correspond to 41 and if1256, which is not surprising if one realizes that the M+ term in (5) is really the commutator of M with all (M .1256 a (7) consequently, the two previously massless bosons $*"-'"',123U and ^'~'"J parametrize N. One still has f°t 8ft^-f • (PA + QA).^Cd where hats denote five- dimensional indices,but now P' in (5) is given by the following closed where X = 1.2.3,1* for spin \, 1, -r, 0 and I is the antisymmetric, 2 2 [EL./2] [a./ expression: symplectic traceless unit tensor and M a = (-) a, ,2-, +-••(-) T. Z 1 k cd cd ^a'b'c'd1 , vabcd p H (oo3hl) ab 5 ab " a'b'c'd' [a,/2] . For example the first graph in Fig.l gives 72 tijses MQ divided (11) ~ey 6 = Su (k-n). We use dimensional regularization, but for the one-loop divergences all methods give the same answer. From (5) it follows that there is now a negative cosmological constant Adding all results one obtains at the point where all fields $ vanish (although we are not sure that this yields the true minimum of the potential; however the potential is always 3{div) = | (723) I i-)2J (2-J+l) non-negative) which would yield & de-Sitter universe. It has opposite sign (8) from the cosaological constant one gets from the gauging of supergravitles. The introduction of H produces in many places new terms. The potential, Hote that the number 723 ia found in all spin 0, ~ and 1 sectors separately. if never vanishing, no longer attains its minimum due to the exponential Since this is sufficient evidence for the ultraviolet finiteness, we left with ^>,but shifting

one can choose a unitary gauge in which the eight Xgj, H (-)2lJ (2J+1) M2* • 0 for k = 0,1,2,3 (9)

*) for k = 2, we see that all divergences cancel. One might cancel both ty generalized dimensional reduction of the gauged d > !t,N = 8 model if it exists. -5- -6- vanish, instead of the eight i|)^ • The three massless vectors A , A and REFERENCES 56 5 e 2 y ' U A acquire masslike terms due to the Maxwell terms (F ) . This suggests 12 3l* 56 that the three massless "bosons ij> , cji and can he eaten. Indeed [l] J.A.M. Vermaseren and P. van Wieuwenhuizen, Phys. Letters 65B, 263 (1976}; this is the case. In $A™ under the 27 local U(l) one finds in 8*A the M.T. Grisaru, P. van Mieuwenhuizen and J.A.M. Vermaseren, Phys. Eev. Q/\ + PA since the A° are of the form (2). Hence, there are now terms Letters 3j_, 1662 (1976); md a11 *as ean ^ gauged M.T. Grisaru, Phys. Letters B6£, 75 (1977); All these results are very similar to a. supersymmetry breaking caused J.A.M. Vermaseren and P. van Hieuwechuizen, Phys. Rev. Dl6. 298 (1977); by adding to the H - 8 model when reduced from a = 11, a total divergence M. Fischler, Phys. Rev. D20, 396 (19T9). F [T], Our symmetry "breaking with M = 0, U # 0 seems to he a [2] M.T. Grisaru and li. Siegel, "Supergraphity (II). Manifestly eovariant two-parameter extension of that one parameter result. rules and higher-loop finiteness", Caltech preprint CALT-68-892 Although the classical spontaneously broken N = 8 model with S = 0 (January 1982). did not have a cosmological constant, a finite non-vanishing value was [3] E. Sezgin and P, van Nieuwenhuizen, Nucl. Phys. B19_5_, 325 (1982). produced "by radiative corrections [It,3]. Correspondingly, the graviton tad- poles, though being finite, were non-zero, and cause infra-red problems. [h] J. Scherk. and J.H. Schvarz, Mucl. Phys. B153, 6l (1976).

Similar results hold for the graviscalar tadpoles. These tadpoles might [5] E. Cremmer, J. Scherk and J.H. Schvarz, Phys. Letters 8UB, 83 (1979). destroy ultraviolet finiteness from the two-loop level onwards. The [6] J. Scherk, "From supergravity to antigravity" in Superp:ra?ity. introduction of the matrices H might prevent these disasters in the following Eds. P. van Ifieuwenhuizen and D.Z. Freedman (North Holland Publishing way. One could take M and H as infinite power series in fi and N to Co., Amsterdam 1979), p.'O. start with fi. Fixing nu and my- at order fi could make the one-loop tadpoles strictly zero, without introducing a cosmological constant. For [7l A. Aurilia, K. Hicolai and P.K. Townsend, Hucl. Phys. B176_, 509 (198O). the higher order loops one would have to fine-tune nij- and m^-, "but whether this scheme would be sufficient to cure infra-red problems at all higher loops requires extensive investigation.

ACKHOWLEDGMEHT

It is a pleasure to acknowledge useful discussions with J.H. Schwarz. This work is partially .supported by the National Science Foundation grant no. PHY-O6376AO1 (State University of Hew York at Stony Brook) and partly by National Science Foundation grant no. PHY-22^89 (University of Texas at Austin). One of the authors (E.S.) would like to thank Professor Ahdus Salam, the International Atomic Energy Agency and UNESCO for hospitality at the International Centre for Theoretical Physics, Trieste.

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