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higher spin gauge theory

Contents

Context

Physics

physics, mathematical physics, philosophy of physics

Surveys, textbooks and lecture notes


theory (physics), model (physics)

experiment, measurement, computable physics

String theory

Contents

Idea

Generally by a higher spin field theory is meant a quantum field theory that involves fields of spin >2\gt 2 (recalling that a spinor field has spin 1/2, a gauge field has spin 1, a gravitino field has spin 3/2 and the field of gravity has spin 2).

Folklore had it that all higher spin field theories with mass-less higher spin fields are inconsistent due to negative norm states (“ghost”) appearing in their quantization. (This argument underlies the dominance of 𝒩=1\mathcal{N} = 1 11-dimensional supergravity, see the introduction to the entry 12-dimensional supergravity for more on this).

But then it was discovered that there is a gigher spin gauge theory (Vasiliev 96) which is a kind of higher gauge theory whose field content is an infinite tower of massless fields of ever higher spin.

Ever since the refine folklore says that higher spin theories with a finite number of higher spin field species is inconsistent, but that an infinite tower can fix the problem (…add reference…).

One way that higher spin gauge theories are thought to naturally arise is as the limiting case of string field theory when the string tension is sent to zero (Henneaux-Teitelboim 87, section 2, Gross 88, Sagnotti-Tsulaia 03, Bonelli 03): The excitation spectrum of the string sigma-model contains beyond the massless particles of the effective supergravity theory an infinite tower of massive excitations, of ever higher spin. There are, however, certain limits in which all these masses become negligible to a reference energy scale – the tensionless limit – this is notably so for compactifications on anti de Sitter spaces of small radius. In this limit the string spectrum looks like an infinite collection of massless spinning particles for ever higher spin. Due to their common origin in the string, these share intricate relations among each other, which are argued to be described by higher spin gauge theory. (Notice that at least closed bosonic string field theory is itself already a higher gauge theory, even without sending the string tension to zero, see at closed string field theory – As an ∞-Chern-Simons theory.)

References

General

Original articles include

Reviews and lecture notes include the following:

Further developments include for instance

  • Johan Engquist, Olaf Hohm, Geometry and dynamics of higher-spin frame fields (arXiv:0708.1391)

Relation to string theory

The idea that higher spin gauge theory appears as the limiting case of string field theory where the string tension vanishes goes back to

and is further developed for instance in

And conversely:

Relation to other systems

Relation to Kac-Moody algebras is discussed in

Expression in terms of AKSZ sigma-models is discussed in

  • K.B. Alkalaev, Maxim Grigoriev, E.D. Skvortsov, Uniformizing higher-spin equations (arXiv:1409.6507)

Higher spin Chern-Simons theory

Chern-Simons theory for higher spin fields is discussed in

  • Miles Blencowe, A consistent interacting massless higher-spin field theory in D=2+1D=2+1 Classical and quantum gravity, volume 6 no 4 (1998)

  • E. S. Fradkin, V. Ya. Linetsky, a Superconformal Theory of Massless Higher Spin Fields in D=2+1 (web)

  • Johan Engquist, Olaf Hohm, Higher-spin Chern-Simons theories in odd dimensions (arXiv:0705.3714)

Relation to holography

We list references that discuss the relation of higher spin gauge theory to the AdS/CFT correspondence.

  • Simone Giombi, Xi Yin, Higher Spin Gauge Theory and Holography: The Three-Point Functions (arXiv:0912.3462)

  • Simone Giombi, Xi Yin, Higher Spins in AdS and Twistorial Holography (arXiv:1004.3736)

  • Simone Giombi, TASI Lectures on the Higher Spin - CFT duality (arXiv:1607.02967)

  • Charlotte Sleight, Lectures on Metric-like Methods in Higher Spin Holography (arXiv:1701.08360)

Last revised on September 10, 2018 at 11:03:23. See the history of this page for a list of all contributions to it.