Abstract
Two frameworks associated with supersymmetry (SUSY) will be the focus of this chapter, with a view to their further application in probing SQC. These are SUSY breaking (see Sects. 3.1 and 3.2) [1–9] and supersymmetric quantum mechanics (SQM) (see Sect. 3.3) [10–70]. Neither of them has been much investigated in SQC, although the latter feature could be associated with the SQC approach introduced in Chap. 6 of Vol. I.
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Notes
- 1.
\({\boldsymbol{\xi}} ^{(a)}=0\) if \((a)\) does not take values in an Abelian factor of the gauge group.
- 2.
With a minimum of V such that \(\langle f^{\mathsf{I}}\rangle \ne 0\) or \(\langle {\mathsf{d}}^{(a)}\rangle \ne 0\), or in other words, no vacuum with \(\langle f^{{\mathsf{I}}}\rangle =\langle {\mathsf{d}}^{(a)}\rangle =0\), i.e., no solution \(\langle \phi^{{\mathsf{I}}}\rangle \) to these equations.
- 3.
Here, q i are the U(1) charges of \(\phi^{{\mathsf{I}}}\).
- 4.
The SUGRA action depends only on the functions \({\mathsf{G}}(\phi ^{*},\phi )\) and \( {\textrm{f}}_{(a)(b)}(\phi )\), whereas in the global SUSY case we had to define the input of \({\mathsf{K, W,}}\) and f. Hence, coupled to gravity, the kinetic function \({\mathsf{K}},\) and the superpotential \({\mathsf{W}}\) lose their independent meaning and combine to \({\mathsf{G}}(\phi ^{*},\phi)\), which determines the Kähler manifold with \({\mathsf{G}}\) now the Kähler potential (see Sect. 3.5 of Vol. I).
- 5.
Hence, in SUGRA theories, one can find a mechanism to tune the cosmological constant to any chosen value: SUSY breaks if one or more auxiliary fields are non-zero at the vacuum. At the vacuum with unbroken SUSY, we have a cosmological constant given by
$$\varLambda \sim -\frac{3}{{{\relax\ifmmode\mathsf{k}\else\textsf{k}\fi}} ^{4}}\left\langle {\mathrm{e}}^{{\mathsf{G}}}\right\rangle\;,$$hence determining a Minkowski or anti-de Sitter space. Phenomenology requires SUSY to be broken, and also a small cosmological constant. These are non-trivial conditions on \(\mathsf{G}\).
- 6.
Recall that this is another superspace, not that of the full function space [i.e., superspace (see Chap. 2)] of all 3-metrics on a spacelike 3-surface embedded in spacetime.
- 7.
Here we introduce the notation as given in [81, 82, 83, 84, 85], which is different from the usual notation of SUSY field theory in 2-spinor form. This choice is inherited from a 4-spinor notation (see Note A.6 in Appendix A), and is widely followed in most of the literature referring to the context in Chap. 8.
- 8.
The Lagrangian can be obtained by dimensional reduction of the N = 1 sigma model in 1 + 1 dimensions.
- 9.
We define the fermion Fock vacuum by \(| 0 \rangle\) and the completely filled fermion state by \(| \varPsi_n \rangle \), where
$$\chi^x|0\rangle = 0\;, \qquad\bar\chi^x|\varPsi_n\rangle = 0 \mbox{for all}\;\, x\;,$$((3.80))the former being trivially annihilated by \(\mathcal{S}\) and the latter by \(\bar {\mathcal{S}}\). Note also that [see (3.79) above]
$$\begin{array}{*{20}l} |\varPsi_n\rangle &=& \frac{1}{n!}\epsilon_{x_1\ldots x_n} \bar{\chi}^{x_1}\ldots\bar{\chi}^{x_n}|0\rangle \\ &=& \frac{1}{n!}\sqrt{|\det({\mathcal{G}}_{XY})|} \epsilon_{X_1\ldots X_n}\bar{\chi}^{X_1} \ldots\bar{\chi}^{X_n}|0\rangle\;.\end{array}$$((3.81)) - 10.
Boundaries (e.g., 3-manifolds) are important when dealing with quantum amplitudes, and so cannot be neglected in off-shell situations (see Note 2.3 in Vol. I).
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Moniz, P.V. (2010). Additional SUSY and SUGRA Issues . In: Quantum Cosmology - The Supersymmetric Perspective - Vol. 2. Lecture Notes in Physics, vol 804. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-11570-7_3
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