Gravitational instantons and anomalous chiral symmetry breaking
We study anomalous chiral symmetry breaking in two-flavor QCD induced by gravitational and QCD-instantons within asymptotically safe gravity within the functional renormalization group approach. Similarly to QCD-instantons, gravitational ones, associated to a K3-surface connected by a wormhole-like...
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| Main Authors: | , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
14 May 2021
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| In: |
Physical review
Year: 2021, Volume: 103, Issue: 10, Pages: 1-15 |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.103.106016 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1103/PhysRevD.103.106016 Verlag, lizenzpflichtig, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.103.106016 
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| Author Notes: | Yu Hamada, Jan M. Pawlowski, and Masatoshi Yamada |
| Summary: | We study anomalous chiral symmetry breaking in two-flavor QCD induced by gravitational and QCD-instantons within asymptotically safe gravity within the functional renormalization group approach. Similarly to QCD-instantons, gravitational ones, associated to a K3-surface connected by a wormhole-like throat in flat spacetime, generate contributions to the ’t Hooft coupling proportional to exp(−1/gN) with the dimensionless Newton coupling gN. Hence, in the asymptotically safe gravity scenario with a nonvanishing fixed point coupling g∗N, the induced ’t Hooft coupling is finite at the Planck scale, and its size depends on the chosen UV-completion. Within this scenario the gravitational effects on anomalous U(1)A-breaking at the Planck scale may survive at low energy scales. In turn, fermion masses of the order of the Planck scale cannot be present. This constrains the allowed asymptotically safe UV-completion of the gravity-QCD system. We map out the parameter regime that is compatible with the existence of light fermions in the low-energy regime. |
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| Item Description: | Gesehen am 04.08.2021 |
| Physical Description: | Online Resource |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.103.106016 |