The continual production of long wavelength gravitons during primordial inflation endows graviton loop corrections with secular growth factors. During a prolonged period of inflation these factors eventually overwhelm the small loop-counting parameter of $G H^2$, causing perturbation theory to break down. A technique was recently developed for summing the leading secular effects at each order in non-linear sigma models, which possess the same kind of derivative interactions as gravity. This technique combines a variant of Starobinsky's stochastic formalism with a variant of the renormalization group. We generalize the new technique to quantum gravity, resulting in a Langevin equation in which secular changes in gravitational phenomena are driven by stochastic fluctuations of the graviton field.
{"title":"Leading Logarithm Quantum Gravity","authors":"S. P. Miao, N. C. Tsamis, R. P. Woodard","doi":"arxiv-2409.12003","DOIUrl":"https://doi.org/arxiv-2409.12003","url":null,"abstract":"The continual production of long wavelength gravitons during primordial\u0000inflation endows graviton loop corrections with secular growth factors. During\u0000a prolonged period of inflation these factors eventually overwhelm the small\u0000loop-counting parameter of $G H^2$, causing perturbation theory to break down.\u0000A technique was recently developed for summing the leading secular effects at\u0000each order in non-linear sigma models, which possess the same kind of\u0000derivative interactions as gravity. This technique combines a variant of\u0000Starobinsky's stochastic formalism with a variant of the renormalization group.\u0000We generalize the new technique to quantum gravity, resulting in a Langevin\u0000equation in which secular changes in gravitational phenomena are driven by\u0000stochastic fluctuations of the graviton field.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251642","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In recent literature on holographic QCD, the consideration of the five-dimensional Einstein-dilaton-Maxwell models has played a crucial role. Typically, one Maxwell field is associated with the chemical potential, while additional Maxwell fields are used to describe the anisotropy of the model. A more general scenario involves up to four Maxwell fields. The second field represents spatial longitudinal-transverse anisotropy, while the third and fourth fields describe anisotropy induced by an external magnetic field. We consider an ansatz for the metric characterized by four functions at zero temperature and five functions at non-zero temperature. Maxwell field related to the chemical potential is treated with the electric ansatz, as is customary, whereas the remaining three Maxwell fields are treated with a magnetic ansatz. We demonstrate that for the fully anisotropic diagonal metric only six out of the seven equations are independent. One of the matter equations -- either the dilaton or the vector potential equation -- follows from the Einstein equations and the remaining matter equation. This redundancy arises due to the Bianchi identity for the Einstein tensor and the specific form of the stress-energy tensor in the model. A procedure for solving this system of six equations is provided. This method generalizes previously studied cases involving up to three Maxwell fields. In the solution with three magnetic fields our analysis shows, that the dilaton equation is a consequence of the five Einstein equations and the equation for the vector potential
{"title":"Einstein-dilaton-four-Maxwell Holographic Anisotropic Models","authors":"Irina Ya. Aref'eva, Kristina Rannu, Pavel Slepov","doi":"arxiv-2409.12131","DOIUrl":"https://doi.org/arxiv-2409.12131","url":null,"abstract":"In recent literature on holographic QCD, the consideration of the\u0000five-dimensional Einstein-dilaton-Maxwell models has played a crucial role.\u0000Typically, one Maxwell field is associated with the chemical potential, while\u0000additional Maxwell fields are used to describe the anisotropy of the model. A\u0000more general scenario involves up to four Maxwell fields. The second field\u0000represents spatial longitudinal-transverse anisotropy, while the third and\u0000fourth fields describe anisotropy induced by an external magnetic field. We\u0000consider an ansatz for the metric characterized by four functions at zero\u0000temperature and five functions at non-zero temperature. Maxwell field related\u0000to the chemical potential is treated with the electric ansatz, as is customary,\u0000whereas the remaining three Maxwell fields are treated with a magnetic ansatz.\u0000We demonstrate that for the fully anisotropic diagonal metric only six out of\u0000the seven equations are independent. One of the matter equations -- either the\u0000dilaton or the vector potential equation -- follows from the Einstein equations\u0000and the remaining matter equation. This redundancy arises due to the Bianchi\u0000identity for the Einstein tensor and the specific form of the stress-energy\u0000tensor in the model. A procedure for solving this system of six equations is\u0000provided. This method generalizes previously studied cases involving up to\u0000three Maxwell fields. In the solution with three magnetic fields our analysis\u0000shows, that the dilaton equation is a consequence of the five Einstein\u0000equations and the equation for the vector potential","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251472","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Yu-Qi Dong, Xiao-Bin Lai, Yu-Qiang Liu, Yu-Xiao Liu
The Isaacson picture provides a general method for describing the effects of gravitational waves, established on two sets of basic equations. The first set of equations describes the propagation of gravitational waves within a given background, while the second set elucidates the interaction between the effective energy-momentum tensor of gravitational waves and the background metric. These two sets of equations are typically derived by expanding the field equations to second-order perturbations. In addition to the method of perturbing field equations, there is an alternative method: obtaining the two sets of basic equations by expanding the action to the second-order of perturbations. In this paper, we elaborate on this method, establishing its foundations more rigorously. Especially, the second-order perturbation action, with the Minkowski metric as the background, contains all necessary information to construct the Isaacson picture far from the source. We outline the derivation of the two sets of basic equations to describe the gravitational wave effects in the Isaacson picture, based on the second-order perturbation action. This will enable us to analyze the following effects: polarizations of gravitational waves, the wave speed for each polarization mode, the effective energy-momentum tensor of gravitational waves, and the nonlinear memory effect of gravitational waves. We illustrate this method by applying it to the most general second-order vector-tensor theory including parity-breaking terms. We further analyze the polarization modes of gravitational waves in this theory. We highlight that this method facilitates model-independent research on various gravitational wave effects in general modified gravity theories. These effects are anticipated to be identified by the upcoming generation of gravitational wave detectors, aimed at testing potential modifications to gravity theory.
{"title":"Analyzing gravitational wave effects in general modified gravity: an example based on the most general vector-tensor theory","authors":"Yu-Qi Dong, Xiao-Bin Lai, Yu-Qiang Liu, Yu-Xiao Liu","doi":"arxiv-2409.11838","DOIUrl":"https://doi.org/arxiv-2409.11838","url":null,"abstract":"The Isaacson picture provides a general method for describing the effects of\u0000gravitational waves, established on two sets of basic equations. The first set\u0000of equations describes the propagation of gravitational waves within a given\u0000background, while the second set elucidates the interaction between the\u0000effective energy-momentum tensor of gravitational waves and the background\u0000metric. These two sets of equations are typically derived by expanding the\u0000field equations to second-order perturbations. In addition to the method of\u0000perturbing field equations, there is an alternative method: obtaining the two\u0000sets of basic equations by expanding the action to the second-order of\u0000perturbations. In this paper, we elaborate on this method, establishing its\u0000foundations more rigorously. Especially, the second-order perturbation action,\u0000with the Minkowski metric as the background, contains all necessary information\u0000to construct the Isaacson picture far from the source. We outline the\u0000derivation of the two sets of basic equations to describe the gravitational\u0000wave effects in the Isaacson picture, based on the second-order perturbation\u0000action. This will enable us to analyze the following effects: polarizations of\u0000gravitational waves, the wave speed for each polarization mode, the effective\u0000energy-momentum tensor of gravitational waves, and the nonlinear memory effect\u0000of gravitational waves. We illustrate this method by applying it to the most\u0000general second-order vector-tensor theory including parity-breaking terms. We\u0000further analyze the polarization modes of gravitational waves in this theory.\u0000We highlight that this method facilitates model-independent research on various\u0000gravitational wave effects in general modified gravity theories. These effects\u0000are anticipated to be identified by the upcoming generation of gravitational\u0000wave detectors, aimed at testing potential modifications to gravity theory.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"196 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251478","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Riccardo Argurio, Andrés Collinucci, Giovanni Galati, Ondrej Hulik, Elise Paznokas
We extend the construction of the T-duality symmetry for the 2d compact boson to arbitrary values of the radius by including topological manipulations such as gauging continuous symmetries with flat connections. We show that the entire circle branch of the $c=1$ conformal manifold can be generated using these manipulations, resulting in a non-invertible T-duality symmetry when the gauging sends the radius to its inverse value. Using the recently proposed symmetry TFT describing continuous global symmetries of the boundary theory, we identify the topological operator corresponding to these new T-duality symmetries as an open condensation defect of the bulk theory, constructed by (higher) gauging an $mathbb{R}$ subgroup of the bulk global symmetries. Notably, when the boundary theory is the compact boson with a rational square radius, this operator reduces to the familiar T-duality defect described by a Tambara-Yamagami fusion category. This construction thus naturally includes all possible discrete T-duality symmetries of the theory in a unified way.
我们将二维紧凑玻色T对偶对称性的构造扩展到任意半径值，包括拓扑操作，如用平面连接测量连续对称性。我们证明，利用这些操作可以生成$c=1$共形流形的整个圆分支，当测量将半径发送到它的逆值时，就会产生不可逆转的T对偶对称性。利用最近提出的描述边界理论连续全局对称性的对称性TFT，我们把对应于这些新的T对偶对称性的拓扑算子识别为体量理论的开放凝聚缺陷，它是通过对体量全局对称性的一个$mathbb{R}$子群进行（高）测量而构造的。值得注意的是，当边界理论是具有有理平方半径的紧凑玻色子时，这个算子就还原为我们熟悉的由坦巴拉-山神融合范畴描述的T对偶缺陷。因此，这种构造自然而然地以统一的方式包含了理论中所有可能的离散 T 对偶对称性。
{"title":"Non-Invertible T-duality at Any Radius via Non-Compact SymTFT","authors":"Riccardo Argurio, Andrés Collinucci, Giovanni Galati, Ondrej Hulik, Elise Paznokas","doi":"arxiv-2409.11822","DOIUrl":"https://doi.org/arxiv-2409.11822","url":null,"abstract":"We extend the construction of the T-duality symmetry for the 2d compact boson\u0000to arbitrary values of the radius by including topological manipulations such\u0000as gauging continuous symmetries with flat connections. We show that the entire\u0000circle branch of the $c=1$ conformal manifold can be generated using these\u0000manipulations, resulting in a non-invertible T-duality symmetry when the\u0000gauging sends the radius to its inverse value. Using the recently proposed\u0000symmetry TFT describing continuous global symmetries of the boundary theory, we\u0000identify the topological operator corresponding to these new T-duality\u0000symmetries as an open condensation defect of the bulk theory, constructed by\u0000(higher) gauging an $mathbb{R}$ subgroup of the bulk global symmetries.\u0000Notably, when the boundary theory is the compact boson with a rational square\u0000radius, this operator reduces to the familiar T-duality defect described by a\u0000Tambara-Yamagami fusion category. This construction thus naturally includes all\u0000possible discrete T-duality symmetries of the theory in a unified way.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"51 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251474","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we extend our previous work [D. Wu, Phys. Rev. D 108, 084041 (2023)] to more general cases by including a rotation parameter. We investigate the topological numbers for the rotating, accelerating neutral black hole and its AdS extension, as well as the rotating, accelerating charged black hole and its AdS extension. We find that the topological number of an asymptotically flat accelerating black hole consistently differs by one from that of its non-accelerating counterpart. Furthermore, we show that for an asymptotically AdS accelerating black hole, the topological number is reduced by one compared to its non-accelerating AdS counterpart. In addition, we demonstrate that within the framework of general relativity, the acceleration parameter and the negative cosmological constant each independently add one to the topological number. However, when both factors are present, their effects neutralize each other, resulting in no overall change to the topological number.
{"title":"Thermodynamic topological classes of the rotating, accelerating black holes","authors":"Wentao Liu, Li Zhang, Di Wu, Jieci Wang","doi":"arxiv-2409.11666","DOIUrl":"https://doi.org/arxiv-2409.11666","url":null,"abstract":"In this paper, we extend our previous work [D. Wu, Phys. Rev. D 108, 084041\u0000(2023)] to more general cases by including a rotation parameter. We investigate\u0000the topological numbers for the rotating, accelerating neutral black hole and\u0000its AdS extension, as well as the rotating, accelerating charged black hole and\u0000its AdS extension. We find that the topological number of an asymptotically\u0000flat accelerating black hole consistently differs by one from that of its\u0000non-accelerating counterpart. Furthermore, we show that for an asymptotically\u0000AdS accelerating black hole, the topological number is reduced by one compared\u0000to its non-accelerating AdS counterpart. In addition, we demonstrate that\u0000within the framework of general relativity, the acceleration parameter and the\u0000negative cosmological constant each independently add one to the topological\u0000number. However, when both factors are present, their effects neutralize each\u0000other, resulting in no overall change to the topological number.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251566","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we proposed a worldsheet construction of a subset of triple product amplitudes proposed by Huang and Remmen. We start with closed bosonic strings but left and right-moving momenta are not necessarily equal. Instead, they satisfy certain conditions. We called them section conditions. These conditions are generalizations of the section condition in double field theory. The vertex operators of chiral strings have nontrivial monodromy, so we interpret them as attached to the end of defects. In the calculation of the amplitude, we not only have to integrate over the moduli space, we also have to sum over different defect configurations. Unitarity and other consistency conditions for chiral string amplitudes are checked. We found the graviton amplitude, the Virasoro amplitude, and also a special kind of amplitude that has one infinite spin tower. Similar kinds of amplitude have appeared in bootstrap literature. The more general $N$-point amplitude could be obtained from a modified KLT relation. The five-point chiral string amplitude is also explicitly calculated.
{"title":"Triple Product Amplitude from Chiral String","authors":"Yu-Ping Wang","doi":"arxiv-2409.11732","DOIUrl":"https://doi.org/arxiv-2409.11732","url":null,"abstract":"In this paper, we proposed a worldsheet construction of a subset of triple\u0000product amplitudes proposed by Huang and Remmen. We start with closed bosonic\u0000strings but left and right-moving momenta are not necessarily equal. Instead,\u0000they satisfy certain conditions. We called them section conditions. These\u0000conditions are generalizations of the section condition in double field theory.\u0000The vertex operators of chiral strings have nontrivial monodromy, so we\u0000interpret them as attached to the end of defects. In the calculation of the\u0000amplitude, we not only have to integrate over the moduli space, we also have to\u0000sum over different defect configurations. Unitarity and other consistency\u0000conditions for chiral string amplitudes are checked. We found the graviton\u0000amplitude, the Virasoro amplitude, and also a special kind of amplitude that\u0000has one infinite spin tower. Similar kinds of amplitude have appeared in\u0000bootstrap literature. The more general $N$-point amplitude could be obtained\u0000from a modified KLT relation. The five-point chiral string amplitude is also\u0000explicitly calculated.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251475","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we study gravitational symmetry algebras that live on 2-dimensional cuts $S$ of asymptotic infinity. We define a notion of wedge algebra $mathcal{W}(S)$ which depends on the topology of $S$. For the cylinder $S=mathbb{C}^*$ we recover the celebrated $Lw_{1+infty}$ algebra. For the 2-sphere $S^2$, the wedge algebra reduces to a central extension of the anti-self-dual projection of the Poincar'e algebra. We then extend $mathcal{W}(S)$ outside of the wedge space and build a new Lie algebra $mathcal{W}_sigma(S)$, which can be viewed as a deformation of the wedge algebra by a spin two field $sigma$ playing the role of the shear at a cut of $mathscr{I}$. This algebra represents the gravitational symmetry algebra in the presence of a non trivial shear and is characterized by a covariantized version of the wedge condition. Finally, we construct a dressing map that provides a Lie algebra isomorphism between the covariant and regular wedge algebras.
{"title":"Asymptotic Higher Spin Symmetries I: Covariant Wedge Algebra in Gravity","authors":"Nicolas Cresto, Laurent Freidel","doi":"arxiv-2409.12178","DOIUrl":"https://doi.org/arxiv-2409.12178","url":null,"abstract":"In this paper, we study gravitational symmetry algebras that live on\u00002-dimensional cuts $S$ of asymptotic infinity. We define a notion of wedge\u0000algebra $mathcal{W}(S)$ which depends on the topology of $S$. For the cylinder\u0000$S=mathbb{C}^*$ we recover the celebrated $Lw_{1+infty}$ algebra. For the\u00002-sphere $S^2$, the wedge algebra reduces to a central extension of the\u0000anti-self-dual projection of the Poincar'e algebra. We then extend\u0000$mathcal{W}(S)$ outside of the wedge space and build a new Lie algebra\u0000$mathcal{W}_sigma(S)$, which can be viewed as a deformation of the wedge\u0000algebra by a spin two field $sigma$ playing the role of the shear at a cut of\u0000$mathscr{I}$. This algebra represents the gravitational symmetry algebra in\u0000the presence of a non trivial shear and is characterized by a covariantized\u0000version of the wedge condition. Finally, we construct a dressing map that\u0000provides a Lie algebra isomorphism between the covariant and regular wedge\u0000algebras.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"100 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251470","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We extend the usual vacuum Metric-Affine $f(R)$ Gravity by supplementing it with all parity even quadratic invariants in torsion and non-metricity. As we show explicitly this supplementation drastically changes the status of the Theory which now propagates an additional scalar degree of freedom on top of the graviton. This scalar degree of freedom has a geometric origin as it relates to spacetime torsion and non-metricity. The resulting Theory can be written equivalently as a metric and torsionless Scalar-Tensor Theory whose potential and kinetic term coupling depend on the choice of the function $f(R)$ and the dimensionless parameters of the quadratic invariants respectively.
{"title":"Extended Metric-Affine $f(R)$ Gravity with Dynamical Connection in Vacuum","authors":"Damianos Iosifidis","doi":"arxiv-2409.11771","DOIUrl":"https://doi.org/arxiv-2409.11771","url":null,"abstract":"We extend the usual vacuum Metric-Affine $f(R)$ Gravity by supplementing it\u0000with all parity even quadratic invariants in torsion and non-metricity. As we\u0000show explicitly this supplementation drastically changes the status of the\u0000Theory which now propagates an additional scalar degree of freedom on top of\u0000the graviton. This scalar degree of freedom has a geometric origin as it\u0000relates to spacetime torsion and non-metricity. The resulting Theory can be\u0000written equivalently as a metric and torsionless Scalar-Tensor Theory whose\u0000potential and kinetic term coupling depend on the choice of the function $f(R)$\u0000and the dimensionless parameters of the quadratic invariants respectively.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251644","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We provide the complete four loop perturbative renormalization of a low temperature statistical mechanics model of flat polymerized membranes. Within a non-local effective flexural theory based on transverse elastic fluctuations, we determine analytically, at the four existing fixed points, the anomalous elasticity critical exponent $eta$ which controls all scaling behaviors in the theory. Results are obtained as apparently convergent series, enabling precise estimates without resummations. We independently confirm and complement the results of recent four-loop work [Pikelner 2022 EPL 138 17002] carried out in a different model. We also find good agreement with non-perturbative approaches and experiments on soft materials and graphene.
{"title":"Four loop elasticity renormalization of low temperature flat polymerized membranes","authors":"S. Metayer","doi":"arxiv-2409.11773","DOIUrl":"https://doi.org/arxiv-2409.11773","url":null,"abstract":"We provide the complete four loop perturbative renormalization of a low\u0000temperature statistical mechanics model of flat polymerized membranes. Within a\u0000non-local effective flexural theory based on transverse elastic fluctuations,\u0000we determine analytically, at the four existing fixed points, the anomalous\u0000elasticity critical exponent $eta$ which controls all scaling behaviors in the\u0000theory. Results are obtained as apparently convergent series, enabling precise\u0000estimates without resummations. We independently confirm and complement the\u0000results of recent four-loop work [Pikelner 2022 EPL 138 17002] carried out in a\u0000different model. We also find good agreement with non-perturbative approaches\u0000and experiments on soft materials and graphene.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251479","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Spectral distortions of the cosmic microwave background (CMB) provide stringent constraints on energy and entropy production in the post-BBN (Big Bang Nucleosynthesis) era. This has been used to constrain dark photon models with COBE/FIRAS and forecast the potential gains with future CMB spectrometers. Here, we revisit these constraints by carefully considering the photon to dark photon conversion process and evolution of the distortion signal. Previous works only included the effect of CMB energy density changes but neglected the change to the photon number density. We clearly define the dark photon distortion signal and show that in contrast to previous analytic estimates the distortion has an opposite sign and a $simeq 1.5$ times larger amplitude. We furthermore extend the treatment into the large distortion regime to also cover the redshift range $simeq 2times 10^6-4times 10^7$ between the $mu$-era and the end of BBN using CosmoTherm. This shows that the CMB distortion constraints for dark photon masses in the range $10^{-4},{rm eV}lesssim m_{rm dp}lesssim 10^{-3},{rm eV}$ were significantly underestimated. We demonstrate that in the small distortion regime the distortion caused by photon to dark photon conversion is extremely close to a $mu$-type distortion independent of the conversion redshift. This opens the possibility to study dark photon models using CMB distortion anisotropies and the correlations with CMB temperature anisotropies as we highlight here.
{"title":"Revisiting Dark Photon Constraints from CMB Spectral Distortions","authors":"Jens Chluba, Bryce Cyr, Matthew C. Johnson","doi":"arxiv-2409.12115","DOIUrl":"https://doi.org/arxiv-2409.12115","url":null,"abstract":"Spectral distortions of the cosmic microwave background (CMB) provide\u0000stringent constraints on energy and entropy production in the post-BBN (Big\u0000Bang Nucleosynthesis) era. This has been used to constrain dark photon models\u0000with COBE/FIRAS and forecast the potential gains with future CMB spectrometers.\u0000Here, we revisit these constraints by carefully considering the photon to dark\u0000photon conversion process and evolution of the distortion signal. Previous\u0000works only included the effect of CMB energy density changes but neglected the\u0000change to the photon number density. We clearly define the dark photon\u0000distortion signal and show that in contrast to previous analytic estimates the\u0000distortion has an opposite sign and a $simeq 1.5$ times larger amplitude. We\u0000furthermore extend the treatment into the large distortion regime to also cover\u0000the redshift range $simeq 2times 10^6-4times 10^7$ between the $mu$-era and\u0000the end of BBN using CosmoTherm. This shows that the CMB distortion constraints\u0000for dark photon masses in the range $10^{-4},{rm eV}lesssim m_{rm\u0000dp}lesssim 10^{-3},{rm eV}$ were significantly underestimated. We\u0000demonstrate that in the small distortion regime the distortion caused by photon\u0000to dark photon conversion is extremely close to a $mu$-type distortion\u0000independent of the conversion redshift. This opens the possibility to study\u0000dark photon models using CMB distortion anisotropies and the correlations with\u0000CMB temperature anisotropies as we highlight here.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"205 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142251476","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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