This note expands on the details of the relationship between 4d kination solutions in string cosmology and Kasner solutions of 10d general relativity. It extends previous analyses of this relationship in IIB string theory to other string theories and also to 11d M-theory, while also providing extensive detail on the relationship between perturbations of the 10d Kasner metric and the presence of radiation and matter backgrounds in the dimensionally reduced 4d kination theory.
{"title":"A Note on 4d Kination and Higher-Dimensional Uplifts","authors":"Fien Apers, Joseph P. Conlon, Martin Mosny","doi":"arxiv-2409.08049","DOIUrl":"https://doi.org/arxiv-2409.08049","url":null,"abstract":"This note expands on the details of the relationship between 4d kination\u0000solutions in string cosmology and Kasner solutions of 10d general relativity.\u0000It extends previous analyses of this relationship in IIB string theory to other\u0000string theories and also to 11d M-theory, while also providing extensive detail\u0000on the relationship between perturbations of the 10d Kasner metric and the\u0000presence of radiation and matter backgrounds in the dimensionally reduced 4d\u0000kination theory.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175967","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}
Yang Jiang, Chen Yuan, Chong-Zhi Li, Qing-Guo Huang
As a promising dark matter candidate, primordial black holes (PBHs) lighter than $sim10^{-18}M_{odot}$ are supposed to have evaporated by today through Hawking radiation. This scenario is challenged by the memory burden effect, which suggests that the evaporation of black holes may slow down significantly after they have emitted about half of their initial mass. We explore the astrophysical implications of the memory burden effect on the PBH abundance by today and the possibility for PBHs lighter than $sim10^{-18}M_{odot}$ to persist as dark matter. Our analysis utilizes current LIGO-Virgo-KAGRA data to constrain the primordial power spectrum and infers the PBH abundance. We find a null detection of scalar-induced gravitational waves that accompanied the formation of the PBHs. Then we place an upper limit on the primordial power spectrum and the PBH abundance to be $f_{mathrm{pbh}}simeq0.3$ for PBHs with masses $sim10^{-24}M_{odot}$. Furthermore, we expect that next-generation gravitational wave detectors, such as the Einstein Telescope and the Cosmic Explorer, will provide even more stringent constraints. Our results indicate that future detectors can reach sensitivities that could rule out PBH as dark matter within $sim[10^{-29}M_{odot},10^{-19}M_{odot}]$ in the null detection of scalar-induced gravitational waves.
{"title":"Constraints on the Primordial Black Hole Abundance through Scalar-Induced Gravitational Waves from Advanced LIGO and Virgo's First Three Observing Runs","authors":"Yang Jiang, Chen Yuan, Chong-Zhi Li, Qing-Guo Huang","doi":"arxiv-2409.07976","DOIUrl":"https://doi.org/arxiv-2409.07976","url":null,"abstract":"As a promising dark matter candidate, primordial black holes (PBHs) lighter\u0000than $sim10^{-18}M_{odot}$ are supposed to have evaporated by today through\u0000Hawking radiation. This scenario is challenged by the memory burden effect,\u0000which suggests that the evaporation of black holes may slow down significantly\u0000after they have emitted about half of their initial mass. We explore the\u0000astrophysical implications of the memory burden effect on the PBH abundance by\u0000today and the possibility for PBHs lighter than $sim10^{-18}M_{odot}$ to\u0000persist as dark matter. Our analysis utilizes current LIGO-Virgo-KAGRA data to\u0000constrain the primordial power spectrum and infers the PBH abundance. We find a\u0000null detection of scalar-induced gravitational waves that accompanied the\u0000formation of the PBHs. Then we place an upper limit on the primordial power\u0000spectrum and the PBH abundance to be $f_{mathrm{pbh}}simeq0.3$ for PBHs with\u0000masses $sim10^{-24}M_{odot}$. Furthermore, we expect that next-generation\u0000gravitational wave detectors, such as the Einstein Telescope and the Cosmic\u0000Explorer, will provide even more stringent constraints. Our results indicate\u0000that future detectors can reach sensitivities that could rule out PBH as dark\u0000matter within $sim[10^{-29}M_{odot},10^{-19}M_{odot}]$ in the null detection\u0000of scalar-induced gravitational waves.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"53 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175980","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 investigate a coupled system consisting of a complex scalar field, a U(1) gauge field, a complex Higgs scalar field, and Einstein gravity. We present nontopological soliton star solutions in which the interior geometry is described by the de Sitter metric, the exterior by the Schwarzschild metric, and these two regions are attached by a spherical surface layer with a finite thickness. This structure is the same as the so-called gravastars, so we refer to these solutions as lq solitonic gravastarsrq . We demonstrate that compact solitonic gravastars that possessing photon spheres can appear. Additionally, we study the mass and compactness of solitonic gravastars for various sets of parameters that characterize the system.
{"title":"Gravastars as Nontopological Solitons","authors":"Tatsuya Ogawa, Hideki Ishihara","doi":"arxiv-2409.07818","DOIUrl":"https://doi.org/arxiv-2409.07818","url":null,"abstract":"We investigate a coupled system consisting of a complex scalar field, a U(1)\u0000gauge field, a complex Higgs scalar field, and Einstein gravity. We present\u0000nontopological soliton star solutions in which the interior geometry is\u0000described by the de Sitter metric, the exterior by the Schwarzschild metric,\u0000and these two regions are attached by a spherical surface layer with a finite\u0000thickness. This structure is the same as the so-called gravastars, so we refer\u0000to these solutions as lq solitonic gravastarsrq . We demonstrate that compact\u0000solitonic gravastars that possessing photon spheres can appear. Additionally,\u0000we study the mass and compactness of solitonic gravastars for various sets of\u0000parameters that characterize the system.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"152 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175968","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}
Guoyang Fu, Yunqi Liu, Bin Wang, Jian-Pin Wu, Chao Zhang
In this paper, we investigate the impact of loop quantum gravity (LQG) on extreme mass-ratio inspirals (EMRIs), and the results indicate that LQG effects cause the orbital decay to occur faster compared to the Schwarzschild case. Furthermore, we use the augmented analytic kludge approach to generate EMRI waveforms and study the LISA's capability to detect the LQG effect with faithfulness. Additionally, employing the Fisher information matrix method for parameter estimation, we estimate that after one year of observation, the uncertainty in $r_0$ reduces to approximately $6.59times 10^{-4}$ with a signal-to-noise ratio of $49$.
{"title":"Probing Quantum Gravity Effects with Eccentric Extreme Mass-Ratio Inspirals","authors":"Guoyang Fu, Yunqi Liu, Bin Wang, Jian-Pin Wu, Chao Zhang","doi":"arxiv-2409.08138","DOIUrl":"https://doi.org/arxiv-2409.08138","url":null,"abstract":"In this paper, we investigate the impact of loop quantum gravity (LQG) on\u0000extreme mass-ratio inspirals (EMRIs), and the results indicate that LQG effects\u0000cause the orbital decay to occur faster compared to the Schwarzschild case.\u0000Furthermore, we use the augmented analytic kludge approach to generate EMRI\u0000waveforms and study the LISA's capability to detect the LQG effect with\u0000faithfulness. Additionally, employing the Fisher information matrix method for\u0000parameter estimation, we estimate that after one year of observation, the\u0000uncertainty in $r_0$ reduces to approximately $6.59times 10^{-4}$ with a\u0000signal-to-noise ratio of $49$.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175976","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 article, we study the black hole evaporation process and shadow property of the Tangherlini-Reissner-Nordstr"om (TRN) black holes. The TRN black holes are the higher-dimensional extension of the Reissner-Nordstr"om (RN) black holes and are characterized by their mass $M$, charge $q$, and spacetime dimensions $D$. In higher-dimensional spacetime, the black hole evaporation occurs rapidly, causing the black hole's horizon to shrink. We derive the rate of mass loss for the higher-dimensional charged black hole and investigate the effect of higher-dimensional spacetime on charged black hole shadow. We derive the complete geodesic equations of motion with the effect of spacetime dimensions $D$. We determine impact parameters by maximizing the black hole's effective potential and estimate the critical radius of photon orbits. The photon orbits around the black hole shrink with the effect of the increasing number of spacetime dimensions. To visualize the shadows of the black hole, we derive the celestial coordinates in terms of the black hole parameters. We use the observed results of M87 and Sgr A$^{*}$ black hole from the Event Horizon Telescope and estimate the angular diameter of the charge black hole shadow in the higher-dimensional spacetime. We also estimate the energy emission rate of the black hole. Our finding shows that the angular diameter of the black hole shadow decreases with the increasing number of spacetime dimensions $D$.
{"title":"Black Hole Evaporation Process and Tangherlini-Reissner-Nordström Black Holes Shadow","authors":"Balendra Pratap Singh","doi":"arxiv-2409.07951","DOIUrl":"https://doi.org/arxiv-2409.07951","url":null,"abstract":"In this article, we study the black hole evaporation process and shadow\u0000property of the Tangherlini-Reissner-Nordstr\"om (TRN) black holes. The TRN\u0000black holes are the higher-dimensional extension of the Reissner-Nordstr\"om\u0000(RN) black holes and are characterized by their mass $M$, charge $q$, and\u0000spacetime dimensions $D$. In higher-dimensional spacetime, the black hole\u0000evaporation occurs rapidly, causing the black hole's horizon to shrink. We\u0000derive the rate of mass loss for the higher-dimensional charged black hole and\u0000investigate the effect of higher-dimensional spacetime on charged black hole\u0000shadow. We derive the complete geodesic equations of motion with the effect of\u0000spacetime dimensions $D$. We determine impact parameters by maximizing the\u0000black hole's effective potential and estimate the critical radius of photon\u0000orbits. The photon orbits around the black hole shrink with the effect of the\u0000increasing number of spacetime dimensions. To visualize the shadows of the\u0000black hole, we derive the celestial coordinates in terms of the black hole\u0000parameters. We use the observed results of M87 and Sgr A$^{*}$ black hole from\u0000the Event Horizon Telescope and estimate the angular diameter of the charge\u0000black hole shadow in the higher-dimensional spacetime. We also estimate the\u0000energy emission rate of the black hole. Our finding shows that the angular\u0000diameter of the black hole shadow decreases with the increasing number of\u0000spacetime dimensions $D$.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175978","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 gauge theories, the running of the anomalous dimension of a fermion bilinear operator is believed to lead to chiral symmetry breaking when gamma=1. Naively using perturbative results to judge when gamma=1 leads to the possibility of large dynamically generated mass hierarchies in models with both two index symmetric representation and fundamental representation fermions. In this paper we study a holographic model of this physics to predict the separation in scales in the meson spectrum. We study SU(Nc) theories at different Nc with one flavour of two index symmetric representation as a function of the number of fundamental fermion flavours NfF. The largest hierarchy we find is for Nc=7 and NfF=22 where the rho mesons made of the two different representations are separated in scale by a factor of 13. For general Nc the hierarchy can be made greater than 7 by tuning NfF. We display the hierarchy as a function of NfF and investigate the quark mass dependence. These predictions do depend on the extrapolation of gamma from the perturbative regime - even in a pessimistic scenario a distinct gap can be achieved.
{"title":"Mass hierarchies in gauge theory with two index symmetric representation matter","authors":"Anja Alfano, Nick Evans","doi":"arxiv-2409.07977","DOIUrl":"https://doi.org/arxiv-2409.07977","url":null,"abstract":"In gauge theories, the running of the anomalous dimension of a fermion\u0000bilinear operator is believed to lead to chiral symmetry breaking when gamma=1.\u0000Naively using perturbative results to judge when gamma=1 leads to the\u0000possibility of large dynamically generated mass hierarchies in models with both\u0000two index symmetric representation and fundamental representation fermions. In\u0000this paper we study a holographic model of this physics to predict the\u0000separation in scales in the meson spectrum. We study SU(Nc) theories at\u0000different Nc with one flavour of two index symmetric representation as a\u0000function of the number of fundamental fermion flavours NfF. The largest\u0000hierarchy we find is for Nc=7 and NfF=22 where the rho mesons made of the two\u0000different representations are separated in scale by a factor of 13. For general\u0000Nc the hierarchy can be made greater than 7 by tuning NfF. We display the\u0000hierarchy as a function of NfF and investigate the quark mass dependence. These\u0000predictions do depend on the extrapolation of gamma from the perturbative\u0000regime - even in a pessimistic scenario a distinct gap can be achieved.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175977","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}
The lowest Landau level on the sphere was recently proposed as a continuum regularization of the three-dimensional conformal field theories, the so-called fuzzy sphere regularization. In this note, we propose an explicit construction of the conformal generators on the fuzzy sphere in terms of the microscopic Hamiltonian. Specifically, we construct the generators for the translation and special conformal transformation, which are used in defining the conformal primary states and thus are of special interest. We apply our method to a concrete example, the fuzzy sphere regularized three-dimensional Ising conformal field theory. We show that it can help capture all primaries with spin $ell < 4$ and scaling dimension $Delta < 7$. In particular, our method can clearly separate the primary from other states that differ in scaling dimension by $1%$, making it hard otherwise based solely on using the conformal tower associated with the primaries.
{"title":"Note on explicit construction of conformal generators on the fuzzy sphere","authors":"Ruihua Fan","doi":"arxiv-2409.08257","DOIUrl":"https://doi.org/arxiv-2409.08257","url":null,"abstract":"The lowest Landau level on the sphere was recently proposed as a continuum\u0000regularization of the three-dimensional conformal field theories, the so-called\u0000fuzzy sphere regularization. In this note, we propose an explicit construction\u0000of the conformal generators on the fuzzy sphere in terms of the microscopic\u0000Hamiltonian. Specifically, we construct the generators for the translation and\u0000special conformal transformation, which are used in defining the conformal\u0000primary states and thus are of special interest. We apply our method to a\u0000concrete example, the fuzzy sphere regularized three-dimensional Ising\u0000conformal field theory. We show that it can help capture all primaries with\u0000spin $ell < 4$ and scaling dimension $Delta < 7$. In particular, our method\u0000can clearly separate the primary from other states that differ in scaling\u0000dimension by $1%$, making it hard otherwise based solely on using the\u0000conformal tower associated with the primaries.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175964","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 present a procedure g5anchor to anchor $gamma_5$ in the definition of a Dirac trace with $gamma_5$ in Dimensional Regularization (DR) in Feynman diagrams for the Standard Model, based on a recent revision of the works by Kreimer, Gottlieb and Donohue. For each closed fermion chain with an odd number of primitive (i.e.~not-yet-clearly-defined) $gamma_5$ in a given Feynman diagram, g5anchor returns a definite set of anchor points for $gamma_5$, in terms of pairs of ordered fermion propagators; at each of these $gamma_5$ anchor points a fixed expression in terms of the Levi-Civita tensor and elementary Dirac matrices will be inserted together with a sign determined by anticommutatively shifting all $gamma_5$ from their original places (dictated by the Feynman rules) to this anchor point. The defining expressions for the cyclic $gamma_5$-odd Dirac traces in DR associated with closed fermion chains in amplitudes, or more generally squared amplitudes, thus follow from this procedure, where the Levi-Civita tensors are not necessarily treated strictly in 4-dimensions. We propose utilizing this definition in practical perturbative calculations in the Standard Model at least to three-loop orders with the current implementation, and maybe to higher loop orders in absence of Yukawa couplings to Higgs fields. Certain limitations and modifications of the KKS and/or the Kreimer scheme are addressed.
{"title":"A Procedure g5anchor to Anchor $γ_5$ in Feynman Diagrams for the Standard Model","authors":"Long Chen","doi":"arxiv-2409.08099","DOIUrl":"https://doi.org/arxiv-2409.08099","url":null,"abstract":"We present a procedure g5anchor to anchor $gamma_5$ in the definition of a\u0000Dirac trace with $gamma_5$ in Dimensional Regularization (DR) in Feynman\u0000diagrams for the Standard Model, based on a recent revision of the works by\u0000Kreimer, Gottlieb and Donohue. For each closed fermion chain with an odd number\u0000of primitive (i.e.~not-yet-clearly-defined) $gamma_5$ in a given Feynman\u0000diagram, g5anchor returns a definite set of anchor points for $gamma_5$, in\u0000terms of pairs of ordered fermion propagators; at each of these $gamma_5$\u0000anchor points a fixed expression in terms of the Levi-Civita tensor and\u0000elementary Dirac matrices will be inserted together with a sign determined by\u0000anticommutatively shifting all $gamma_5$ from their original places (dictated\u0000by the Feynman rules) to this anchor point. The defining expressions for the\u0000cyclic $gamma_5$-odd Dirac traces in DR associated with closed fermion chains\u0000in amplitudes, or more generally squared amplitudes, thus follow from this\u0000procedure, where the Levi-Civita tensors are not necessarily treated strictly\u0000in 4-dimensions. We propose utilizing this definition in practical perturbative\u0000calculations in the Standard Model at least to three-loop orders with the\u0000current implementation, and maybe to higher loop orders in absence of Yukawa\u0000couplings to Higgs fields. Certain limitations and modifications of the KKS\u0000and/or the Kreimer scheme are addressed.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"384 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142176026","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 study a magnetic domain wall in the ferromagnetic phase in chiral magnets in two dimensions with an in-plane easy-axis anisotropy and an out-of-plane Zeeman magnetic field, and find a chiral soliton lattice (spiral) phase beside a ferromegnetic phase inside the domain line, where the former represents a domain-wall skyrmion crystal from the bulk point of view. We first determine the phase diagram on the domain wall by numerically constructing domain wall solutions. We then analytically reproduce the phase diagram in a domain-wall theory (a chiral double sine-Gordon model) that we construct within the moduli approximation by treating the Zeeman magnetic field perturbatively. While we find good agreements between the phase diagrams of the numerical and effective theory methods, the numerical solution exhibits a decomposition of the topological charge into a bimeron which cannot be captured by the effective theory.
{"title":"Skyrmion crystal phase on a magnetic domain wall in chiral magnets","authors":"Yuki Amari, Muneto Nitta","doi":"arxiv-2409.07943","DOIUrl":"https://doi.org/arxiv-2409.07943","url":null,"abstract":"We study a magnetic domain wall in the ferromagnetic phase in chiral magnets\u0000in two dimensions with an in-plane easy-axis anisotropy and an out-of-plane\u0000Zeeman magnetic field, and find a chiral soliton lattice (spiral) phase beside\u0000a ferromegnetic phase inside the domain line, where the former represents a\u0000domain-wall skyrmion crystal from the bulk point of view. We first determine\u0000the phase diagram on the domain wall by numerically constructing domain wall\u0000solutions. We then analytically reproduce the phase diagram in a domain-wall\u0000theory (a chiral double sine-Gordon model) that we construct within the moduli\u0000approximation by treating the Zeeman magnetic field perturbatively. While we\u0000find good agreements between the phase diagrams of the numerical and effective\u0000theory methods, the numerical solution exhibits a decomposition of the\u0000topological charge into a bimeron which cannot be captured by the effective\u0000theory.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175979","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}
Jing-Zhi Zhou, Yu-Ting Kuang, Di Wu, Fei-Yu Chen, H. Lü, Zhe Chang
We investigate the first and second order cosmological perturbation equations in f(R) modified gravity theory and provide the equation of motion of second order scalar induced gravitational waves. We find that the effects of modified gravity not only change the form of the equation of motion of second order scalar induced gravitational waves but also contribute an additional anisotropic stress tensor, composed of first order scalar perturbations, to the source term of the gravitational waves. We calculate the energy density spectrum of second order scalar induced gravitational waves in the HS model. Utilizing current pulsar timing array observational data, we perform a rigorous Bayesian analysis of the parameter space of the HS model.
{"title":"Scalar induced gravitational waves in f(R) gravity","authors":"Jing-Zhi Zhou, Yu-Ting Kuang, Di Wu, Fei-Yu Chen, H. Lü, Zhe Chang","doi":"arxiv-2409.07702","DOIUrl":"https://doi.org/arxiv-2409.07702","url":null,"abstract":"We investigate the first and second order cosmological perturbation equations\u0000in f(R) modified gravity theory and provide the equation of motion of second\u0000order scalar induced gravitational waves. We find that the effects of modified\u0000gravity not only change the form of the equation of motion of second order\u0000scalar induced gravitational waves but also contribute an additional\u0000anisotropic stress tensor, composed of first order scalar perturbations, to the\u0000source term of the gravitational waves. We calculate the energy density\u0000spectrum of second order scalar induced gravitational waves in the HS model.\u0000Utilizing current pulsar timing array observational data, we perform a rigorous\u0000Bayesian analysis of the parameter space of the HS model.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175981","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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