The standard Komar charge is a $(d-2)$-form that can be defined in spacetimes admitting a Killing vector and which is closed when the vacuum Einstein equations are satisfied. Its integral at spatial infinity (the Komar integral) gives the conserved charge associated to the Killing vector, and, due to its on-shell closedness, the same value (expressed in terms of other physical variables) is obtained integrating over the event horizon (if any). This equality is the basis of the Smarr formula. This charge can be generalized so that it still is closed on-shell in presence of matter and its integrals give generalizations of the Smarr formula. We show how the Komar charge and other closed $(d-2)$-form charges can be used to prove non-existence theorems for gravitational solitons and boson stars. In particular, we show how one can deal with generalized symmetric fields (invariant under a combination of isometries and other global symmetries) and how the geralized symmetric ansatz permits to evade the non-existence theorems.
{"title":"Generalized Komar charges and Smarr formulas for black holes and boson stars","authors":"Romina Ballesteros, Tomas Ortin","doi":"arxiv-2409.08268","DOIUrl":"https://doi.org/arxiv-2409.08268","url":null,"abstract":"The standard Komar charge is a $(d-2)$-form that can be defined in spacetimes\u0000admitting a Killing vector and which is closed when the vacuum Einstein\u0000equations are satisfied. Its integral at spatial infinity (the Komar integral)\u0000gives the conserved charge associated to the Killing vector, and, due to its\u0000on-shell closedness, the same value (expressed in terms of other physical\u0000variables) is obtained integrating over the event horizon (if any). This\u0000equality is the basis of the Smarr formula. This charge can be generalized so\u0000that it still is closed on-shell in presence of matter and its integrals give\u0000generalizations of the Smarr formula. We show how the Komar charge and other\u0000closed $(d-2)$-form charges can be used to prove non-existence theorems for\u0000gravitational solitons and boson stars. In particular, we show how one can deal\u0000with generalized symmetric fields (invariant under a combination of isometries\u0000and other global symmetries) and how the geralized symmetric ansatz permits to\u0000evade the non-existence theorems.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"16 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175975","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 construct the first-order perturbative Taub-NUT black hole solutions in Einstein gravity extended with a cubic curvature invariant. The corrected thermodynamic quantities are then obtained by the standard method and the first law and Smarr relation are satisfied. We also study the perturbative correction to thermodynamics using the Reall-Santos (RS) method and verify that the method is still applicable even though the metrics are no longer asymptotic to Minkowski spacetime. We then apply the RS method to obtain the leading correction to the thermodynamics of the complicated Kerr-Taub-NUT black holes.
{"title":"Taub-NUT Black Hole in Higher Derivative Gravity and Its Thermodynamics","authors":"Yu-Qi Chen, Hai-Shan Liu, H. Lu","doi":"arxiv-2409.07692","DOIUrl":"https://doi.org/arxiv-2409.07692","url":null,"abstract":"We construct the first-order perturbative Taub-NUT black hole solutions in\u0000Einstein gravity extended with a cubic curvature invariant. The corrected\u0000thermodynamic quantities are then obtained by the standard method and the first\u0000law and Smarr relation are satisfied. We also study the perturbative correction\u0000to thermodynamics using the Reall-Santos (RS) method and verify that the method\u0000is still applicable even though the metrics are no longer asymptotic to\u0000Minkowski spacetime. We then apply the RS method to obtain the leading\u0000correction to the thermodynamics of the complicated Kerr-Taub-NUT black holes.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"153 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142176033","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 years, the holographic duality between $Tbar{T}$-deformed conformal field theory (CFT) and Anti-de Sitter (AdS) space with finite radial truncation has received significant attention. The study of $Tbar{T}$ deformation within the framework of de Sitter (dS)/CFT duality has also progressed. This paper shows that the trace flow equation in dS spacetime can be analytically extended from its AdS counterpart through double Wick rotations. Additionally, we generalize the replica sphere method in both AdS and dS holography to derive a general expression for the entanglement entropy of arbitrary single spatial intervals. For both finite size and finite temperature systems, we obtain the entanglement entropy corrections due to $Tbar{T}$ deformation. Finally, using strong subadditivity and boosted strong subadditivity, we show that the dual field theory on the timelike boundary is non-local in dS holography.
{"title":"The holographic $Tbar{T}$ deformation of the entanglement entropy in (A)dS$_3$/CFT$_2$","authors":"Jing-Cheng Chang, Song He, Yu-Xiao Liu, Long Zhao","doi":"arxiv-2409.08198","DOIUrl":"https://doi.org/arxiv-2409.08198","url":null,"abstract":"In recent years, the holographic duality between $Tbar{T}$-deformed\u0000conformal field theory (CFT) and Anti-de Sitter (AdS) space with finite radial\u0000truncation has received significant attention. The study of $Tbar{T}$\u0000deformation within the framework of de Sitter (dS)/CFT duality has also\u0000progressed. This paper shows that the trace flow equation in dS spacetime can\u0000be analytically extended from its AdS counterpart through double Wick\u0000rotations. Additionally, we generalize the replica sphere method in both AdS\u0000and dS holography to derive a general expression for the entanglement entropy\u0000of arbitrary single spatial intervals. For both finite size and finite\u0000temperature systems, we obtain the entanglement entropy corrections due to\u0000$Tbar{T}$ deformation. Finally, using strong subadditivity and boosted strong\u0000subadditivity, we show that the dual field theory on the timelike boundary is\u0000non-local in dS holography.","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":"142175965","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 $ mathcal{O}left( r^N right) $ asymptotic symmetries for a two-form gauge field in four-dimensional Minkowski spacetime. By employing symplectic renormalization, we identify $ N $ independent asymptotic charges, with each charge being parametrised by an arbitrary function of the angular variables. Working in Lorenz gauge, the gauge parameters require a radial expansion involving logarithmic (subleading) terms to ensure nontrivial angular dependence at leading order. At the same time, we adopt a setup where the field strength admits a power expansion, allowing logarithms in the gauge field expansions within pure gauge sectors. The same setup is studied for electromagnetism.
我们研究了四维闵科夫斯基时空中两形式规量场的$ mathcal{O}left( r^N right) $渐近对称性。通过采用交错重正化，我们确定了 $ N $ 独立渐近电荷，每个电荷由角变量的任意函数参数化。在洛伦兹规中工作时，规参数需要涉及对数（次前导）项的径向展开，以确保在前导阶时的非rivial角度依赖性。同时，我们采用了一种场强允许幂级数展开的设置，允许在纯轨距扇形内的轨距场展开中使用对数。同样的设置也用于研究电磁学。
{"title":"${mathcal{O}(r^N)} $ two-form asymptotic symmetries and renormalized charges","authors":"Matteo Romoli","doi":"arxiv-2409.08131","DOIUrl":"https://doi.org/arxiv-2409.08131","url":null,"abstract":"We investigate $ mathcal{O}left( r^N right) $ asymptotic symmetries for a\u0000two-form gauge field in four-dimensional Minkowski spacetime. By employing\u0000symplectic renormalization, we identify $ N $ independent asymptotic charges,\u0000with each charge being parametrised by an arbitrary function of the angular\u0000variables. Working in Lorenz gauge, the gauge parameters require a radial\u0000expansion involving logarithmic (subleading) terms to ensure nontrivial angular\u0000dependence at leading order. At the same time, we adopt a setup where the field\u0000strength admits a power expansion, allowing logarithms in the gauge field\u0000expansions within pure gauge sectors. The same setup is studied for\u0000electromagnetism.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"2016 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175966","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 the present work we introduce a holographic prescription to independently describe sea and valence quarks in the context of the gauge/gravity correspondence. We use such prescription to perform an initial calculation that permits us to compare our results with those obtained through lattice techniques when studding magnetic catalysis and its inverse. We find, in agreement with previous studies, that the elaborated behavior of the condensate is mostly attributable to the sea quarks, rather than the valence which show a quite featureless participation.
{"title":"Identifying sea and valence quarks in a magnetically driven catalysis","authors":"Daniel Kosoi, Leonardo Patiño","doi":"arxiv-2409.07531","DOIUrl":"https://doi.org/arxiv-2409.07531","url":null,"abstract":"In the present work we introduce a holographic prescription to independently\u0000describe sea and valence quarks in the context of the gauge/gravity\u0000correspondence. We use such prescription to perform an initial calculation that\u0000permits us to compare our results with those obtained through lattice\u0000techniques when studding magnetic catalysis and its inverse. We find, in\u0000agreement with previous studies, that the elaborated behavior of the condensate\u0000is mostly attributable to the sea quarks, rather than the valence which show a\u0000quite featureless participation.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"122 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175972","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 (multi) fermion - monopole bound states, many of which are the states that dyons adiabatically transition into as fermions become light. The properties of these bound states depend critically on the UV symmetries preserved by the fermion mass terms, their relative size, and the value of $theta$. Depending on the relative size of the mass terms and the value of $theta$, the bound states can undergo phase transitions as well as transition from being stable to unstable. In some simple situations, the bound state solution can be related to the Witten effect of another theory with fewer fermions and larger gauge coupling. These bound states are a result of mass terms and symmetry breaking boundary conditions at the monopole core and, consequently, these bound states do not necessarily have definite quantum numbers under accidental IR symmetries. Additionally, they have binding energies that are $mathcal{O}(1)$ times the fermion mass and bound state radii of order their inverse mass. As the massless limit is approached, the bound state radii approach infinity, and they become new asymptotic states with odd quantum numbers giving a dynamical understanding to the origin of semitons.
{"title":"Dyonic bound states","authors":"Anson Hook, Clayton Ristow","doi":"arxiv-2409.07549","DOIUrl":"https://doi.org/arxiv-2409.07549","url":null,"abstract":"We study (multi) fermion - monopole bound states, many of which are the\u0000states that dyons adiabatically transition into as fermions become light. The\u0000properties of these bound states depend critically on the UV symmetries\u0000preserved by the fermion mass terms, their relative size, and the value of\u0000$theta$. Depending on the relative size of the mass terms and the value of\u0000$theta$, the bound states can undergo phase transitions as well as transition\u0000from being stable to unstable. In some simple situations, the bound state\u0000solution can be related to the Witten effect of another theory with fewer\u0000fermions and larger gauge coupling. These bound states are a result of mass\u0000terms and symmetry breaking boundary conditions at the monopole core and,\u0000consequently, these bound states do not necessarily have definite quantum\u0000numbers under accidental IR symmetries. Additionally, they have binding\u0000energies that are $mathcal{O}(1)$ times the fermion mass and bound state radii\u0000of order their inverse mass. As the massless limit is approached, the bound\u0000state radii approach infinity, and they become new asymptotic states with odd\u0000quantum numbers giving a dynamical understanding to the origin of semitons.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"40 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175970","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 derive a cutting rule for equal-time in-in correlators including cosmological correlators based on Keldysh $r/a$ basis, which decomposes diagrams into fully retarded functions and cut-propagators consisting of Wightman functions. Our derivation relies only on basic assumptions such as unitarity, locality, and the causal structure of the in-in formalism, and therefore holds for theories with arbitrary particle contents and local interactions at any loop order. As an application, we show that non-local cosmological collider signals arise solely from cut-propagators under the assumption of microcausality. Since the cut-propagators do not contain (anti-)time-ordering theta functions, the conformal time integrals are factorized, simplifying practical calculations.
{"title":"Cutting rule for in-in correlators and cosmological collider","authors":"Yohei Ema, Kyohei Mukaida","doi":"arxiv-2409.07521","DOIUrl":"https://doi.org/arxiv-2409.07521","url":null,"abstract":"We derive a cutting rule for equal-time in-in correlators including\u0000cosmological correlators based on Keldysh $r/a$ basis, which decomposes\u0000diagrams into fully retarded functions and cut-propagators consisting of\u0000Wightman functions. Our derivation relies only on basic assumptions such as\u0000unitarity, locality, and the causal structure of the in-in formalism, and\u0000therefore holds for theories with arbitrary particle contents and local\u0000interactions at any loop order. As an application, we show that non-local\u0000cosmological collider signals arise solely from cut-propagators under the\u0000assumption of microcausality. Since the cut-propagators do not contain\u0000(anti-)time-ordering theta functions, the conformal time integrals are\u0000factorized, simplifying practical calculations.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175974","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}
It has recently been conjectured [A. Ianniccari {it et al.}, Phys. Rev. Lett. {bf 133}, 081401 (2024)] that there exists a correspondence between the critical threshold of black-hole formation and the stability properties of null circular geodesics in the curved spacetime of the collapsing matter configuration. In the present compact paper we provide a non-trivial test of this intriguing conjecture. In particular, using analytical techniques we study the physical and mathematical properties of self-gravitating scalar field configurations that possess marginally-stable (degenerate) null circular geodesics. We reveal the interesting fact that the {it analytically} calculated critical compactness parameter ${cal C}^{text{analytical}}equiv{text{max}_r}{m(r)/r}=6/25$, which signals the appearance of the first (marginally-stable) null circular geodesic in the curved spacetime of the self-gravitating scalar fields, agrees quite well (to within $sim10%$) with the exact compactness parameter ${cal C}^{text{numerical}}equivtext{max}_t{text{max}_r{m(r)/r}}simeq0.265$ which is computed {it numerically} using fully non-linear numerical simulations of the gravitational collapse of scalar fields at the threshold of black-hole formation [here $m(r)$ is the gravitational mass contained within a sphere of radius $r$].
{"title":"A test of the conjectured critical black-hole formation -- null geodesic correspondence: The case of self-gravitating scalar fields","authors":"Shahar Hod","doi":"arxiv-2409.07517","DOIUrl":"https://doi.org/arxiv-2409.07517","url":null,"abstract":"It has recently been conjectured [A. Ianniccari {it et al.}, Phys. Rev.\u0000Lett. {bf 133}, 081401 (2024)] that there exists a correspondence between the\u0000critical threshold of black-hole formation and the stability properties of null\u0000circular geodesics in the curved spacetime of the collapsing matter\u0000configuration. In the present compact paper we provide a non-trivial test of\u0000this intriguing conjecture. In particular, using analytical techniques we study\u0000the physical and mathematical properties of self-gravitating scalar field\u0000configurations that possess marginally-stable (degenerate) null circular\u0000geodesics. We reveal the interesting fact that the {it analytically}\u0000calculated critical compactness parameter ${cal\u0000C}^{text{analytical}}equiv{text{max}_r}{m(r)/r}=6/25$, which signals the\u0000appearance of the first (marginally-stable) null circular geodesic in the\u0000curved spacetime of the self-gravitating scalar fields, agrees quite well (to\u0000within $sim10%$) with the exact compactness parameter ${cal\u0000C}^{text{numerical}}equivtext{max}_t{text{max}_r{m(r)/r}}simeq0.265$\u0000which is computed {it numerically} using fully non-linear numerical\u0000simulations of the gravitational collapse of scalar fields at the threshold of\u0000black-hole formation [here $m(r)$ is the gravitational mass contained within a\u0000sphere of radius $r$].","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175983","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}
I. Andrade, D. Bazeia, M. A. Marques, R. Menezes, G. J. Olmo
We investigate Maxwell-scalar models on radially symmetric spacetimes in which the gauge and scalar fields are coupled via the electric permittivity. We find the conditions that allow for the presence of minimum energy configurations. In this formalism, the charge density must be written exclusively in terms of the components of the metric tensor and the scalar field is governed by first-order equations. We also find a manner to map the aforementioned equation into the corresponding one associated to kinks in $(1,1)$ spacetime dimensions, so we get analytical solutions for three specific spacetimes. We then calculate the energy density and show that the energy is finite. The stability of the solutions against contractions and dilations, following Derrick's argument, and around small fluctuations in the fields is also investigated. In this direction, we show that the solutions obeying the first-order framework are stable.
{"title":"Analytical solutions for Maxwell-scalar system on radially symmetric spacetimes","authors":"I. Andrade, D. Bazeia, M. A. Marques, R. Menezes, G. J. Olmo","doi":"arxiv-2409.07633","DOIUrl":"https://doi.org/arxiv-2409.07633","url":null,"abstract":"We investigate Maxwell-scalar models on radially symmetric spacetimes in\u0000which the gauge and scalar fields are coupled via the electric permittivity. We\u0000find the conditions that allow for the presence of minimum energy\u0000configurations. In this formalism, the charge density must be written\u0000exclusively in terms of the components of the metric tensor and the scalar\u0000field is governed by first-order equations. We also find a manner to map the\u0000aforementioned equation into the corresponding one associated to kinks in\u0000$(1,1)$ spacetime dimensions, so we get analytical solutions for three specific\u0000spacetimes. We then calculate the energy density and show that the energy is\u0000finite. The stability of the solutions against contractions and dilations,\u0000following Derrick's argument, and around small fluctuations in the fields is\u0000also investigated. In this direction, we show that the solutions obeying the\u0000first-order framework are stable.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"152 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142175982","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 found that, unlike General Relativity, the shift-symmetric subclass of Beyond Horndeski theories provides black holes with primary hair, which are thermodynamically stable and compatible with current Event Horizon Telescope observations for M87* and Sgr A* black holes. We first investigate its thermodynamic properties by studying the influence of the primary hair on the thermodynamic quantities and the local stability, imposing severe constraints in the allowed range of the primary hair values. Then, we analyze the null geodesics near this black hole, demonstrating how the scalar hair influences the shadow diameter, finding that higher values of the primary hair lead to smaller shadow sizes. Additionally, we constrain the scalar hair using the observational data, revealing its sensitivity to the choice of other black hole parameters. To further probe the observational features of the scalar hair, we simulate face-on two-dimensional images of spherically infalling accretion disks, examining how the primary scalar hair affects the black hole's shadow. Finally, we impose all relevant constraints to identify black holes that are both stable and consistent with observational data.
{"title":"Thermodynamic and observational constraints on black holes with primary hair in Beyond Horndeski Gravity: Stability and shadows","authors":"Cristian Erices, Mohsen Fathi","doi":"arxiv-2409.07312","DOIUrl":"https://doi.org/arxiv-2409.07312","url":null,"abstract":"We found that, unlike General Relativity, the shift-symmetric subclass of\u0000Beyond Horndeski theories provides black holes with primary hair, which are\u0000thermodynamically stable and compatible with current Event Horizon Telescope\u0000observations for M87* and Sgr A* black holes. We first investigate its\u0000thermodynamic properties by studying the influence of the primary hair on the\u0000thermodynamic quantities and the local stability, imposing severe constraints\u0000in the allowed range of the primary hair values. Then, we analyze the null\u0000geodesics near this black hole, demonstrating how the scalar hair influences\u0000the shadow diameter, finding that higher values of the primary hair lead to\u0000smaller shadow sizes. Additionally, we constrain the scalar hair using the\u0000observational data, revealing its sensitivity to the choice of other black hole\u0000parameters. To further probe the observational features of the scalar hair, we\u0000simulate face-on two-dimensional images of spherically infalling accretion\u0000disks, examining how the primary scalar hair affects the black hole's shadow.\u0000Finally, we impose all relevant constraints to identify black holes that are\u0000both stable and consistent with observational data.","PeriodicalId":501339,"journal":{"name":"arXiv - PHYS - High Energy Physics - Theory","volume":"153 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142176023","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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