The European Physical Journal C最新文献

{"title":"Conformal line defects from matter-coupled 5D (N=4) gauged supergravity","authors":"Parinya Karndumri","doi":"10.1140/epjc/s10052-026-16503-4","DOIUrl":"10.1140/epjc/s10052-026-16503-4","url":null,"abstract":"<div><p>We study a number of holographic solutions describing conformal line defects within <span>(N=2)</span> SCFTs from matter-coupled <span>(N=4)</span> gauged supergravity in five dimensions. For <span>(SO(2)_Dtimes SO(3))</span> gauge group, the gauged supergravity admits two supersymmetric <span>(AdS_5)</span> vacua with <span>(N=4)</span> and <span>(N=2)</span> unbroken supersymmetries. It turns out that only solutions that are asymptotic to the <span>(N=4)</span> vacuum are possible leading to line defects within the dual <span>(N=2)</span> SCFT. In gauged supergravity with <span>(SO(2)times ISO(3))</span> gauge group, we find similar solutions with the <span>(N=2)</span> SCFT appearing in the IR while the UV field theories correspond to six-dimensional <span>(N=(0,2))</span> field theories arising from M5-branes wrapped on a hyperbolic space <span>(H^2)</span>. The solution with <span>(SO(2)times SO(3))</span> symmetry is also uplifted to eleven dimensions via a consistent truncation on <span>(H^2times S^4)</span>. Finally, for gauged supergravity with <span>(SO(2)times SO(3)times SO(3))</span> gauge group that admits two <span>(N=4)</span> supersymmetric <span>(AdS_5)</span> vacua, we find a solution describing a line defect that interpolates between these two vacua as well as a solution with only one asymptotic <span>(AdS_5)</span> geometry.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16503-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338907","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Signatures of Lorentz violation in the bright ring for Sgr A* images from radiatively inefficient accretion flows","authors":"Cuiyu Zhao,&nbsp;Songbai Chen,&nbsp;Jiliang Jing","doi":"10.1140/epjc/s10052-026-16583-2","DOIUrl":"10.1140/epjc/s10052-026-16583-2","url":null,"abstract":"<div><p>We have investigated the effects of Lorentz violation (LV) on the bright ring in Sgr A* images illuminated by the 230 GHz thermal synchrotron emission from radiatively inefficient accretion flows around a rotating LV black hole within the low-energy Hořava gravity framework. Our results reveal that the LV parameter reduces the bright ring diameter yet increases its width, luminosity, azimuthal asymmetry and orientation angle. A higher spin parameter strengthens the LV-induced effects on the bright ring properties. Increasing disk thickness reduces the ring diameter and enhances the LV parameter’s effects on this diameter. The ring width shows no systematic dependence on the disk thickness. These quantities of the bright ring display similar trends against the black hole spin and the LV parameter for the rotating LV black hole. Using EHT observational data of Sgr A*, we find that, at fixed disk thickness, the parameter-space map illustrates that the bounded range of the LV parameter first broadens and then contracts with the growing black hole spin, and shifts toward smaller LV parameter values. In addition, the LV parameter narrows the bounded range of black hole spin: negative LV parameter values shift this range to a higher spin, while positive values shift it to a lower spin. Finally, we probe effects of the LV parameter on the peak position value and the width of the primary image and the <span>(n=1)</span> photon ring for the rotating LV black hole. The peak positions and their widths nearly always decrease with the LV parameter. The peak position differences for various LV parameters are more pronounced for a purely Keplerian accretion flow. In addition, the primary image and the <span>(n=1)</span> photon ring produced by purely radially free-falling flows are broader than their counterparts generated by purely Keplerian flows.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16583-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338908","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Meissner effect in Kerr–Bertotti–Robinson spacetime","authors":"Haryanto M. Siahaan","doi":"10.1140/epjc/s10052-026-16539-6","DOIUrl":"10.1140/epjc/s10052-026-16539-6","url":null,"abstract":"<div><p>We study the black-hole Meissner effect for extremal Kerr–Bertotti–Robinson (Kerr–BR) black holes, exact Einstein–Maxwell solutions describing a rotating black hole immersed in a uniform Bertotti–Robinson electromagnetic universe. We show that extremality alone is not sufficient for complete magnetic-flux expulsion in this family. For a purely magnetic external BR field, finite extremal holes with <span>(0&lt;Ba&lt;1)</span> carry the exact northern-hemisphere flux <span>(Phi _N=-2pi Ba^2sqrt{1-B^2a^2})</span>, which is nonzero and maximal in magnitude at <span>(Ba=1/sqrt{2})</span>. Complete expulsion occurs only in the static near-horizon boundary limit <span>(Barightarrow 1^-)</span>, equivalently <span>(krightarrow 0)</span>, where the <i>U</i>(1) fibration of the near-horizon metric trivialises. The proof relies on two exact identities that hold at extremality for all values of the external field, <span>(Omega _x|_{r_e}=0)</span> and <span>(Omega _r|_{r_e}=B^2a)</span>, both consequences of the double-root structure of the horizon function <span>(Delta )</span>. Together they force the azimuthal potential <span>(A_phi |_{r_e})</span> in the purely magnetic sector to become independent of the polar angle in the static boundary limit, so that the gauge-invariant horizon flux density <span>(F_{xphi }|_{r_e})</span> and the flux through any smooth horizon cap vanish. The Kerr–BR result is contrasted with the Kerr–Melvin family, where the static limit occurs at a finite interior field strength, and with the Melvin–Kerr–Newman–Taub–NUT spacetime, where the NUT parameter is known to prevent expulsion. A complementary throat-geometry argument and qualitative implications for Blandford–Znajek jet suppression near the static boundary of the extremal branch are discussed.</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16539-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149339047","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Observational signatures of thin accretion disks around rotating black holes embedded in dark matter halos","authors":"Jia-Ying Zhang,&nbsp;Wei-Lun Tong,&nbsp;Tian-Yun Ye,&nbsp;Yong-You Liu,&nbsp;Zhen Li","doi":"10.1140/epjc/s10052-026-16569-0","DOIUrl":"10.1140/epjc/s10052-026-16569-0","url":null,"abstract":"<div><p>Black holes embedded in a dark matter background represent an important candidate model that extends the standard vacuum case, characterizing the strong gravitational environments at galactic centers and the gravitational influence of dark matter. This study focuses on dark matter halo-modified Kerr black holes and systematically investigates the observational characteristics of their surrounding thin accretion disks. Starting from static black hole solutions with dark matter halos, we employ the Newman–Janis algorithm to construct its rotating counterpart. The dark matter halo is modeled by a general double power-law density profile, whose integrated mass <span>(M_D(r))</span> modifies the radial mass function of Kerr metric to <span>(m(r) = M + M_D(r))</span>. Based on this spacetime, we analyze the observational properties of their thin accretion disk, including the radiative flux, temperature, differential luminosity, and spectral luminosity as a function of radius, with respect to the black hole spin and dark matter halo parameters. Furthermore, by combining ray-tracing methods, we simulate the bolometric image of the thin accretion disk under different black hole spins, dark matter halo parameters, and viewing inclinations. The dark matter halo enhances the gravitational potential, shifting the event horizon, innermost stable circular orbit, and photon shell outward, suppressing the peak radiative flux, and producing a fainter image, thereby generating signatures that are possibly observational distinguishable from standard vacuum Kerr black holes.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16569-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338462","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Silent coverage failures in rare-event searches and a degeneracy index that predicts them","authors":"Davide Pagano","doi":"10.1140/epjc/s10052-026-16570-7","DOIUrl":"10.1140/epjc/s10052-026-16570-7","url":null,"abstract":"<div><p>Searches for new physics in low-background experiments infer a non-negative signal strength from few events and often report an upper limit. Nominal frequentist coverage requires both a valid interval construction and an adequate data model. We study how controlled model departures affect lower- and upper-endpoint coverage for six interval procedures in an exact Poisson counting experiment, dark-matter recoil spectra, and a neutrinoless-double-beta-decay peak search. We introduce the Poisson–Fisher degeneracy index <span>(mathcal I_{textrm{PF}}(delta nu ;vartheta _0)=(beta ,gamma ))</span>, which maps a specified expected-count deformation, after projection onto the complete fitted tangent space, to <span>(beta )</span>, the signed fitted signal shift in profiled standard-error units, and <span>(gamma )</span>, the Poisson–Fisher norm of the unabsorbed residual. Locally, the sign of <span>(beta )</span> identifies the threatened endpoint, while <span>(gamma )</span> provides a local indication of detectability by the saturated-Poisson goodness-of-fit test used here at a <span>(5%)</span> nominal type-I error rate. Across the studied deformations, positive signal-like bias degrades discovery-side coverage while making upper limits conservative; negative signal bias from overestimated signal efficiency can make the upper endpoint undercover. Calibration under the nominal simulator does not protect against misspecification of that simulator relative to the data-generating process. A plausible deformation with large <span>(|beta |)</span> and small <span>(gamma )</span> may therefore evade diagnosis and should be represented by a nuisance constrained with auxiliary information or included in a defensible envelope. In the exactly collinear constrained-nuisance benchmark, modelling the deformation restores coverage at the evaluated grid points, at a quantifiable cost in interval sensitivity.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16570-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338465","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Holonomies and boundary symmetries in discrete Jackiw–Teitelboim gravity","authors":"H. T. Özer,&nbsp;Aytül Filiz","doi":"10.1140/epjc/s10052-026-16522-1","DOIUrl":"10.1140/epjc/s10052-026-16522-1","url":null,"abstract":"<div><p>We develop a fully discrete and non-perturbative realization of two-dimensional Jackiw–Teitelboim (JT) gravity as an <span>({textrm{sl}}(2,{mathbb {R}}))</span> BF theory. Using group-valued holonomies and Lie-algebra-valued dilatons, the bulk theory is shown to be purely topological, with all physical information encoded at the boundary. We analyze admissible discrete boundary conditions and derive the corresponding asymptotic symmetry algebras directly at the lattice level, including an affine Kac–Moody symmetry and its Brown–Henneaux reduction to a Virasoro algebra, together with the associated Virasoro–dilaton structure. A precise operator product expansion (OPE) dictionary is established by taking the controlled continuum limit of the discrete Poisson brackets. Beyond asymptotic symmetries, we provide an effective boundary description and a representation-theoretic quantization organized by monodromy sectors. Within this discrete framework, black hole entropy follows from gauge-invariant holonomy data and is expressed in terms of the dilaton Casimir, reproducing the Bekenstein–Hawking result within a framework that does not require an explicit Schwarzian action.\u0000\u0000\u0000\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16522-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338909","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Magnetic pressure anisotropy in ultra-dense white dwarfs: Landau quantization and neutronization effects","authors":"Edson Otoniel,&nbsp;Juan M. Z. Pretel,&nbsp;Victor B. T. Alves,&nbsp;César O. V. Flores,&nbsp;Clésio E. Mota","doi":"10.1140/epjc/s10052-026-16568-1","DOIUrl":"10.1140/epjc/s10052-026-16568-1","url":null,"abstract":"<div><p>Strong magnetic fields modify the thermodynamics of white dwarf (WD) matter by quantizing the transverse motion of degenerate electrons into Landau levels and splitting the pressure into components parallel and perpendicular to the magnetic field. We investigate how this microscopic pressure anisotropy affects ultra-dense WD sequences when Coulomb lattice contributions, electron capture thresholds, neutron drip limits, and nuclear composition are treated consistently in the equation of state (EoS). The stellar equilibrium structure is obtained by solving an anisotropic extension of the Tolman–Oppenheimer–Volkoff (TOV) equations, where <span>(P_r = P_parallel )</span> and <span>(P_t = P_perp )</span> denote the radial and tangential pressures, respectively. We compare the post-electron-capture branches with their corresponding pre-capture sequences for pure <span>(^{12}textrm{C})</span>, <span>(^{16}textrm{O})</span>, <span>(^{20}textrm{Ne})</span>, and <span>(^{24}textrm{Mg})</span> compositions, as well as for fixed 50/50 C/O, Ne/O, and Mg/Ne mixtures. The EoS predicts <span>(P_perp &lt; P_parallel )</span> in density ranges where only a few Landau levels are occupied. Consequently, pressure anisotropy shifts the stellar sequences toward smaller radii, with only minor changes in the maximum masses. We also find that post-capture configurations cannot be interpreted from the mass–radius plane alone, since the corresponding <span>(M(rho _c))</span> curves reveal portions with <span>(dM/drho _c&lt;0)</span> that are flagged by the turning-point diagnostic after the maximum mass is reached. Our results show that strong magnetic fields significantly reduce the radii of low-mass WDs, placing the calculated branches in the same broad mass–radius domain as a selected observational sample, without constituting a specific observational identification or statistical validation, and suggesting that future high-precision observations of massive magnetic WDs could help assess the role of magnetic pressure anisotropy in determining their masses and radii.\u0000\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16568-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149339046","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Stationary solutions in the small-c expansion of GR","authors":"Enes Bal,&nbsp;Ertuğrul Ekiz,&nbsp;Emre Onur Kahya,&nbsp;Utku Zorba","doi":"10.1140/epjc/s10052-026-16509-y","DOIUrl":"10.1140/epjc/s10052-026-16509-y","url":null,"abstract":"<div><p>We study the small-<i>c</i> expansion of general relativity in ADM variables up to next-to-next-to-leading order (NNLO). We show that, in the stationary sector, this formulation renders the field equations more tractable for explicit solution building. The stationary equations acquire a structure, in which the leading lapse and spatial metric are determined by a closed subsystem, the NLO rotational field satisfies a linear equation on that background, and the NNLO fields satisfy a linear system sourced by the NLO data. The stationary sector exhibits both strong-gravity and weak-field branches, whose structure becomes richer at NNLO. In the strong-gravity branch, we first obtain exact vacuum solutions of NLO Carroll gravity, including the Lense–Thirring and rotating C-metric backgrounds. At NNLO, we then construct the corresponding Lense–Thirring-type and C-metric-type exact vacuum geometries. These solutions also arise from the small-<i>c</i> expansion of the Kerr and rotating C-metric geometries around the strong-gravity background, up to <span>(mathcal {O}(J))</span> at NLO and up to <span>(mathcal {O}(J^3))</span> at NNLO. In the weak-field branch, we find exact Hartle–Thorne-type solutions with an independent quadrupole moment, together with exact spin-squared corrections and a mixed quadrupolar-rotating solution. We further extend the <span>(ell =0,2)</span> sector by including higher multipoles up to <span>(ell =4)</span>, where <span>(ell )</span> denotes the multipole index. These results show that the full NLO/NNLO theory admits a richer stationary vacuum sector than the magnetic Carroll truncation. More broadly, the ADM formulation provides a practical framework for constructing and analyzing stationary backgrounds in the small-<i>c</i> expansion of general relativity, and may also offer a useful framework for organizing rotational and higher-multipole deformations motivated by relativistic compact-object geometries.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16509-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338912","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Effective reheating in Gauss–Bonnet inflation with (mu (phi ,X)) coupling","authors":"Ali Seidabadi,&nbsp;Sara Saghafi,&nbsp;Kourosh Nozari","doi":"10.1140/epjc/s10052-026-16525-y","DOIUrl":"10.1140/epjc/s10052-026-16525-y","url":null,"abstract":"<div><p>We study effective reheating in a scalar–Gauss–Bonnet inflationary model with a phase-space-dependent coupling <span>(mu (phi ,X),)</span> in which a compact field-space feature is combined with a bounded kinetic gate. The modified inflationary background determines the pivot-scale quantities and the effective energy density at the end of inflation. These quantities are then used to derive the reheating duration <span>(N_{textrm{re}})</span> and temperature <span>(T_{textrm{re}})</span> through the thermal-history matching relation. We first perform two fixed-pivot reference scans by varying the overall Gauss–Bonnet strength <span>(lambda _{textrm{GB}})</span> and the kinetic-gate amplitude <span>(g_{_X})</span> separately. For the reference parameter choices, increasing either parameter increases <span>(N_{textrm{re}})</span> and decreases <span>(T_{textrm{re}})</span> for the selected reheating equations of state. Additional benchmark calculations clarify how these variations depend on the dynamical regime of the model. In the <span>(lambda _{textrm{GB}})</span> scan, the increase in <span>(N_{textrm{re}})</span> and the decrease in <span>(T_{textrm{re}})</span> persist, although both variations become strongly suppressed when the coupling is more localized or when the end of inflation is controlled more strongly by the E-model potential. In the <span>(g_{_X})</span> scan, stronger field-space localization and kinetic saturation can instead lead to a slight decrease in <span>(N_{textrm{re}})</span> and an increase in <span>(T_{textrm{re}})</span> as <span>(g_{_X})</span> is increased. When the bounded kinetic contribution is considered together with a weaker overall Gauss–Bonnet interaction, the resulting changes in the reheating quantities become nearly negligible. The fixed-pivot predictions of the representative and alternative benchmarks are compared with CMB constraints. These reheating constraints are then discussed for four representative values of the effective equation-of-state parameter, <span>(overline{w}_{textrm{re}}=-1/3,0,2/3,)</span> and 1. Finally, the analysis is generalized to a time-dependent reheating equation of state <span>(w_{textrm{re}}(N),)</span> showing that the thermal-history matching relations depend only on its e-fold average <span>(overline{w}_{textrm{re}},)</span> while the detailed evolution of <span>(w_{textrm{re}}(N))</span> remains degenerate within the effective framework adopted here.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16525-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338466","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tests of general relativity in pseudo-Newtonian approach","authors":"Naman Goyal,&nbsp;Banibrata Mukhopadhyay,&nbsp;Ashish Kumar Meena","doi":"10.1140/epjc/s10052-026-16547-6","DOIUrl":"10.1140/epjc/s10052-026-16547-6","url":null,"abstract":"<div><p>We investigate the extent to which pseudo-Newtonian gravitational potentials can reproduce classic tests of general relativity without resorting to full general relativistic formalisms. This is useful for the researchers seeking intuitive insight into relativistic gravity. Focusing on the perihelion precession of Mercury, gravitational redshift, and gravitational light bending, we derive analytical expressions for orbital precession and demonstrate that, with suitable physically acceptable parameters, pseudo-Newtonian approaches can accurately reproduce the observed perihelion advance and gravitational redshift. However, we confirm that no single potential consistently captures all relativistic effects. In particular, while certain parameters yield agreement with general relativity for planetary motion and redshift, they fail to reproduce gravitational lensing over a broad range of impact parameters. Our results highlight both the usefulness and limitations of pseudo-Newtonian methods in modeling gravitational phenomena. Although the pseudo-Newtonian approach cannot serve as universal substitutes for general relativity, especially in strong-field regimes, it provides valuable semi-analytical insight and pedagogical simplicity. Our results indicate the usefulness of the pseudo-Newtonian approach to uncover more complicated phenomena involved with strong field gravity in possibly modification to general relativity.\u0000</p></div>","PeriodicalId":788,"journal":{"name":"The European Physical Journal C","volume":"86 11","pages":""},"PeriodicalIF":4.9,"publicationDate":"2026-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1140/epjc/s10052-026-16547-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149338906","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}