Physics of the Dark Universe最新文献

{"title":"The impact on non-Gaussianities of the ISW-Lensing correlation in non-standard cosmologies","authors":"Matteo Forconi ,&nbsp;Alessandro Melchiorri","doi":"10.1016/j.dark.2025.102126","DOIUrl":"10.1016/j.dark.2025.102126","url":null,"abstract":"<div><div>The detection of non-Gaussianities (NG) in the Cosmic Microwave Background (CMB) is essential to better understand the early epochs of our Universe. One way to observe NG is to constrain the bispectrum, which usually is the largest non-trivial correlation function for most of the inflationary models. However, natural NG arise from late-time evolution and they need to be subtracted from the signal. In this work, we investigate the impact of different dark energy models to the bias induced by the cross-correlation between the Integrated Sachs–Wolfe effect and the weak lensing. More specifically, we compute the predictions for models of dynamical dark energy, <span><math><mrow><mi>w</mi><mo>≠</mo><mo>−</mo><mn>1</mn></mrow></math></span> and CPL parametrization, as well as different realizations of the sign-switching cosmological constant model.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102126"},"PeriodicalIF":6.4,"publicationDate":"2025-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266299","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Chaotic dynamics of string around a charged Kalb–Ramond black hole with Lorentz symmetry breaking","authors":"Anum Fayyaz ,&nbsp;G. Abbas ,&nbsp;Awatef Abidi ,&nbsp;Arafa A. Yagob","doi":"10.1016/j.dark.2025.102125","DOIUrl":"10.1016/j.dark.2025.102125","url":null,"abstract":"<div><div>The dynamics of a relativistic string close to a charged Kalb-Ramond black hole’s boundary is examined in this article. We show that the development of the string is extremely chaotic and often surpasses the Maldacena–Shenker–Stanford constraint, using the Lyapunov exponent as a diagnostic instrument. Our study also shows that the string’s energy and rotational momentum are crucial in determining its dynamic properties. By increasing the Lorentz symmetry-breaking parameter, the event horizon radius decreases, while the surface gravity increases. Furthermore, when all other parameters are fixed and the angular momentum <span><math><mi>L</mi></math></span> is varied, it is observed that for inner points, increasing <span><math><mi>L</mi></math></span> leads to a decrease in the values of <span><math><mrow><msup><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>−</mo><msup><mrow><mi>κ</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> , whereas for outer points, increasing <span><math><mi>L</mi></math></span> results in an increase in <span><math><mrow><msup><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>−</mo><msup><mrow><mi>κ</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> . Similarly, when <span><math><mi>L</mi></math></span> and other parameters are kept constant and the energy <span><math><mi>E</mi></math></span> is varied, the behavior differs: for inner points, increasing <span><math><mi>E</mi></math></span> causes <span><math><mrow><msup><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>−</mo><msup><mrow><mi>κ</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> to rise, indicating stronger chaotic behavior; in contrast, for outer points, increasing <span><math><mi>E</mi></math></span> leads to a decrease in <span><math><mrow><msup><mrow><mi>λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>−</mo><msup><mrow><mi>κ</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> , suggesting a tendency toward satisfying the Maldacena–Shenker–Stanford bound. Furthermore, we find that a higher energy in the case of outer points suppresses chaotic behavior, as evidenced by a decreasing Lyapunov exponent. These findings contribute to a deeper understanding of chaotic geodesics and the role of Lorentz-symmetry violation in modified gravity frameworks.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102125"},"PeriodicalIF":6.4,"publicationDate":"2025-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Impact of dynamical dark energy on black hole dynamics in an accelerated expanding universe","authors":"Debasis Sahu ,&nbsp;Bibekananda Nayak ,&nbsp;Lambodar Prasad Singh","doi":"10.1016/j.dark.2025.102117","DOIUrl":"10.1016/j.dark.2025.102117","url":null,"abstract":"<div><div>In this work, an interacting dark energy model is introduced for explaining the dynamical behaviour of our universe, where dark energy is evolved through continuous interaction with matter. Basing on this model, we have first computed the basic parameters like the density of dark energy, which is further utilized to illustrate the universe’s expansion dynamics. Our study suggests that the interacting nature of dark energy is sufficient to explain the observed accelerated expansion of present universe, if it is quintessence type. While the equation of state parameter (<span><math><msub><mrow><mi>γ</mi></mrow><mrow><mi>ϕ</mi></mrow></msub></math></span>) for quintessence ranges between 0 and <span><math><mrow><mo>−</mo><mn>1</mn></mrow></math></span>, our analysis predicts that accelerating nature of universe’s expansion can only occur, if the present value of <span><math><msub><mrow><mi>γ</mi></mrow><mrow><mi>ϕ</mi></mrow></msub></math></span> is less (more negative) than <span><math><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>7866</mn></mrow></math></span>. It is also concluded that the universe’s expansion would undergo a decelerating phase in the early epoch and would shift to accelerated expansion, around <span><math><mrow><mn>0</mn><mo>.</mo><mn>655</mn><msub><mrow><mi>t</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow></math></span>, with <span><math><msub><mrow><mi>t</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> representing the current age of our universe. Further, our model indicates that the accelerated expanding phase will continue for ever. Our focus also attributes to the mass evolution of Schwarzschild type black hole. In this context we consider the accumulation of energy-matter and the quantum mechanical Hawking evaporation as the active ingredients for evolution of black holes’ mass and found that accretion efficiency (<span><math><mi>f</mi></math></span>) creates different patterns of mass variations. Again, we have taken a look on the astrophysical constraints that affected the abundance of black holes and found that with increasing accretion efficiency, limits imposed on the black holes’ initial mass fraction would become more tightened.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102117"},"PeriodicalIF":6.4,"publicationDate":"2025-10-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266301","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Rotating Yukawa-modified black holes: QNM and shadow studies","authors":"Muhammad Zahid ,&nbsp;Chao Shen ,&nbsp;Javlon Rayimbaev ,&nbsp;Bekzod Rahmatov ,&nbsp;Inomjon Ibragimov ,&nbsp;Sokhibjan Muminov ,&nbsp;Maksud Umaraliyev","doi":"10.1016/j.dark.2025.102124","DOIUrl":"10.1016/j.dark.2025.102124","url":null,"abstract":"<div><div>This study investigates the quasinormal modes (QNMs) and shadows of rotating black holes (BHs) with a Yukawa-type scalar field in Modified Gravity (MOG), also known as scalar-tensor-vector gravity (STVG), providing tests using data from Event Horizon Telescope (EHT) observations. The metric incorporates Yukawa-like corrections to the gravitational potential in MOG, characterized by parameters <span><math><mi>α</mi></math></span> (MOG field strength) and <span><math><mi>β</mi></math></span> (Yukawa field exponent). We derive the corresponding rotating black hole solution, study the event horizon, ergoregion, static limit, and effective mass, analyzing their dependence on the black hole and gravity parameters. We calculated the photonsphere and shadow radii, and our analysis confirmed that increasing the black hole spin reduces the shadow size and increases the distortion. In contrast, the presence of MOG and Yukawa fields causes an increase in shadow size with constraints from EHT data on M87* and Sgr A*, yielding bounds like <span><math><mrow><mi>α</mi><mo>&lt;</mo><mn>0</mn><mo>.</mo><mn>5</mn></mrow></math></span> and <span><math><mrow><mi>β</mi><mo>≈</mo><mn>0</mn><mo>.</mo><mn>2</mn></mrow></math></span> at <span><math><mrow><mn>2</mn><mi>σ</mi></mrow></math></span> confidence for moderate spins. Furthermore, we study equatorial and polar QNMs using the geometric–optics correspondence between photon ring parameters and QNM frequencies, in order to assess the impact of the deformations. Energy emission rates via Hawking radiation are also studied, linking to the shadow radius. Results demonstrate deviations from Kerr, with EHT compatibility favoring small Yukawa and STVG modifications. These findings bridge theoretical predictions with observations, constraining alternative gravity models.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102124"},"PeriodicalIF":6.4,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266914","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cracking and overturning of Finch–Skea stellar objects obeying Karmarkar conditions in f(R,T) gravity","authors":"Adnan Malik ,&nbsp;Attiya Shafaq ,&nbsp;Shahid Chaudhary ,&nbsp;M. Zeeshan Gul ,&nbsp;Fatemah Mofarreh ,&nbsp;Muhammad Tahir Khan","doi":"10.1016/j.dark.2025.102114","DOIUrl":"10.1016/j.dark.2025.102114","url":null,"abstract":"<div><div>This work employs the cracking approach to analyze the implications of density fluctuations on anisotropic, spherically symmetric stellar models within <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. This analysis presents the field equations and derives a corresponding equation for the equilibrium state of anisotropic stellar configurations under <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. Further, we employed the Karmarkar conditions in conjunction with the Finch–Skea ansatz to solve corresponding equations. Additionally, we established a comprehensive framework for locating the cracking and overturning points by disrupting the configuration through local density fluctuation. The analytical framework to analyze the cracking has been deployed to the stars: SAXJ1808.4-3658, SMCX-1, 4U1538-52, EXO 1785-248, and 4U 1728-34 to assess the feasibility of the presented technique. This analysis concludes that cracking emerges in different regions of the above-mentioned stellar models. Significantly, this analysis provides notable insights into the structural dynamics of Finch–Skea stellar structures by locating the regions impacted by density disruptions, thus demonstrating the efficacy of the cracking approach.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102114"},"PeriodicalIF":6.4,"publicationDate":"2025-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266847","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Optical properties of black holes immersed in Galactic Dark Matter Halo","authors":"Aqsa Mehmood ,&nbsp;A. Eid ,&nbsp;M. Umair Shahzad ,&nbsp;Abdul Malik Sultan","doi":"10.1016/j.dark.2025.102115","DOIUrl":"10.1016/j.dark.2025.102115","url":null,"abstract":"<div><div>We present a comprehensive investigation into the optical and topological properties of black holes (BHs) immersed in a Galactic Dark Matter Halo (GDMH). Our analysis focuses on shadow morphology, photon ring luminosity, and thermodynamic classification, using spherically symmetric accretion models in both static and infalling frameworks. In both scenarios, we observe that the shadow radius decreases monotonically with increasing halo parameter (<span><math><mi>a</mi></math></span>), reflecting the influence of dark matter on photon trajectories. Within the static accretion model, the brightness of the photon ring intensifies significantly with increasing <span><math><mi>a</mi></math></span>, more prominently than with variations in the asymptotic circular velocity (<span><math><msub><mrow><mi>V</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>). BHs surrounded by radially infalling accretion flows exhibit darker shadows compared to those with static flows, a consequence of relativistic Doppler dimming; however, the shadow size remains invariant, reaffirming its geometric origin. We further analyze the visual manifestation and observational significance of these luminous features, including shadow contours and intensity profiles. Finally, using the generalized off-shell Helmholtz free energy framework, we classify the BH in GDMH as belonging to the <span><math><msup><mrow><mi>W</mi></mrow><mrow><mn>1</mn><mo>−</mo></mrow></msup></math></span> topological class, indicating a thermodynamically unstable configuration with a single negative winding number.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102115"},"PeriodicalIF":6.4,"publicationDate":"2025-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266915","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Exploring traversable wormholes in modified theory: Complexity and VIQ perspective under solitonic quantum wave dark matter halo","authors":"Tayyab Naseer ,&nbsp;M. Sharif ,&nbsp;Mona Faiza ,&nbsp;Fakhranda Afandi ,&nbsp;Mohamed R. Eid ,&nbsp;Abdel-Haleem Abdel-Aty","doi":"10.1016/j.dark.2025.102112","DOIUrl":"10.1016/j.dark.2025.102112","url":null,"abstract":"<div><div>The traversable wormholes are analyzed in this study, incorporating the quantum wave dark matter halo and the electromagnetic field, in the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. The wormhole model is built upon the Morris-Thorne geometry, and the corresponding motion equations are derived for an anisotropic fluid within a typical modified gravity framework. Our next step is to derive the shape functions by considering distinct redshift parameters. These two functions adhere to the required conditions, linking two asymptotically flat regions of spacetime. We then proceed to formulate a couple of solutions through the resulting shape functions and make sure that they are in accordance with the violation of null energy bounds. Moreover, we assess the complexity factor and active gravitational mass, studying the point or area on the manifold where they approach to zero. It is demonstrated that both these quantities gain negative values in particular spacetime areas. The study also looks into the physical properties of wormholes, paying attention to the volume integral quantifier and embedding diagrams. The conclusions point to the fact that the derived wormhole geometries fulfill the necessary requirements, enabling them to exist within the modified gravity framework under consideration.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102112"},"PeriodicalIF":6.4,"publicationDate":"2025-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266846","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Search for deexcitations of 178m2Hf isomer induced by inelastic Dark Matter candidates in ultra-low-background conditions","authors":"P. Belli ,&nbsp;R. Bernabei ,&nbsp;F. Cappella ,&nbsp;V. Caracciolo ,&nbsp;R. Cerulli ,&nbsp;F.A. Danevich ,&nbsp;S.S. Drapey ,&nbsp;A. Incicchitti ,&nbsp;S.I. Kirischuk ,&nbsp;V.I. Kirischuk ,&nbsp;M. Laubenstein ,&nbsp;A. Leoncini ,&nbsp;V.I. Tretyak","doi":"10.1016/j.dark.2025.102113","DOIUrl":"10.1016/j.dark.2025.102113","url":null,"abstract":"<div><div>The <span><math><mi>γ</mi></math></span>-ray radiation from a ^178m2Hf source with an activity of <span><math><mrow><mo>≈</mo><mn>63</mn></mrow></math></span> Bq was measured for the first time with two ultra-low-background HPGe <span><math><mi>γ</mi></math></span> spectrometers over cumulative 1170 h deep underground at the Gran Sasso National Laboratory (LNGS) of the INFN. The aim of the measurements was the search for deexcitations of the ^178m2Hf isomer induced by inelastic Dark Matter candidates. The process would lead to <span><math><mi>γ</mi></math></span>-ray emission from the excited levels of the ¹⁷⁸Hf that are not populated in the spontaneous decay of the ^178m2Hf. In this way improved limits on the half-life of eighteen inelastic-dark-matter-induced transitions, at the level of <span><math><mrow><mo>lim</mo><msub><mrow><mi>T</mi></mrow><mrow><mn>1</mn><mo>/</mo><mn>2</mn></mrow></msub><mo>∼</mo><mn>4</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>5</mn></mrow></msup><mtext>–</mtext><mn>6</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>6</mn></mrow></msup></mrow></math></span> yr are derived. The parameters’ space of such inelastic candidates is also derived for some given model assumptions. Elements towards progress in sensitivity are briefly mentioned.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102113"},"PeriodicalIF":6.4,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266916","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Lorentz-violating and topological effects on gravitational lensing phenomena and wave optics in wormhole backgrounds","authors":"Faizuddin Ahmed ,&nbsp;Abdelmalek Bouzenada","doi":"10.1016/j.dark.2025.102111","DOIUrl":"10.1016/j.dark.2025.102111","url":null,"abstract":"<div><div>In this paper, we present a comprehensive analysis of photon trajectories and electromagnetic wave propagation in Lorentz-violating wormhole (LVWH) spacetimes embedded with topological defects-specifically, a cosmic string (CS) and a global monopole. We begin by deriving the equations of motion for null geodesics and analyze the behavior of photon paths in relation to the wormhole throat radius and parameters characterizing Lorentz symmetry violation. An explicit expression for the photon deflection angle is obtained, which is then used to derive a lens equation. We show that both the cosmic string parameter and Lorentz-violating terms significantly modify this equation compared to the standard Ellis–Bronnikov–Morris–Thorne wormhole (EBMTWH) case. To go beyond the geometric optics approximation, we formulate the scalar Helmholtz wave equation in the curved LVWH background. The resulting effective potential governing wave propagation is shown to be strongly dependent on the throat size, cosmic string parameter, and Lorentz-violating contributions. This leads to a spatially varying refractive index, indicating substantial alterations in the optical properties of the spacetime due to these effects. We extend the analysis to a second LVWH scenario embedded with a global monopole charge. A parallel treatment reveals how the interplay between the monopole parameter, throat radius, and Lorentz-violating terms influences both the lens equation and wave propagation characteristics. Our results highlight how topological defects combined with Lorentz symmetry breaking lead to distinctive modifications in both ray and wave optics, offering potential observational signatures and deeper insights into exotic gravitational structures.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102111"},"PeriodicalIF":6.4,"publicationDate":"2025-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145266848","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Observational constraining on baryon to entropy ratios in modified theories of gravity","authors":"Abdulmohsen Daham Alruwaili ,&nbsp;Nadeem Azhar ,&nbsp;Abdul Jawad","doi":"10.1016/j.dark.2025.102103","DOIUrl":"10.1016/j.dark.2025.102103","url":null,"abstract":"<div><div>Baryogenesis, the generation of the cosmic matter-antimatter asymmetry, remains one of the profound questions in theoretical physics. This research explores the mechanisms of baryogenesis and extends the investigation to its more generalized theoretical frameworks within the context of squared energy–momentum theories, specifically <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><msup><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow></mrow></math></span>, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>G</mi><mo>,</mo><msup><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow></mrow></math></span> and <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><msup><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow></mrow></math></span>. These theories extend conventional general relativity by incorporating novel couplings between the trace of the energy–momentum squared tensor, <span><math><mrow><msup><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>≡</mo><msub><mrow><mi>T</mi></mrow><mrow><mi>μ</mi><mi>ν</mi></mrow></msub><msup><mrow><mi>T</mi></mrow><mrow><mi>μ</mi><mi>ν</mi></mrow></msup></mrow></math></span>, and fundamental geometric scalars: the Ricci scalar <span><math><mi>R</mi></math></span>, the Gauss–Bonnet invariant <span><math><mi>G</mi></math></span>, and the non-metricity scalar <span><math><mi>Q</mi></math></span>. We consider two generic models within each theory to explore their implications on the dynamical evolution of the early universe and their potential role in generating the observed baryon asymmetry. By analyzing the interplay between gravity and particle physics in the high-energy regime, we derive conditions under which baryogenesis can occur in each theory. Furthermore, by integrating the power law scale factor into our models, we examine its impact on the baryogenesis mechanism and resulting matter-antimatter asymmetry. Through detailed numerical simulations and analytical calculations, we assess the viability of each model in generating the observed baryon asymmetry, contributing to a deeper understanding of the connection between gravitational theories and fundamental processes in cosmology. These findings pave the way for future experimental tests and observational constraints on these theories.</div></div>","PeriodicalId":48774,"journal":{"name":"Physics of the Dark Universe","volume":"50 ","pages":"Article 102103"},"PeriodicalIF":6.4,"publicationDate":"2025-09-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145220738","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}