Journal of High Energy Astrophysics最新文献

{"title":"Antisymmetric tensor influence on charged black hole lensing phenomena and time delay","authors":"A.A. Araújo Filho","doi":"10.1016/j.jheap.2025.100401","DOIUrl":"10.1016/j.jheap.2025.100401","url":null,"abstract":"<div><div>In this work, we investigate the gravitational lensing of a charged black hole (spherically symmetric) within the context of Lorentz violation triggered by an antisymmetric tensor field. Our calculations consider two different scenarios: the weak and strong deflection limits. For the weak deflection limit, we employ the <em>Gauss–Bonnet</em> theorem to obtain our results. In the strong deflection limit, we utilize the <em>Tsukamoto</em> methodology, which provides measurable outcomes such as relativistic image positions and magnifications. Applying the latter methodology, we analyze the gravitational lensing by Sagittarius <span><math><msup><mrow><mi>A</mi></mrow><mrow><mo>⁎</mo></mrow></msup></math></span> and derive the related observables, which are expressed as functions of the Lorentz violation parameter. Finally, the time delay is addressed as well.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100401"},"PeriodicalIF":10.2,"publicationDate":"2025-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144139105","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Multi-wavelength analysis of FSRQ B2 1348+30B: Constraints on the jet power","authors":"Sajad Ahanger ,&nbsp;Sunder Sahayanathan ,&nbsp;Sitha K. Jagan ,&nbsp;Shah Zahir ,&nbsp;Naseer Iqbal","doi":"10.1016/j.jheap.2025.100400","DOIUrl":"10.1016/j.jheap.2025.100400","url":null,"abstract":"<div><div>We present 14.5-year multi-wavelength analysis of flat-spectrum radio quasar B2<!--> <!-->1348+30B using Swift-UVOT, Swift-XRT, and <em>Fermi</em>-LAT observations. In the <em>γ</em>-ray band, the 3<!--> <!-->day bin lightcurve reveals two major flaring events on 2010-09-19 (55458 MJD) and 2022-05-26 (59725 MJD) detected at flux levels <span><math><mo>(</mo><mn>2.5</mn><mo>±</mo><mn>0.5</mn><mo>)</mo><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup><mspace></mspace><mrow><mi>ph c</mi><msup><mrow><mi>m</mi></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup><mspace></mspace><msup><mrow><mi>s</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span> and <span><math><mo>(</mo><mn>5.2</mn><mo>±</mo><mn>0.6</mn><mo>)</mo><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup><mspace></mspace><mrow><mi>ph c</mi><msup><mrow><mi>m</mi></mrow><mrow><mo>−</mo><mn>2</mn></mrow></msup><mspace></mspace><msup><mrow><mi>s</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>. The Bayesian block analysis of the flares suggested the variability timescale to be ≤ 3<!--> <!-->day. To study the dynamic nature of the source, multi-wavelength spectrum was obtained for three flux states which includes the two flaring state and a relative low state. The <em>γ</em>-ray spectra of the source in all the states are well fitted by a power-law model with maximum photon energy &lt; 20 GeV. In X-ray, a power-law model can explain the flaring state spectra while a broken power-law with extremely hard high energy component was required to model the low flux state. This indicates the presence of the low energy cutoff in the Compton spectral component. A simple one-zone leptonic model involving synchrotron, synchrotron self Compton and external Compton mechanism can successfully reproduce the broad-band spectral energy distribution of all the flux states. The model parameters suggest significant increase in the jet Lorentz factor during the high flux states. Further, the best fit parameters are used to constrain the minimum energy of the emitting electron distribution from the hard high energy spectrum of the low flux state. This analysis was extended to draw limits on the kinetic power of the blazar jet and was compared with the Eddington luminosity of the central black hole.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100400"},"PeriodicalIF":10.2,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144146737","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Einstein-Gauss-Bonnet cosmology confronted with observations","authors":"Sergei D. Odintsov ,&nbsp;V.K. Oikonomou ,&nbsp;German S. Sharov","doi":"10.1016/j.jheap.2025.100398","DOIUrl":"10.1016/j.jheap.2025.100398","url":null,"abstract":"<div><div>Several models within the framework of Einstein-Gauss-Bonnet gravities are considered with regard their late-time phenomenological viability. The models contain a non-minimally coupled scalar field and satisfy a constraint on the scalar field Gauss-Bonnet coupling, that guarantees that the speed of the tensor perturbations is equal to the speed of light. The late-time cosmological evolution of these Einstein-Gauss-Bonnet models is confronted with the observational data including the Pantheon plus Type Ia supernovae catalogue, the Hubble parameter measurements (cosmic chronometers), data from cosmic microwave background radiation (CMB) and baryon acoustic oscillations (BAO) including the latest measurements from Dark Energy Spectroscopic Instrument (DESI). Among the considered class of models some of them do not fit the CMB and BAO data. However, there exists some models that generate a viable Einstein-Gauss-Bonnet scenario with well-behaved late-time cosmological evolution that fits the observational data essentially better in comparison to the standard Λ-Cold-Dark-Matter model.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100398"},"PeriodicalIF":10.2,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144089269","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Chasing super-horizon correlations: The promise of LiteBIRD polarization measurements","authors":"Francesca Di Nella,&nbsp;Alessandro Melchiorri","doi":"10.1016/j.jheap.2025.100399","DOIUrl":"10.1016/j.jheap.2025.100399","url":null,"abstract":"<div><div>It is well known that, since Cosmic Microwave Background (CMB) polarization originates at the surface of last scattering, scenarios in which perturbations are generated causally within the horizon cannot produce correlations at angular scales larger than about 2 degrees. In contrast, inflationary models predict a distinctive peak in the correlation functions at these large angular scales. By comparing the null hypothesis (no <em>TE</em> signal at large scales) with the ΛCDM prediction, we show that while Planck already provides strong statistical evidence for super-horizon perturbations, a future CMB satellite experiment as LiteBIRD will further reinforce this conclusion by improving current constraints by more than a factor of 3. We then consider an alternative explanation for the observed suppression of large-scale polarization: a low-<em>k</em> cutoff in the primordial power spectrum. We forecast the sensitivity of LiteBIRD to this cutoff scale, <span><math><msub><mrow><mi>k</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>. In particular, we find that LiteBIRD will improve the constraint on <span><math><msub><mrow><mi>k</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span> by a factor of 1.4, outperforming Planck. These results highlight the critical role of large-scale polarization in establishing the presence of super-horizon correlations and offer new avenues to probe deviations from a scale-invariant primordial spectrum.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100399"},"PeriodicalIF":10.2,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144084191","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Cosmological phase-space analysis of f(G)-theories of gravity","authors":"Giannis Papagiannopoulos ,&nbsp;Orlando Luongo ,&nbsp;Genly Leon ,&nbsp;Andronikos Paliathanasis","doi":"10.1016/j.jheap.2025.100397","DOIUrl":"10.1016/j.jheap.2025.100397","url":null,"abstract":"<div><div>The impact of topological terms that modify the Hilbert-Einstein action is here explored by virtue of a further <span><math><mi>f</mi><mo>(</mo><mi>G</mi><mo>)</mo></math></span> contribution. In particular, we investigate the phase-space stability and critical points of an equivalent scalar field representation that makes use of a massive field, whose potential is function of the topological correction. To do so, we introduce to the gravitational Action Integral a Lagrange multiplier and model the modified Friedmann equations by virtue of new non-dimensional variables. We single out dimensionless variables that permit <em>a priori</em> the Hubble rate change of sign, enabling regions in which the Hubble parameter either vanishes or becomes negative. In this respect, we thus analyze the various possibilities associated with a universe characterized by such topological contributions and find the attractors, saddle points and regions of stability, in general. The overall analysis is carried out considering the exponential potential first and then shifting to more complicated cases, where the underlying variables do not simplify. We compute the eigenvalues of our coupled differential equations and, accordingly, the stability of the system, in both a spatially-flat and non-flat universe. Quite remarkably, regardless of the spatial curvature, we show that a stable de Sitter-like phase that can model current time appears only a small fraction of the entire phase-space, suggesting that the model under exam is unlikely in describing the whole universe dynamics, i.e., the topological terms appear disfavored in framing the entire evolution of the universe.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100397"},"PeriodicalIF":10.2,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143918193","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Late-time constraints on dynamical dark energy models using DESI DR2, Type Ia supernova, and CC measurements","authors":"Ritika Nagpal ,&nbsp;Himanshu Chaudhary ,&nbsp;Harshita Gupta ,&nbsp;S.K.J. Pacif","doi":"10.1016/j.jheap.2025.100396","DOIUrl":"10.1016/j.jheap.2025.100396","url":null,"abstract":"<div><div>The ΛCDM model has successfully explained various cosmological phenomena, yet persistent discrepancies in the measured value of the Hubble constant (<span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>) known as the “<em>Hubble Tension</em>” challenge its completeness. Early Universe measurements from the cosmic microwave background (CMB) suggest <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>67.4</mn><mo>±</mo><mn>0.5</mn></math></span> km<!--> <!-->s⁻¹ <!-->Mpc⁻¹, whereas late-time measurements using the cosmic distance ladder yield <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>73.04</mn><mo>±</mo><mn>1.04</mn></math></span> km<!--> <!-->s⁻¹ <!-->Mpc⁻¹, resulting in a tension of 4<em>σ</em> to 5.7<em>σ</em>. To address this issue, researchers have proposed a range of alternative cosmological models in recent years. These models are based on dynamic dark energy scenarios featuring various parameterization schemes of the equation of state <span><math><mi>w</mi><mo>(</mo><mi>z</mi><mo>)</mo></math></span>. In this study, we investigate some well-known dark energy models employing both two-parameter and three-parameter parameterizations of the equation of state <span><math><mi>w</mi><mo>(</mo><mi>z</mi><mo>)</mo></math></span>. Using observational data from Cosmic Chronometers, Type Ia Supernovae, and Baryon Acoustic Oscillations (BAO) including the latest release from the Dark Energy Spectroscopic Instrument (DESI) Data Release 2 (DR2), we constrain key cosmological parameters such as the Hubble constant <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> and the sound horizon at the baryon drag epoch <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span>. We explore these parameterizations and their impact on the expansion history of the Universe, with particular emphasis on the late-time cosmic evolution. Our analysis employs Markov Chain Monte Carlo simulations and several statistical tests to estimate parameter values, evaluate model performance, and assess deviations from the ΛCDM model.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100396"},"PeriodicalIF":10.2,"publicationDate":"2025-05-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143913037","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"The role of saturated thermal conduction in shaping electric current dynamics in jet-launching disks","authors":"Ghassen Rezgui ,&nbsp;Reinhold Preiner","doi":"10.1016/j.jheap.2025.100394","DOIUrl":"10.1016/j.jheap.2025.100394","url":null,"abstract":"<div><div>This study investigates the dynamics of jet formation from a viscous, resistive accretion disk around a young stellar object using MHD simulations with the PLUTO code. We conducted an in-depth analysis of electric currents from various perspectives to elucidate how their dynamics, influenced by saturated thermal conduction, impact jet acceleration and collimation processes. Our simulations confirm the butterfly topology of electric current lines, as predicted by earlier analytic models. Crucially, increasing the saturation parameter <span><math><msub><mrow><mi>ϕ</mi></mrow><mrow><mi>s</mi></mrow></msub></math></span> alters the current line topology: higher saturation enhances collimation in the inner disk regions while inducing decollimation in the outer regions. By the end of our simulations (<span><math><mi>t</mi><mo>=</mo><mn>700</mn></math></span>, ∼112 rotational periods), higher <span><math><msub><mrow><mi>ϕ</mi></mrow><mrow><mi>s</mi></mrow></msub></math></span> results in a faster and more collimated jet compared to its lower <span><math><msub><mrow><mi>ϕ</mi></mrow><mrow><mi>s</mi></mrow></msub></math></span> counterpart, whereas at earlier times (<span><math><mi>t</mi><mo>=</mo><mn>200</mn></math></span>, ∼32 rotational periods), the jet exhibits lower acceleration despite enhanced collimation. In our reference case, we find that the electric current lines connect the launching region to the Alfvén and fast magnetosonic surfaces from early times, confirming the effectiveness of the acceleration mechanism at the onset of jet formation. Our study reveals that the upper jet regions are transitioning toward Kelvin–Helmholtz instability (KHI), while the jet base continues to exhibit wave activity. At <span><math><mi>t</mi><mo>=</mo><mn>700</mn></math></span>, doubling the saturation parameter reduces these oscillations and suppresses KHI, indicating faster plasma propagation. Analysis of the vertical profile of the current density, <span><math><msub><mrow><mi>J</mi></mrow><mrow><mi>z</mi></mrow></msub></math></span>, shows a clear correlation between increased saturation and both enhanced jet acceleration and current density. Furthermore, the ratio of electric currents at the Alfvén point, <span><math><msub><mrow><mi>I</mi></mrow><mrow><mi>A</mi></mrow></msub></math></span>, and sub-magnetosonic point, <span><math><msub><mrow><mi>I</mi></mrow><mrow><mi>s</mi><mi>m</mi></mrow></msub></math></span>, indicates that higher saturation significantly improves the efficiency of matter propulsion and energy transfer within the jet.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100394"},"PeriodicalIF":10.2,"publicationDate":"2025-05-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143913036","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Numerical studies of (in)stabilities of shocks in perturbed advective flows around black holes","authors":"Junxing Zhou ,&nbsp;Junxiang Huang ,&nbsp;Xin Chang ,&nbsp;Toru Okuda ,&nbsp;Chandra B. Singh","doi":"10.1016/j.jheap.2025.100395","DOIUrl":"10.1016/j.jheap.2025.100395","url":null,"abstract":"<div><div>Using two-dimensional hydrodynamic simulations, we investigate the stability of shocked accretion flows around black holes under non-axisymmetric perturbations. By systematically exploring the parameter space of specific energy and angular momentum that permits shock formation in advective accretion flows, we demonstrate that quasi-periodic oscillations (QPOs) naturally emerge in perturbed systems. Our spectral analysis reveals characteristic QPO frequencies spanning 0.44-146.57<em>Hz</em>, effectively bridging the observed low-frequency (LFQPOs) and high-frequency QPOs (HFQPOs) in black hole X-ray binaries. The quality factors (<span><math><mi>Q</mi><mo>=</mo><msub><mrow><mi>μ</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>/</mo><mn>2</mn><mi>Δ</mi></math></span>) of these oscillations range from 1.66 to 203.58, with multiple Lorentzian components indicating distinct oscillation modes. Through wavelet analysis and cross-validation with recent observations (e.g., Swift J1727.8-1613 and GX 339-4), we establish that shock instabilities driven by acoustic wave interactions between the non-axisymmetric perturbation and the shock location can quantitatively explain the temporal features observed in accreting black hole systems. Furthermore, we characterize the <em>γ</em>-dependence of shock morphology, showing that increasing the adiabatic index from 4/3 to 1.4 changes shock positions outward while maintaining oscillation coherence.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100395"},"PeriodicalIF":10.2,"publicationDate":"2025-05-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143903721","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"An explanation for the radio variation associated with the Vela pulsar glitch occurred on December 12 2016","authors":"Shuang Du","doi":"10.1016/j.jheap.2025.100393","DOIUrl":"10.1016/j.jheap.2025.100393","url":null,"abstract":"<div><div>The elaborate observation of the single radio pulses of Vela pulsar around the pulsar glitch that occurred on December 12, 2016 reveals that the physical mechanism associated with this glitch exerts a profound influence on the pulsar's magnetosphere. According to the evolution of these pulses, we propose a scenario regarding how the pulsar magnetic field might undergo alterations within the framework of the inner gap model. We deduce that the liberation of the free energy within Vela pulsar results in the emergence of new magnetic multipole components. The progressively developing multipole components cause the magnetic field lines in a section of the polar cap region to become increasingly curved, ultimately resulting in the observed pulse broadening and pulse missing. At last, we discuss the possible connection between magnetic variations and fast radio bursts according to the inspiration of the presented picture.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100393"},"PeriodicalIF":10.2,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143882927","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Black holes immersed in polytropic scalar field gas","authors":"Y. Sekhmani ,&nbsp;S. Zare ,&nbsp;L.M. Nieto ,&nbsp;H. Hassanabadi ,&nbsp;K. Boshkayev","doi":"10.1016/j.jheap.2025.100389","DOIUrl":"10.1016/j.jheap.2025.100389","url":null,"abstract":"<div><div>By implementing the concept of polytropic structures as a scalar field gas with a dark energy-like behavior, we obtain a static spherically symmetric black hole solution in the framework of general relativity. In this paper, we study the quasinormal modes, the greybody bound process, the shadow behaviors, and the sparsity of black holes with a surrounding polytropic scalar field gas. Using the Wentzel-Kramers-Brillouin (WKB) approach, we evaluate the impact of a particular set of polytropic parameters <span><math><mo>(</mo><mi>ξ</mi><mo>,</mo><mi>A</mi><mo>)</mo></math></span> with a fixed setting of the polytropic index <em>n</em> on the oscillation frequency and damping rate of gravitational waves. The results show that the effect of the parameter <em>ξ</em> is much less significant than that of the parameter <em>A</em> on the gravitational waves oscillation frequency and damping rate. Furthermore, the analysis of the greybody factor bounds reveals special insight into the effect of certain parameters where the multipole moments <em>l</em> and the polytropic index <em>n</em> have similar effects, in contrast to the pair of polytropic parameters (<span><math><mi>ξ</mi><mo>,</mo><mi>A</mi></math></span>). In light of such a comparative study, we investigate, on the other hand, the third-order Padé WKB method, which results in a more accurate process for quasinormal mode frequencies compared to the third-order standard WKB method. In this way, exploring the sparsity of Hawking radiation is another task that provides a better understanding of the behavior of the black hole solution. In this respect, the results show that the black hole behaves like blackbody radiation for a sufficiently large entropy. And for <span><math><mi>ξ</mi><mo>=</mo><mi>A</mi><mo>=</mo><mn>0</mn></math></span>, the relevant sparsity acts exactly like the Schwarzschild sparsity. These results provide an insight into the dynamics of black holes with a surrounding polytropic scalar field gas from the analysis of their quasinormal modes, greybody factors, shadow behaviors, energy emission rate and sparsity process. Constraints on the associated BH parameters, derived from the Event Horizon Telescope observations of M87* and Sgr A*, indicate that this black hole model stands as a compelling candidate for representing astrophysical black holes.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"47 ","pages":"Article 100389"},"PeriodicalIF":10.2,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143865168","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}