Journal of High Energy Astrophysics最新文献

{"title":"Exploring embedded wormhole solutions and thermodynamics in extended teleparallel gravity","authors":"Allah Ditta ,&nbsp;G. Mustafa ,&nbsp;Asif Mahmood","doi":"10.1016/j.jheap.2025.01.006","DOIUrl":"10.1016/j.jheap.2025.01.006","url":null,"abstract":"<div><div>This work investigates the wormhole thermodynamics in teleparallel Rastall gravity using the Karmarkar condition. We apply the first law of wormhole thermodynamics to evaluate the total energy of the wormhole system. In addition, we analyze the stability and equilibrium and thermal stability by investigating the thermodynamic features of wormholes, such as Hawking temperature, wormhole temperature, average wormhole pressure, work energy, total energy, energy flux, and specific heat. We conclude that all the thermodynamic features ensure the thermal stability and equilibrium of the wormhole.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 350-358"},"PeriodicalIF":10.2,"publicationDate":"2025-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102771","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":"NuSTAR view of the X-ray transients Swift J174805.3-244637 and IGR J17511-3057","authors":"Aditya S. Mondal ,&nbsp;Mahasweta Bhattacharya ,&nbsp;Mayukh Pahari ,&nbsp;Biplab Raychaudhuri ,&nbsp;Rohit Ghosh ,&nbsp;Gulab C. Dewangan","doi":"10.1016/j.jheap.2025.01.005","DOIUrl":"10.1016/j.jheap.2025.01.005","url":null,"abstract":"<div><div>We report on the <em>NuSTAR</em> observations of the neutron star low-mass X-ray binary Swift J174805.3-244637 (hereafter Swift J17480) and the accreting millisecond X-ray pulsar IGR J17511-3057 performed on March 4, 2023, and April 8, 2015, respectively. We describe the continuum emission of Swift J17480 with a combination of two soft thermal components and an additional hard X-ray emission described by a power-law. We suggest that the spectral properties of Swift J17480 are consistent with a soft spectral state. The source IGR J17511-3057 exhibits a hard spectrum characterized by a Comptonized emission from the corona. The X-ray spectrum of both sources shows evidence of disc reflection. For the first time, we employ the self-consistent reflection models (<span>relxill</span> and <span>relxillNS</span>) to fit the reflection features in the <em>NuSTAR</em> spectrum. From the best-fit spectral model, we find an inner disc radius (<span><math><msub><mrow><mi>R</mi></mrow><mrow><mi>i</mi><mi>n</mi></mrow></msub></math></span>) is precisely constrained to <span><math><mo>(</mo><mn>1.99</mn><mo>−</mo><mn>2.68</mn><mo>)</mo><mspace></mspace><msub><mrow><mi>R</mi></mrow><mrow><mi>I</mi><mi>S</mi><mi>C</mi><mi>O</mi></mrow></msub></math></span> and inclination to <span><math><mn>30</mn><mo>±</mo><mn>1</mn><mi>°</mi></math></span> for Swift J17480. We determine an inner disc radius of <span><math><mo>≲</mo><mn>1.3</mn><mspace></mspace><msub><mrow><mi>R</mi></mrow><mrow><mi>I</mi><mi>S</mi><mi>C</mi><mi>O</mi></mrow></msub></math></span> and inclination of <span><math><mn>44</mn><mo>±</mo><mn>3</mn><mi>°</mi></math></span> for IGR J17511-3057. A low inclination angle of the system is required for both sources. For the source IGR J17511-3057, spinning at 4.1 ms, the value of co-rotation radius (<span><math><msub><mrow><mi>R</mi></mrow><mrow><mi>c</mi><mi>o</mi></mrow></msub></math></span>) is estimated to be ∼42 km (<span><math><mn>3.6</mn><mspace></mspace><msub><mrow><mi>R</mi></mrow><mrow><mi>I</mi><mi>S</mi><mi>C</mi><mi>O</mi></mrow></msub><mo>)</mo></math></span>, consistent with the position of inner disc radius as <span><math><msub><mrow><mi>R</mi></mrow><mrow><mi>i</mi><mi>n</mi></mrow></msub><mo>≲</mo><msub><mrow><mi>R</mi></mrow><mrow><mi>c</mi><mi>o</mi></mrow></msub></math></span>. We further place an upper limit on the magnetic field strength of the sources, considering the disc is truncated at the magnetospheric radius.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 359-370"},"PeriodicalIF":10.2,"publicationDate":"2025-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102772","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":"Exploring temperature influences on gravitational wave production in binary white dwarfs","authors":"Sílvia P. Nunes ,&nbsp;José D.V. Arbañil ,&nbsp;César H. Lenzi ,&nbsp;Jaziel G. Coelho","doi":"10.1016/j.jheap.2025.01.004","DOIUrl":"10.1016/j.jheap.2025.01.004","url":null,"abstract":"<div><div>This study investigates the conditions under which gravitational waves (GWs) are emitted during the merger of hot white dwarfs (WDs) in a binary system. Traditionally, these systems consist of two low-mass stars or a more massive WD paired with a less massive companion. In addition, recent work has investigated the possibility that double white dwarf (DWD) mergers are possibly the leading formation channel of massive, rapidly rotating, high-field magnetic WDs, particularly SDSS J221141.80 + 113604.4 (hereafter J2211+1136) and ZTF J190132.9 + 145808.7 (hereafter J1901 + 14588). Motivated by these findings and the Laser Interferometer Space Antenna (LISA) prospects, this study aims to calculate the tidal Love number, the dimensionless tidal deformability, as well as the frequency and amplitude of GWs of hot WDs. The results indicate that the tidal deformability is more pronounced in stars with higher central temperatures and lower masses, which would lead to reduced emission of GWs. In contrast, more massive stars exhibit less deformability, making them prime candidates for generating stronger GWs. Additionally, the analysis of frequency and amplitude reveals that the frequencies of high-mass binaries are smaller and evolve more rapidly, reaching a limit that aligns with the operational detection capabilities of LISA during its initial phase.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 333-339"},"PeriodicalIF":10.2,"publicationDate":"2025-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102769","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":"A possible jet and corona configuration for Swift J1727.8–1613 during the hard state","authors":"Jing-Qiang Peng ,&nbsp;Shu Zhang ,&nbsp;Qing-Cang Shui ,&nbsp;Shuang-Nan Zhang ,&nbsp;Yu-Peng Chen","doi":"10.1016/j.jheap.2025.01.003","DOIUrl":"10.1016/j.jheap.2025.01.003","url":null,"abstract":"<div><div>Swift J1727.8–1613 is a black hole X-ray binary that differs from other black hole X-ray binaries in that it has an extra hard component in addition to a reflection component. We perform spectral analysis with simultaneous Insight-HXMT, NICER and NuSTAR observations when the source was in the hard and hard intermediate states. For the presentation of the extra components, we investigate the correlation between the <span>relxill</span> parameters. We find that the correlation between the spectral index and the reflection fraction is consistent with MAXI J1820+070 when the jet dominates the reflection. This provides the second sample to have such a correlation during an outburst. Interestingly, when the reflection component is attributed to the corona, the spectral fit results in a small reflection fraction and the correlation between the spectral index and reflection fraction is in agreement with the overall trend built-in <span><span>You et al. (2023)</span></span> with a large sample of outbursts from other X-ray binaries. Hence Swift J1727.8–1613 turns out to be the first sample to bridge the MAXI J1820+070 to the majority of X-ray binaries according to the dual correlations observed between the spectral index and the reflection fraction. We speculate that a configuration of a jet plus a hot inner flow may account for this peculiar outburst behavior of Swift J1727.8–1613.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 316-324"},"PeriodicalIF":10.2,"publicationDate":"2025-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102768","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":"Extracting H0 and rd in q(t) parametrization models","authors":"Himanshu Chaudhary ,&nbsp;S.K.J. Pacif ,&nbsp;G. Mustafa ,&nbsp;Farruh Atamurotov ,&nbsp;Faisal Javed","doi":"10.1016/j.jheap.2025.01.001","DOIUrl":"10.1016/j.jheap.2025.01.001","url":null,"abstract":"<div><div>This study explores five models derived from the Pacif parameterization scheme of the Hubble parameter (<em>H</em>), which represent different forms of the deceleration parameter (DP). Our primary objective is to determine the parameter distributions of the Hubble constant (<span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>) and the sound horizon (<span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span>) for each model. Additionally, we analyze the evolution of the DP in each scenario to assess its implications for late-time cosmic evolution. In our analysis, we treat <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span> as a free parameter, which allows us to avoid relying on specific assumptions about early-Universe physics and recombination models. This approach ensures model independence on the early-Universe side and enables late-time cosmological observations to directly constrain <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span> alongside other key parameters. To extract the parameter distributions for the Pacif scheme, we use a combination of Baryon Acoustic Oscillation (BAO) data, Cosmic Chronometers (CC), Type Ia Supernovae (SNe Ia), Gamma-Ray Bursts (GRBs), and Quasars. Our results yield posterior distributions for <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> and <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span>, which demonstrate notable consistency with the Planck CMB data. Using the Akaike Information Criterion (AIC), we evaluate the models, finding that all five models provide robust agreement with the latest observational data.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 340-349"},"PeriodicalIF":10.2,"publicationDate":"2025-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102770","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":"Role of internal space correlations in the dynamics of a higher-dimensional Bianchi type-I universe: Shear scalar and Hubble parameter perspectives","authors":"Nihan Katırcı","doi":"10.1016/j.jheap.2025.01.002","DOIUrl":"10.1016/j.jheap.2025.01.002","url":null,"abstract":"<div><div>We investigate exact solutions of the Einstein field equations in higher-dimensional, spatially homogeneous Bianchi type-I spacetimes, introducing a real parameter <em>λ</em> that correlates the expansion rates of external and internal spaces. Extending beyond Robertson–Walker spacetime, our approach includes positive and negative correlations, suggesting a broader and isotropic/anisotropic cosmological model space. Positively correlated dimensions manifest as a cosmological constant at late times, while at early times, they mimic stiff-fluid-like dark energy that dilutes faster than radiation, paralleling early dark energy models. This suggests a pathway for alleviating the Hubble tension by tailoring higher-dimensional dynamics to reduce the sound horizon. When anisotropic expansion is allowed, these models achieve isotropization more efficiently than predicted by Wald's cosmic no-hair theorem. Negative correlations, in contrast, yield a higher-dimensional steady-state universe where the shear scalar remains constant, effectively emulating a negative cosmological constant. These distinct behaviors arise from a simple signature change: positive correlation accelerates shear scalar decay, while negative correlation stabilizes it. We demonstrate that the solutions admit analytic continuation from the Lorentzian to Euclidean regime (<span><math><mi>t</mi><mo>→</mo><mo>−</mo><mi>i</mi><mi>τ</mi></math></span>), revealing a wormhole-like topology that connects two asymptotic regions via a throat, with <span><math><mi>λ</mi><mo>→</mo><mo>−</mo><mi>λ</mi></math></span>.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 382-391"},"PeriodicalIF":10.2,"publicationDate":"2025-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143162957","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":"On the duration of gamma-ray bursts","authors":"Bing Zhang","doi":"10.1016/j.jheap.2024.12.013","DOIUrl":"10.1016/j.jheap.2024.12.013","url":null,"abstract":"<div><div>Recently, a short-duration GRB with supernova association (GRB 200826A) and two long-duration GRBs with kilonova associations (GRB 211211A and GRB 230307A) have been detected, which demolished the hope for a tidy connection between GRB duration with their progenitor systems. Here I summarize various physical factors that can shape the duration of a GRB and propose that the duration of a GRB can be defined by four factors: progenitor, central engine, emitter, and geometry. The progenitor-defined duration is only relevant when the central engine is powered by accretion and when the modifications by other factors are not important. The untidy situation of duration - progenitor mismatches suggests that other factors likely play important roles in defining GRB duration at least in some GRBs. In particular, a GRB may not be powered by accretion but rather by a millisecond magnetar at least for some GRBs. The complicated lightcurve of GRB 211211A suggests both progenitor- and engine-defined durations, which may require a new type of progenitor system involving a white dwarf - neutron star merger with a magnetar merger product. The single broad pulse lightcurve with well-behaved energy-dependent behavior of GRB 230307A suggests an emitter-defined long duration. The central engine timescale may be short enough to be accommodated within the framework of a standard binary neutron star merger. Its spiky lightcurve with fast variability as well as extended X-ray emission suggest the existence of mini-jets in the global dissipation region, powered by an underlying magnetar.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 325-332"},"PeriodicalIF":10.2,"publicationDate":"2025-01-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102420","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":"Particle dynamics and quasi-periodic oscillations in the Dyonic ModMax: Constraint using quasars data","authors":"Husanboy Hoshimov ,&nbsp;Akbar Davlataliev ,&nbsp;Farruh Atamurotov ,&nbsp;Ahmadjon Abdujabbarov ,&nbsp;Ali Övgün","doi":"10.1016/j.jheap.2024.12.012","DOIUrl":"10.1016/j.jheap.2024.12.012","url":null,"abstract":"<div><div>In this work, we have worked out dynamical aspects for the particles moving in the Dyonic Mod Max spacetime. We have calculated the innermost stable circular orbit (ISCO) around black hole in Dyonic Mod Max and explored its implications for different microquasars. Considering the Dyonic Mod Max black hole as a microquasar source, we have studied quasi-periodic oscillation (QPO) around such a black hole. Finally, we determine constraint values for the parameters <em>Q</em> and <em>γ</em> in the Dyonic ModMax spacetime by analyzing QPOs observed from the quasars GRO J1655–40, XTE J1550–564, XTE J1859+226, GRS 1915+105, and H1743-322. We use the Monte Carlo Markov Chain (MCMC) method to analyze the observational data, which helps us refine these parameters and better understand the behavior of black holes in the Dyonic ModMax model.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 306-315"},"PeriodicalIF":10.2,"publicationDate":"2025-01-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102767","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":"Static, spherically symmetric solutions in f(Q)-gravity and in nonmetricity scalar-tensor theory","authors":"Nikolaos Dimakis ,&nbsp;Petros A. Terzis ,&nbsp;Andronikos Paliathanasis ,&nbsp;Theodosios Christodoulakis","doi":"10.1016/j.jheap.2024.12.011","DOIUrl":"10.1016/j.jheap.2024.12.011","url":null,"abstract":"<div><div>We solve the gravitational field equations for a static, spherically symmetric spacetime within the framework of the symmetric teleparallel theory of gravity. Specifically, we derive new solutions within the context of power-law <span><math><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)</mo></math></span> gravity and the nonmetricity scalar-tensor theory. For the connection in the non-coincidence gauge, we present the point-like Lagrangian that describes the employed field equations. Furthermore, we construct two conservation laws, and for different values of these conserved quantities, we analytically solve the gravitational field equations. New solutions are obtained, we investigate their physical properties and their general relativistic limit. Finally, we discuss the algebraic properties for the derived spacetimes.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 273-289"},"PeriodicalIF":10.2,"publicationDate":"2024-12-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102790","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":"NuSTAR and NICER observations of X Persei","authors":"Binay Rai,&nbsp;Mohammed Tobrej,&nbsp;Manoj Ghising,&nbsp;Bikash Chandra Paul","doi":"10.1016/j.jheap.2024.12.009","DOIUrl":"10.1016/j.jheap.2024.12.009","url":null,"abstract":"<div><div>We have studied the timing and spectral properties of the persistent Be/X-ray pulsar namely, X Persei using the <em>NuSTAR</em> and <em>NICER</em> observations of 2019. The pulsar is continuously in spin-up phase since 2003 with a spin-up rate of ∼(-3.18±0.04)×10⁻⁴ <span><math><mi>y</mi><msup><mrow><mi>r</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math></span>. A broadband 0.7-79 keV energy spectral fitting is performed using <em>NuSTAR</em> and <em>NICER</em> observations. It is found that the two component model considered here fits the spectrum more satisfactorily than the single-component model. An additional <span>gabs</span> model was used to fit an absorption-like feature found in the residuals of the spectrum fitted by the two components model. We interpret the absorption-like feature in the spectrum with a cyclotron line as reported in the literature. The centroid energy of the absorption-like feature is found to lie in the energy range of 32.5- 36.0 keV. The absorption feature found here is independent of the models used in fitting the spectrum. The broadband spectrum is also fitted making use of the physical bulk and thermal Comptonization model suggesting that thermal Comptonization dominates over bulk Comptonization.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 265-272"},"PeriodicalIF":10.2,"publicationDate":"2024-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102789","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}