Journal of High Energy Astrophysics最新文献_第6页

Exploring temperature influences on gravitational wave production in binary white dwarfs 探索温度对双白矮星引力波产生的影响

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-10 DOI: 10.1016/j.jheap.2025.01.004

Sílvia P. Nunes , José D.V. Arbañil , César H. Lenzi , Jaziel G. Coelho

{"title":"Exploring temperature influences on gravitational wave production in binary white dwarfs","authors":"Sílvia P. Nunes , José D.V. Arbañil , César H. Lenzi , 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}

引用次数: 0

A possible jet and corona configuration for Swift J1727.8–1613 during the hard state 在硬状态下，雨燕J1727.8-1613可能的射流和日冕结构

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-09 DOI: 10.1016/j.jheap.2025.01.003

Jing-Qiang Peng , Shu Zhang , Qing-Cang Shui , Shuang-Nan Zhang , Yu-Peng Chen

{"title":"A possible jet and corona configuration for Swift J1727.8–1613 during the hard state","authors":"Jing-Qiang Peng , Shu Zhang , Qing-Cang Shui , Shuang-Nan Zhang , 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}

引用次数: 0

Extracting H0 and rd in q(t) parametrization models 在q(t)参数化模型中提取H0和rd

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-09 DOI: 10.1016/j.jheap.2025.01.001

Himanshu Chaudhary , S.K.J. Pacif , G. Mustafa , Farruh Atamurotov , Faisal Javed

{"title":"Extracting H0 and rd in q(t) parametrization models","authors":"Himanshu Chaudhary , S.K.J. Pacif , G. Mustafa , Farruh Atamurotov , 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}

引用次数: 0

Role of internal space correlations in the dynamics of a higher-dimensional Bianchi type-I universe: Shear scalar and Hubble parameter perspectives 内部空间关联在高维Bianchi - i型宇宙动力学中的作用：剪切标量和哈勃参数视角

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-09 DOI: 10.1016/j.jheap.2025.01.002

Nihan Katırcı

{"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}

引用次数: 0

On the duration of gamma-ray bursts 伽马射线暴的持续时间

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-07 DOI: 10.1016/j.jheap.2024.12.013

Bing Zhang

{"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}

引用次数: 0

Particle dynamics and quasi-periodic oscillations in the Dyonic ModMax: Constraint using quasars data Dyonic ModMax中的粒子动力学和准周期振荡：使用类星体数据的约束

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2025-01-03 DOI: 10.1016/j.jheap.2024.12.012

Husanboy Hoshimov , Akbar Davlataliev , Farruh Atamurotov , Ahmadjon Abdujabbarov , Ali Övgün

引用次数: 0

Static, spherically symmetric solutions in f(Q)-gravity and in nonmetricity scalar-tensor theory f(Q)-重力和非度量量-张量理论的静态球对称解

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2024-12-31 DOI: 10.1016/j.jheap.2024.12.011

Nikolaos Dimakis , Petros A. Terzis , Andronikos Paliathanasis , Theodosios Christodoulakis

引用次数: 0

NuSTAR and NICER observations of X Persei NuSTAR和NICER对X英仙座的观测

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2024-12-30 DOI: 10.1016/j.jheap.2024.12.009

Binay Rai, Mohammed Tobrej, Manoj Ghising, Bikash Chandra Paul

{"title":"NuSTAR and NICER observations of X Persei","authors":"Binay Rai, Mohammed Tobrej, Manoj Ghising, 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<sup>−4</sup> <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}

引用次数: 0

Detection of polarized Fermi-bubble synchrotron and dust emission 偏振费米泡同步加速器的探测与尘埃发射

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2024-12-30 DOI: 10.1016/j.jheap.2024.12.010

Uri Keshet

引用次数: 0

A doublet of cosmological models to challenge the H0 tension in the Pantheon Supernovae Ia catalog 宇宙学模型的双重挑战在万神殿超新星Ia目录中的H0张力

IF 10.2 4区物理与天体物理

Journal of High Energy Astrophysics Pub Date : 2024-12-24 DOI: 10.1016/j.jheap.2024.12.003

B. De Simone , M.H.P.M. van Putten , M.G. Dainotti , G. Lambiase

{"title":"A doublet of cosmological models to challenge the H0 tension in the Pantheon Supernovae Ia catalog","authors":"B. De Simone , M.H.P.M. van Putten , M.G. Dainotti , G. Lambiase","doi":"10.1016/j.jheap.2024.12.003","DOIUrl":"10.1016/j.jheap.2024.12.003","url":null,"abstract":"<div><div>ΛCDM provides a leading framework in the interpretation of modern cosmology. Nevertheless, the scientific community still struggles with many open problems in cosmology. Among the most noticeable ones, the tension in the Hubble constant <em>H</em><sub>0</sub> is particularly intriguing, prompting a wide range of possible solutions. In the present work, the flat scale-free cosmology (<em>S</em> CDM) of Maeder (2017) is tested for <em>H</em><sub>0</sub> tension in fits to the Pantheon sample of Supernovae Ia. The Pantheon sample is a collection of 1048 SNe Ia, which formally defines <em>H</em><sub>0</sub> = <em>H</em>(0) by extrapolation to redshift zero of data over positive redshifts <em>z</em> > 0. Here, we consider <em>H</em><sub>0,</sub><em><sub>k</sub></em> in fits of <em>S</em> CDM over <em>k</em> equally sized bins of sub-samples of mean redshift <em>z<sub>k</sub></em>. To quantify a trend in <em>H</em><sub>0,</sub><em><sub>k</sub></em> with <em>z<sub>k</sub></em>, the results are fit by <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msup><mrow><mrow><msubsup><mi>H</mi><mn>0</mn><mo>′</mo></msubsup><mo>/</mo><mrow><mo>(</mo><mrow><mn>1</mn><mo>+</mo><mi>z</mi></mrow><mo>)</mo></mrow></mrow></mrow><mi>α</mi></msup></mrow></math></span> in the two parameters <span><math><msubsup><mi>H</mi><mn>0</mn><mo>′</mo></msubsup></math></span> and α. This approach tests for model imperfections or data biases by trends that are inconsistent with zero. Our findings show a decreasing trend inconsistent with zero at 5.3σ significance, significantly more so than in ΛCDM. These results are further confirmed in Pantheon+. It appears that a solution to <em>H</em><sub>0</sub> tension is to be found in models with a deceleration parameter <em>q</em><sub>0</sub> < <em>q</em><sub>0,Λ</sub> below that of ΛCDM, rather than <em>q</em><sub>0,Λ</sub> < <em>q</em><sub>0,</sub><em><sub>S</sub></em> < 0 satisfied by <em>S</em> CDM.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"45 ","pages":"Pages 290-298"},"PeriodicalIF":10.2,"publicationDate":"2024-12-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143102791","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0