Pub Date : 2025-12-04DOI: 10.1016/j.jheap.2025.100530
D. Pugliese , Z. Stuchlík
A Ringed Accretion disk (RAD) is a cluster of axially symmetric, mixed co–rotating and counter–rotating co–planar tori, orbiting on the equatorial plane of a central Kerr black hole (BH). In this work we focus on the red-shift and spectral lines emission from the RAD. Our analysis of the emissions maps, giving appearance of the RAD, envisages the possibility that the presence of a possible disk internal ringed structure could be observable from a density radial discrete structure, and a composite radial distribution of angular momentum in the disk. The co–rotating and counter–rotating bands, in the disk internal structure, are found distinguished in red-shift, in dependence on the view angle, and the BH spin. We frame our investigation, using different source corona models, and emissivity profiles for the disk. Lines emission turns affected by the knobby surface of the disk. The results of this analysis have been compared with the results for the infinite disk and the correspondent unstructured disks.
{"title":"The red-shift and spectral lines of the Kerr black hole ringed accretion disks","authors":"D. Pugliese , Z. Stuchlík","doi":"10.1016/j.jheap.2025.100530","DOIUrl":"10.1016/j.jheap.2025.100530","url":null,"abstract":"<div><div>A Ringed Accretion disk (<strong>RAD</strong>) is a cluster of axially symmetric, mixed co–rotating and counter–rotating co–planar tori, orbiting on the equatorial plane of a central Kerr black hole (<strong>BH</strong>). In this work we focus on the red-shift and spectral lines emission from the <strong>RAD</strong>. Our analysis of the emissions maps, giving appearance of the <strong>RAD</strong>, envisages the possibility that the presence of a possible disk internal ringed structure could be observable from a density radial discrete structure, and a composite radial distribution of angular momentum in the disk. The co–rotating and counter–rotating bands, in the disk internal structure, are found distinguished in red-shift, in dependence on the view angle, and the <strong>BH</strong> spin. We frame our investigation, using different source corona models, and emissivity profiles for the disk. Lines emission turns affected by the knobby surface of the disk. The results of this analysis have been compared with the results for the infinite disk and the correspondent unstructured disks.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100530"},"PeriodicalIF":10.5,"publicationDate":"2025-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748542","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}
Pub Date : 2025-12-04DOI: 10.1016/j.jheap.2025.100529
Na Wang , Guowei Ren , Shun Zhang , Tingfeng Yi , Tong Liu , Mouyuan Sun
Based on the Zwicky Transient Facility (ZTF), we selected 10 blazars as our sample sources. Among these, we found four blazars (J 0923.5+4125, J 1221.3+3010, J 1503.5+4759, and J 1652.7+4024) showing possible indications of quasi periodic oscillations (QPOs) modulation. We conducted a detailed analysis of their optical light curves (g- and r-bands) over the past five years using the root mean square (RMS)-Flux relation, flux distribution, and QPO detection methods to investigate their variability characteristics. A linear RMS-Flux relation is present in both bands, and their flux distributions follow a log-normal form. This suggests that optical variability may arise from multiplicative, nonlinear processes across different timescales and flux states. Further QPO analysis using the weighted wavelet Z-transform (WWZ), Lomb-Scargle periodogram (LSP), and autoregressive integrated moving average (ARIMA) methods identified candidate periodic signals in four blazars. J 0923.5+4125 (period ∼ 205 days) and J 1221.3+3010 ( ∼ 630 days) show local significances of ∼ 3σ, whereas J 1503.5+4759 ( ∼ 38.5 days) and J 1652.7+4024 ( ∼ 48 days) reach ∼ 4σ. After accounting for the look-elsewhere effect, the global significances for J 1503.5+4759 in the g- and r-bands are ∼ 2.7σ, while for J 1652.7+4024 they are approximately ∼ 2.5σ in both bands. These two blazars warrant further monitoring and investigation.
{"title":"Possible quasi-periodic optical oscillations of ZTF blazars","authors":"Na Wang , Guowei Ren , Shun Zhang , Tingfeng Yi , Tong Liu , Mouyuan Sun","doi":"10.1016/j.jheap.2025.100529","DOIUrl":"10.1016/j.jheap.2025.100529","url":null,"abstract":"<div><div>Based on the Zwicky Transient Facility (ZTF), we selected 10 blazars as our sample sources. Among these, we found four blazars (J 0923.5+4125, J 1221.3+3010, J 1503.5+4759, and J 1652.7+4024) showing possible indications of quasi periodic oscillations (QPOs) modulation. We conducted a detailed analysis of their optical light curves (g- and r-bands) over the past five years using the root mean square (RMS)-Flux relation, flux distribution, and QPO detection methods to investigate their variability characteristics. A linear RMS-Flux relation is present in both bands, and their flux distributions follow a log-normal form. This suggests that optical variability may arise from multiplicative, nonlinear processes across different timescales and flux states. Further QPO analysis using the weighted wavelet Z-transform (WWZ), Lomb-Scargle periodogram (LSP), and autoregressive integrated moving average (ARIMA) methods identified candidate periodic signals in four blazars. J 0923.5+4125 (period ∼ 205 days) and J 1221.3+3010 ( ∼ 630 days) show local significances of ∼ 3<em>σ</em>, whereas J 1503.5+4759 ( ∼ 38.5 days) and J 1652.7+4024 ( ∼ 48 days) reach ∼ 4<em>σ</em>. After accounting for the look-elsewhere effect, the global significances for J 1503.5+4759 in the g- and r-bands are ∼ 2.7<em>σ</em>, while for J 1652.7+4024 they are approximately ∼ 2.5<em>σ</em> in both bands. These two blazars warrant further monitoring and investigation.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100529"},"PeriodicalIF":10.5,"publicationDate":"2025-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748543","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}
As an update on the initial findings of DESI, the new results provide the first hint of potential deviations from a cosmological constant (), which, if confirmed with significance , would challenge the validity of Λ within the ΛCDM model. We explore the Generalized Emergent Dark Energy (GEDE) model using recent BAO measurements from DESI DR2, Type Ia supernova compilations, and CMB distance priors. Employing nested sampling, we constrain the parameter Δ, which characterizes deviations from ΛCDM. Our analysis shows that with CMB+DESI DR2 alone, GEDE tends to prefer positive values of Δ. However, when different SNe Ia calibrations are included, the model favors negative values of Δ, corresponding to an earlier injection of dark energy. The Marginalized constraints on ω(z) further shows that GEDE sharply emerges but then asymptotes to without crossing it. At z ∼ 1 data, GEDE provides a better fit than ΛCDM, while at z ≲ 0.5 the data favor , bringing the model deviate from ΛCDM. Bayesian model comparison shows weak support for GEDE with CMB+DESI DR2 (), moderate with PP (), weak-to-moderate with Union3 (), and weak with DES-SN5Y (). Overall, GEDE is consistent with current data and mildly favored when SNe Ia are included, making it a viable extension of ΛCDM that merits further investigation with future high precision measurements.
{"title":"Probing generalized emergent dark energy with DESI DR2","authors":"Vipin Kumar Sharma , Himanshu Chaudhary , Sanved Kolekar","doi":"10.1016/j.jheap.2025.100518","DOIUrl":"10.1016/j.jheap.2025.100518","url":null,"abstract":"<div><div>As an update on the initial findings of DESI, the new results provide the first hint of potential deviations from a cosmological constant (<span><math><mrow><mi>ω</mi><mo>=</mo><mo>−</mo><mn>1</mn></mrow></math></span>), which, if confirmed with significance <span><math><mrow><mo>></mo><mo>(</mo><mn>2</mn><mo>−</mo><mn>4</mn><mo>)</mo><mi>σ</mi></mrow></math></span>, would challenge the validity of Λ within the ΛCDM model. We explore the Generalized Emergent Dark Energy (GEDE) model using recent BAO measurements from DESI DR2, Type Ia supernova compilations, and CMB distance priors. Employing nested sampling, we constrain the parameter Δ, which characterizes deviations from ΛCDM. Our analysis shows that with CMB+DESI DR2 alone, GEDE tends to prefer positive values of Δ. However, when different SNe Ia calibrations are included, the model favors negative values of Δ, corresponding to an earlier injection of dark energy. The Marginalized constraints on <em>ω</em>(<em>z</em>) further shows that GEDE sharply emerges but then asymptotes to <span><math><mrow><mi>ω</mi><mo>=</mo><mo>−</mo><mn>1</mn></mrow></math></span> without crossing it. At <em>z</em> ∼ 1 data, GEDE provides a better fit than ΛCDM, while at <em>z</em> ≲ 0.5 the data favor <span><math><mrow><mi>ω</mi><mo>></mo><mo>−</mo><mn>1</mn></mrow></math></span>, bringing the model deviate from ΛCDM. Bayesian model comparison shows weak support for GEDE with CMB+DESI DR2 (<span><math><mrow><mi>ln</mi><mi>B</mi><mi>F</mi><mo>=</mo><mn>1.96</mn></mrow></math></span>), moderate with PP (<span><math><mrow><mi>ln</mi><mi>B</mi><mi>F</mi><mo>=</mo><mn>2.65</mn></mrow></math></span>), weak-to-moderate with Union3 (<span><math><mrow><mi>ln</mi><mi>B</mi><mi>F</mi><mo>=</mo><mn>2.34</mn></mrow></math></span>), and weak with DES-SN5Y (<span><math><mrow><mi>ln</mi><mi>B</mi><mi>F</mi><mo>=</mo><mn>1.44</mn></mrow></math></span>). Overall, GEDE is consistent with current data and mildly favored when SNe Ia are included, making it a viable extension of ΛCDM that merits further investigation with future high precision measurements.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100518"},"PeriodicalIF":10.5,"publicationDate":"2025-12-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748544","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}
Pub Date : 2025-11-29DOI: 10.1016/j.jheap.2025.100519
A. Kaushal , A. Manchanda , M.G. Dainotti , K. Gupta , Z. Nogala , A. Madhan , S. Naqi , Ritik Kumar , V. Oad , N. Indoriya , Krishnanjan Sil , D.H. Hartmann , M. Bogdan , A. Pollo , J.X. Prochaska , N. Fraija
Mitigating data gaps in Gamma-ray bursts (GRBs) light curves (LCs) is crucial for cosmological research, enhancing the precision of parameters, assuming perfect satellite conditions for complete LC coverage with no gaps. This analysis improves the applicability of the two-dimensional Dainotti relation, which connects the rest-frame end time of the plateau emission (Ta) and its luminosity (La), derived from the fluxes (Fa). The study expands on a previous 521 GRB sample by incorporating seven models: Deep Gaussian Process (DGP), Temporal Convolutional Network (TCN), Hybrid CNN with Bidirectional Long Short-Term Memory (CNN-BiLSTM), Bayesian Neural Network (BNN), Polynomial Curve Fitting, Isotonic Regression, and Quartic Smoothing Spline (QSS). Results indicate that QSS significantly reduces uncertainty across parameters–43.5 % for log Ta, 43.2 % for log Fa, and 48.3 % for α, outperforming the other models where α denotes the slope post-plateau based on Willingale’s 2007 functional form. The Polynomial Curve Fitting model demonstrates moderate uncertainty reduction across parameters, while CNN-BiLSTM has the lowest outlier rate for α at 0.77 %. These models broaden the application of machine-learning techniques in GRB LC analysis, enhancing uncertainty estimation and parameter recovery, and complement traditional methods like the Attention U-Net and Multilayer Perceptron (MLP). These advancements highlight the potential of GRBs as cosmological probes, supporting their role in theoretical model discrimination via LC parameters, serving as standard candles, and facilitating GRB redshift predictions through advanced machine-learning approaches.
{"title":"Multi-model framework for reconstructing gamma-Ray burst light curves","authors":"A. Kaushal , A. Manchanda , M.G. Dainotti , K. Gupta , Z. Nogala , A. Madhan , S. Naqi , Ritik Kumar , V. Oad , N. Indoriya , Krishnanjan Sil , D.H. Hartmann , M. Bogdan , A. Pollo , J.X. Prochaska , N. Fraija","doi":"10.1016/j.jheap.2025.100519","DOIUrl":"10.1016/j.jheap.2025.100519","url":null,"abstract":"<div><div>Mitigating data gaps in Gamma-ray bursts (GRBs) light curves (LCs) is crucial for cosmological research, enhancing the precision of parameters, assuming perfect satellite conditions for complete LC coverage with no gaps. This analysis improves the applicability of the two-dimensional Dainotti relation, which connects the rest-frame end time of the plateau emission (<em>T<sub>a</sub></em>) and its luminosity (<em>L<sub>a</sub></em>), derived from the fluxes (<em>F<sub>a</sub></em>). The study expands on a previous 521 GRB sample by incorporating seven models: Deep Gaussian Process (DGP), Temporal Convolutional Network (TCN), Hybrid CNN with Bidirectional Long Short-Term Memory (CNN-BiLSTM), Bayesian Neural Network (BNN), Polynomial Curve Fitting, Isotonic Regression, and Quartic Smoothing Spline (QSS). Results indicate that QSS significantly reduces uncertainty across parameters–43.5 % for log <em>T<sub>a</sub></em>, 43.2 % for log <em>F<sub>a</sub></em>, and 48.3 % for <em>α</em>, outperforming the other models where <em>α</em> denotes the slope post-plateau based on Willingale’s 2007 functional form. The Polynomial Curve Fitting model demonstrates moderate uncertainty reduction across parameters, while CNN-BiLSTM has the lowest outlier rate for <em>α</em> at 0.77 %. These models broaden the application of machine-learning techniques in GRB LC analysis, enhancing uncertainty estimation and parameter recovery, and complement traditional methods like the Attention U-Net and Multilayer Perceptron (MLP). These advancements highlight the potential of GRBs as cosmological probes, supporting their role in theoretical model discrimination via LC parameters, serving as standard candles, and facilitating GRB redshift predictions through advanced machine-learning approaches.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100519"},"PeriodicalIF":10.5,"publicationDate":"2025-11-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748545","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}
Pub Date : 2025-11-24DOI: 10.1016/j.jheap.2025.100517
Manuel Gonzalez-Espinoza , Genly Leon , Yoelsy Leyva , Giovanni Otalora , Andronikos Paliathanasis , Aleksander Kozak
We study scalar field cosmologies in higher-order gravity, inspired by the Pais–Uhlenbeck oscillator, which admits a fourth-order ghost-free sector. By recasting the equations as a slow–fast system, we analyze phase-space evolution under exponential, power-law, and arbitrary potentials using both analytical and geometric methods. The full system exhibits a rational structure with singular surfaces and, under a slow manifold constraint, reduces to a regular four-dimensional form that supports global analysis and perturbative stability. The -deviser technique reconstructs potential-adapted functions , enabling attractor classification and center manifold analysis. Two-field extensions yield scaling laws and tracking behavior in the quintom regime. In the quintessence regime, we examine de Sitter stability, incorporating radiation and dust to model realistic transitions, and derive analytic expressions for and across reconstructed inflationary potentials-obtained from standard, Gaussian, hybrid, extended, and logarithmic expansions of the scale factor-with a scalar field evolving linearly in time. Our results confirm the viability of Pais–Uhlenbeck scalar models for inflation and dark energy, offering tools to study attractors and bifurcations in higher-derivative cosmology.
{"title":"Slow–fast evolution of scalar fields in higher-order cosmological gravity dynamics inspired by the Pais–Uhlenbeck oscillator","authors":"Manuel Gonzalez-Espinoza , Genly Leon , Yoelsy Leyva , Giovanni Otalora , Andronikos Paliathanasis , Aleksander Kozak","doi":"10.1016/j.jheap.2025.100517","DOIUrl":"10.1016/j.jheap.2025.100517","url":null,"abstract":"<div><div>We study scalar field cosmologies in higher-order gravity, inspired by the Pais–Uhlenbeck oscillator, which admits a fourth-order ghost-free sector. By recasting the equations as a slow–fast system, we analyze phase-space evolution under exponential, power-law, and arbitrary potentials using both analytical and geometric methods. The full system exhibits a rational structure with singular surfaces and, under a slow manifold constraint, reduces to a regular four-dimensional form that supports global analysis and perturbative stability. The <span><math><mi>f</mi></math></span>-deviser technique reconstructs potential-adapted functions <span><math><mrow><mi>f</mi><mo>(</mo><mi>λ</mi><mo>)</mo></mrow></math></span>, enabling attractor classification and center manifold analysis. Two-field extensions yield scaling laws and tracking behavior in the quintom regime. In the quintessence regime, we examine de Sitter stability, incorporating radiation and dust to model realistic transitions, and derive analytic expressions for <span><math><msub><mi>n</mi><mi>s</mi></msub></math></span> and <span><math><mi>r</mi></math></span> across reconstructed inflationary potentials-obtained from standard, Gaussian, hybrid, extended, and logarithmic expansions of the scale factor-with a scalar field evolving linearly in time. Our results confirm the viability of Pais–Uhlenbeck scalar models for inflation and dark energy, offering tools to study attractors and bifurcations in higher-derivative cosmology.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100517"},"PeriodicalIF":10.5,"publicationDate":"2025-11-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748541","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}
Pub Date : 2025-11-21DOI: 10.1016/j.jheap.2025.100516
M. Koussour , O. Donmez , S. Bekov , A. Altaibayeva , A. Saginbay , S. Muminov , J. Rayimbaev
<div><div>We introduce and constrain a new parameterization for the dark energy equation of state, the b-CPL model, defined as <span><math><mrow><msub><mi>ω</mi><mrow><mi>b</mi><mtext>-CPL</mtext></mrow></msub><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msub><mi>ω</mi><mn>0</mn></msub><mo>+</mo><msub><mi>ω</mi><mn>1</mn></msub><mfrac><mi>z</mi><mrow><mn>1</mn><mo>+</mo><mi>b</mi><mi>z</mi></mrow></mfrac></mrow></math></span>, which extends the standard CPL framework by including a parameter <em>b</em>. This additional degree of freedom provides enhanced flexibility to capture potential deviations from standard dynamical dark energy behavior, while reducing to CPL for <span><math><mrow><mi>b</mi><mo>=</mo><mn>1</mn></mrow></math></span> and to ΛCDM in specific limits. Notably, the b-CPL parameterization remains finite at future times, avoiding divergences. Using a combined dataset of cosmic chronometers, PantheonPlus Type Ia supernovae, and DESI baryon acoustic oscillations, we perform a Markov Chain Monte Carlo analysis to constrain the cosmological parameters for the b-CPL, CPL, and ΛCDM models. The b-CPL model yields a more negative present-day equation of state (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>1</mn><mo>.</mo><msubsup><mn>12</mn><mrow><mo>−</mo><mn>0.20</mn></mrow><mrow><mo>+</mo><mn>0.31</mn></mrow></msubsup></mrow></math></span>) and a higher matter density (<span><math><mrow><msubsup><mstyle><mi>Ω</mi></mstyle><mi>m</mi><mn>0</mn></msubsup><mo>=</mo><mn>0</mn><mo>.</mo><msubsup><mn>332</mn><mrow><mo>−</mo><mn>0.049</mn></mrow><mrow><mo>+</mo><mn>0.065</mn></mrow></msubsup></mrow></math></span>) compared to CPL and ΛCDM. Model selection statistics based on the reduced chi-square, AIC, and BIC indicate that b-CPL is strongly preferred, showing decisive evidence over ΛCDM (<span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>AIC</mtext><mo>=</mo><mo>−</mo><mn>41.83</mn></mrow></math></span>, <span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>BIC</mtext><mo>=</mo><mo>−</mo><mn>30.91</mn></mrow></math></span>) and significant improvement over CPL (<span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>AIC</mtext><mo>=</mo><mo>−</mo><mn>26.05</mn></mrow></math></span>, <span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>BIC</mtext><mo>=</mo><mo>−</mo><mn>9.66</mn></mrow></math></span>). Physically, the b-CPL model exhibits a mild redshift evolution of the EoS parameter and tends to remain in the phantom regime (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo><</mo><mo>−</mo><mn>1</mn></mrow></math></span>) at present, although within 68 % confidence level, the quintessence region (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo>></mo><mo>−</mo><mn>1</mn></mrow></math></span>) is still allowed. It predicts the strongest present-day acceleration (<span><math><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>0.62</mn><mo>±</mo><mn>0.27</mn></mrow></math></span>), and
{"title":"Testing the b-CPL dynamical dark energy model with recent cosmological data","authors":"M. Koussour , O. Donmez , S. Bekov , A. Altaibayeva , A. Saginbay , S. Muminov , J. Rayimbaev","doi":"10.1016/j.jheap.2025.100516","DOIUrl":"10.1016/j.jheap.2025.100516","url":null,"abstract":"<div><div>We introduce and constrain a new parameterization for the dark energy equation of state, the b-CPL model, defined as <span><math><mrow><msub><mi>ω</mi><mrow><mi>b</mi><mtext>-CPL</mtext></mrow></msub><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow><mo>=</mo><msub><mi>ω</mi><mn>0</mn></msub><mo>+</mo><msub><mi>ω</mi><mn>1</mn></msub><mfrac><mi>z</mi><mrow><mn>1</mn><mo>+</mo><mi>b</mi><mi>z</mi></mrow></mfrac></mrow></math></span>, which extends the standard CPL framework by including a parameter <em>b</em>. This additional degree of freedom provides enhanced flexibility to capture potential deviations from standard dynamical dark energy behavior, while reducing to CPL for <span><math><mrow><mi>b</mi><mo>=</mo><mn>1</mn></mrow></math></span> and to ΛCDM in specific limits. Notably, the b-CPL parameterization remains finite at future times, avoiding divergences. Using a combined dataset of cosmic chronometers, PantheonPlus Type Ia supernovae, and DESI baryon acoustic oscillations, we perform a Markov Chain Monte Carlo analysis to constrain the cosmological parameters for the b-CPL, CPL, and ΛCDM models. The b-CPL model yields a more negative present-day equation of state (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>1</mn><mo>.</mo><msubsup><mn>12</mn><mrow><mo>−</mo><mn>0.20</mn></mrow><mrow><mo>+</mo><mn>0.31</mn></mrow></msubsup></mrow></math></span>) and a higher matter density (<span><math><mrow><msubsup><mstyle><mi>Ω</mi></mstyle><mi>m</mi><mn>0</mn></msubsup><mo>=</mo><mn>0</mn><mo>.</mo><msubsup><mn>332</mn><mrow><mo>−</mo><mn>0.049</mn></mrow><mrow><mo>+</mo><mn>0.065</mn></mrow></msubsup></mrow></math></span>) compared to CPL and ΛCDM. Model selection statistics based on the reduced chi-square, AIC, and BIC indicate that b-CPL is strongly preferred, showing decisive evidence over ΛCDM (<span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>AIC</mtext><mo>=</mo><mo>−</mo><mn>41.83</mn></mrow></math></span>, <span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>BIC</mtext><mo>=</mo><mo>−</mo><mn>30.91</mn></mrow></math></span>) and significant improvement over CPL (<span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>AIC</mtext><mo>=</mo><mo>−</mo><mn>26.05</mn></mrow></math></span>, <span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>BIC</mtext><mo>=</mo><mo>−</mo><mn>9.66</mn></mrow></math></span>). Physically, the b-CPL model exhibits a mild redshift evolution of the EoS parameter and tends to remain in the phantom regime (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo><</mo><mo>−</mo><mn>1</mn></mrow></math></span>) at present, although within 68 % confidence level, the quintessence region (<span><math><mrow><msub><mi>ω</mi><mn>0</mn></msub><mo>></mo><mo>−</mo><mn>1</mn></mrow></math></span>) is still allowed. It predicts the strongest present-day acceleration (<span><math><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>0.62</mn><mo>±</mo><mn>0.27</mn></mrow></math></span>), and ","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100516"},"PeriodicalIF":10.5,"publicationDate":"2025-11-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145610151","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}
Pub Date : 2025-11-21DOI: 10.1016/j.jheap.2025.100515
Dorian Araya , Cristian Castillo , Genly Leon , Juan Magaña , Angie Barr Domínguez , Miguel A. García-Aspeitia
We revisit a cosmological model where dark matter (DM) and dark energy (DE) follow barotropic equations of state, allowing deviations from the standard ΛCDM framework (i.e. wdm ≠ 0, ), considering both flat and non-flat curvature. Using a dynamical system approach, we identify equilibrium states that govern stability, expansion, and contraction. Expansion occurs when H > 0, while contraction is linked to H < 0. Accelerated expansion arises from DE dominance, whereas radiation- and matter-dominated phases lead to deceleration. Some solutions are unphysical due to density constraints, but viable cases offer insights into cosmic transitions, including the Einstein static universe, which allows for shifts between accelerating and decelerating phases. We perform a Bayesian analysis with updated datasets, including observational Hubble data, Pantheon+ Type Ia supernovae, strong lensing systems, baryon acoustic oscillations and cosmic microwave background, to constrain the parameters wdm and wde. Our results from the data joint analysis show consistency with ΛCDM within 3σ, but none of the cases reproduce and . Nevertheless, the comparison with the standard model using the Akaike and Bayesian information criteria indicates that only the non-flat scenario has the potential to be competitive. This suggests that a non-dust-like DM may impact structure formation, while DE could shift toward quintessence fluid. While ΛCDM remains a strong model, our findings indicate that alternative dark sector models with non-standard EoS could be viable and offer new insights into cosmic evolution.
{"title":"wdm−wde cosmological model with new data samples of cosmological observations","authors":"Dorian Araya , Cristian Castillo , Genly Leon , Juan Magaña , Angie Barr Domínguez , Miguel A. García-Aspeitia","doi":"10.1016/j.jheap.2025.100515","DOIUrl":"10.1016/j.jheap.2025.100515","url":null,"abstract":"<div><div>We revisit a cosmological model where dark matter (DM) and dark energy (DE) follow barotropic equations of state, allowing deviations from the standard ΛCDM framework (i.e. <em>w<sub>dm</sub></em> ≠ 0, <span><math><mrow><msub><mi>w</mi><mrow><mi>d</mi><mi>e</mi></mrow></msub><mo>≠</mo><mo>−</mo><mn>1</mn></mrow></math></span>), considering both flat and non-flat curvature. Using a dynamical system approach, we identify equilibrium states that govern stability, expansion, and contraction. Expansion occurs when <em>H</em> > 0, while contraction is linked to <em>H</em> < 0. Accelerated expansion arises from DE dominance, whereas radiation- and matter-dominated phases lead to deceleration. Some solutions are unphysical due to density constraints, but viable cases offer insights into cosmic transitions, including the Einstein static universe, which allows for shifts between accelerating and decelerating phases. We perform a Bayesian analysis with updated datasets, including observational Hubble data, Pantheon+ Type Ia supernovae, strong lensing systems, baryon acoustic oscillations and cosmic microwave background, to constrain the parameters <em>w<sub>dm</sub></em> and <em>w<sub>de</sub></em>. Our results from the data joint analysis show consistency with ΛCDM within 3<em>σ</em>, but none of the cases reproduce <span><math><mrow><msub><mi>w</mi><mrow><mi>d</mi><mi>m</mi></mrow></msub><mo>=</mo><mn>0</mn></mrow></math></span> and <span><math><mrow><msub><mi>w</mi><mrow><mi>d</mi><mi>e</mi></mrow></msub><mo>=</mo><mo>−</mo><mn>1</mn></mrow></math></span>. Nevertheless, the comparison with the standard model using the Akaike and Bayesian information criteria indicates that only the non-flat scenario has the potential to be competitive. This suggests that a non-dust-like DM may impact structure formation, while DE could shift toward quintessence fluid. While ΛCDM remains a strong model, our findings indicate that alternative dark sector models with non-standard EoS could be viable and offer new insights into cosmic evolution.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"51 ","pages":"Article 100515"},"PeriodicalIF":10.5,"publicationDate":"2025-11-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145694269","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}
Pub Date : 2025-11-19DOI: 10.1016/j.jheap.2025.100513
Manoj Ghising , Nirpat Subba , Mohammed Tobrej , Binay Rai , Bikash Chandra Paul
We present a comprehensive spectral–timing analysis of a BHXB Swift J1727.8−1613 during its 2023 outburst, using five pointed NuSTAR observations sampling the luminous hard–intermediate state. Broadband 3–79 keV spectroscopy employs a physically motivated model combining a cool truncated disk (diskbb), relativistic reflection (relxill in reflection-only mode), and Comptonized continuum (nthComp) to probe the inner accretion geometry around a rapidly spinning black hole () at moderate inclination. Simultaneous timing analysis reveals type-C quasi-periodic oscillations (QPOs) with novel coherence evolution: the quality factor (Q) exhibits a striking non-monotonic dependence on both QPO frequency and luminosity, peaking near Hz and declining at both lower and higher frequencies. This turnover directly constrains Lense–Thirring precession geometry, implying optimal coherence at intermediate truncation radius. A tight photon-index–QPO-frequency correlation demonstrates that spectral softening and frequency rise are concurrent signatures of inward truncation-radius motion. The triadic luminosity evolution—rising disk and Compton, declining reflection—traces precession-driven geometry changes and corona beaming effects. Interpreting disk-normalization variability as apparent-area changes rather than physical radius swings provides new insight into disk-corona boundary layers. These quantitative results provide strong evidence for global Lense–Thirring precession regulation of both timing and spectral properties, establishing Swift J1727.8−1613 as a benchmark source for understanding accretion-geometry physics during black hole state transitions.
{"title":"Spectral–timing evolution of a black hole X-ray binary Swift J1727.8–1613: Linking disk reflection and type-C QPO frequency during the 2023 outburst","authors":"Manoj Ghising , Nirpat Subba , Mohammed Tobrej , Binay Rai , Bikash Chandra Paul","doi":"10.1016/j.jheap.2025.100513","DOIUrl":"10.1016/j.jheap.2025.100513","url":null,"abstract":"<div><div>We present a comprehensive spectral–timing analysis of a BHXB Swift J1727.8−1613 during its 2023 outburst, using five pointed <em>NuSTAR</em> observations sampling the luminous hard–intermediate state. Broadband 3–79 keV spectroscopy employs a physically motivated model combining a cool truncated disk (<span>diskbb</span>), relativistic reflection (<span>relxill</span> in reflection-only mode), and Comptonized continuum (<span>nthComp</span>) to probe the inner accretion geometry around a rapidly spinning black hole (<span><math><msub><mrow><mi>a</mi></mrow><mrow><mo>⁎</mo></mrow></msub><mo>=</mo><mn>0.98</mn></math></span>) at moderate inclination. Simultaneous timing analysis reveals type-C quasi-periodic oscillations (QPOs) with novel coherence evolution: the quality factor (<em>Q</em>) exhibits a striking non-monotonic dependence on both QPO frequency and luminosity, peaking near <span><math><msub><mrow><mi>ν</mi></mrow><mrow><mi>QPO</mi></mrow></msub><mo>∼</mo><mn>1.2</mn></math></span> Hz and declining at both lower and higher frequencies. This turnover directly constrains Lense–Thirring precession geometry, implying optimal coherence at intermediate truncation radius. A tight photon-index–QPO-frequency correlation demonstrates that spectral softening and frequency rise are concurrent signatures of inward truncation-radius motion. The triadic luminosity evolution—rising disk and Compton, declining reflection—traces precession-driven geometry changes and corona beaming effects. Interpreting disk-normalization variability as apparent-area changes rather than physical radius swings provides new insight into disk-corona boundary layers. These quantitative results provide strong evidence for global Lense–Thirring precession regulation of both timing and spectral properties, establishing Swift J1727.8−1613 as a benchmark source for understanding accretion-geometry physics during black hole state transitions.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"50 ","pages":"Article 100513"},"PeriodicalIF":10.5,"publicationDate":"2025-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145571749","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}
Pub Date : 2025-11-19DOI: 10.1016/j.jheap.2025.100514
Manish Yadav , Archana Dixit , M.S. Barak , Anirudh Pradhan
In this study, we investigate the wCDM dynamical dark energy model with spatial curvature utilizing the recently released DESI Collaboration data (DR1 and DR2) in conjunction with other observational probes such as BBN, Observational Hubble Data (OHD), and Pantheon Plus (PP). Our investigation attempts to discover which DESI dataset gives a better match to the wCDM framework and assess the impact of spatial curvature on cosmological constraints. We find that the cosmic curvature parameter, , disfavors the cosmological constant for the DR2+BBN and DR2+BBN+OHD data combinations. However, the deviation from the cosmological constant remains below the 1σ level, indicating a mild preference for a open universe. In contrast, when using the DR1 based combinations namely DR1+BBN and DR1+BBN+OHD—the deviation from the cosmological constant increases to approximately 1.2σ, suggesting a slightly stronger indication of a open geometry. Also, the best-fit values of the Hubble constant () obtained from the DR1+BBN+OHD+PP and DR2+BBN+OHD+PP combinations within the dynamical dark energy model are consistent with the results reported by the Planck Collaboration. Our findings provide constraints on the dark energy EoS parameter , reveal a mild but notable deviation from the vacuum energy () scenario at a significance level 1.8σ from DR2+BBN+OHD+PP and 0.5σ from DR1+BBN+OHD+PP, both favoring the quintessence region of dark energy. Furthermore, the key physical distance measures , , and show better consistency with our model when analyzed with the DR2 data.
在这项研究中，我们利用最近发布的DESI协作数据（DR1和DR2），结合其他观测探测器，如BBN、哈勃观测数据（OHD）和Pantheon Plus (PP)，研究了wCDM动态暗能量模型的空间曲率。我们的研究试图发现哪个DESI数据集能更好地匹配wCDM框架，并评估空间曲率对宇宙学约束的影响。我们发现宇宙曲率参数Ωk不利于DR2+BBN和DR2+BBN+OHD数据组合的宇宙学常数。然而，与宇宙学常数的偏差仍然低于1σ水平，表明对开放宇宙有轻微的偏好。相比之下，当使用基于DR1的组合（即DR1+BBN和DR1+BBN+ ohd）时，与宇宙学常数的偏差增加到约1.2σ，表明开放几何的迹象略强。此外，DR1+BBN+OHD+PP和DR2+BBN+OHD+PP组合在动态暗能量模型中获得的哈勃常数（H0）的最佳拟合值与普朗克合作报告的结果一致。我们的发现提供了对暗能量EoS参数w0的约束，揭示了与真空能量（w= - 1）情景的轻微但显著的偏差，从DR2+BBN+OHD+PP到DR1+BBN+OHD+PP的显著性水平为1.8σ，从DR1+BBN+OHD+PP到0.5σ，都有利于暗能量的精髓区域。此外，当与DR2数据进行分析时，关键物理距离测量DH、DV和DM与我们的模型具有更好的一致性。
{"title":"Constraints on spatial curvature and dark energy dynamics in the wCDM model from DESI DR1 and DR2","authors":"Manish Yadav , Archana Dixit , M.S. Barak , Anirudh Pradhan","doi":"10.1016/j.jheap.2025.100514","DOIUrl":"10.1016/j.jheap.2025.100514","url":null,"abstract":"<div><div>In this study, we investigate the <em>w</em>CDM dynamical dark energy model with spatial curvature utilizing the recently released DESI Collaboration data (DR1 and DR2) in conjunction with other observational probes such as BBN, Observational Hubble Data (OHD), and Pantheon Plus (PP). Our investigation attempts to discover which DESI dataset gives a better match to the <em>w</em>CDM framework and assess the impact of spatial curvature on cosmological constraints. We find that the cosmic curvature parameter, <span><math><msub><mrow><mi>Ω</mi></mrow><mrow><mi>k</mi></mrow></msub></math></span>, disfavors the cosmological constant for the DR2+BBN and DR2+BBN+OHD data combinations. However, the deviation from the cosmological constant remains below the 1<em>σ</em> level, indicating a mild preference for a open universe. In contrast, when using the DR1 based combinations namely DR1+BBN and DR1+BBN+OHD—the deviation from the cosmological constant increases to approximately 1.2<em>σ</em>, suggesting a slightly stronger indication of a open geometry. Also, the best-fit values of the Hubble constant (<span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>) obtained from the DR1+BBN+OHD+PP and DR2+BBN+OHD+PP combinations within the dynamical dark energy model are consistent with the results reported by the Planck Collaboration. Our findings provide constraints on the dark energy EoS parameter <span><math><msub><mrow><mi>w</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span>, reveal a mild but notable deviation from the vacuum energy (<span><math><mi>w</mi><mo>=</mo><mo>−</mo><mn>1</mn></math></span>) scenario at a significance level 1.8<em>σ</em> from DR2+BBN+OHD+PP and 0.5<em>σ</em> from DR1+BBN+OHD+PP, both favoring the quintessence region of dark energy. Furthermore, the key physical distance measures <span><math><msub><mrow><mi>D</mi></mrow><mrow><mi>H</mi></mrow></msub></math></span>, <span><math><msub><mrow><mi>D</mi></mrow><mrow><mi>V</mi></mrow></msub></math></span>, and <span><math><msub><mrow><mi>D</mi></mrow><mrow><mi>M</mi></mrow></msub></math></span> show better consistency with our model when analyzed with the DR2 data.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"50 ","pages":"Article 100514"},"PeriodicalIF":10.5,"publicationDate":"2025-11-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145617888","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}
Pub Date : 2025-11-17DOI: 10.1016/j.jheap.2025.100511
Khawaja T. Tasneem , M. Umair Shahzad , Nusrat Perveen , Kamal M. Othman , Abdulfattah Noorwali , Esam Y.O. Zafar
Blue straggler stars (BSSs) are intriguing anomalies in Globular Clusters (GCs) that challenge conventional stellar evolution models by appearing both younger and more luminous than their cluster counterparts. Accurately estimating their populations is crucial for understanding their formation mechanisms and the dynamic evolution of GCs. However, traditional photometric and spectroscopic methods are constrained by observational biases and computational limitations. In this study, we propose a machine learning (ML) framework to predict BSS populations in GCs using simulated data from the Monte Carlo Cluster simulator (MOCCA) Survey Database 1, which models 12 Gyr of GC evolution. We train three ML algorithms: XGBoost, Gradient Boosting, and Random Forest Regression on 12 dynamical and structural cluster properties to estimate BSS numbers. Model performance is assessed by utilizing normalized root mean square error (nRMSE), normalized mean absolute error (nMAE), and coefficient of determination (). Among the tested models, XGBoost exhibits the most accurate model (, , ), outperforming Gradient Boosting (, , ) and Random Forest Regression (, , ). Our results demonstrate that ML models can accurately predict BSS populations in real GCs, offering a robust alternative to traditional observational methods. This approach enables efficient, high-precision BSS estimation while mitigating the challenges posed by observational constraints, thereby advancing our understanding of GC stellar populations and their evolutionary pathways. Additionally, we compare our findings with literature and discover that ML outperforms conventional observational techniques by detecting noticeably more BSS in the majority of, especially in packed settings. This implies that ML is eeficient technique for examining star development and cluster dynamics and that earlier research may have understated BSS populations.
{"title":"Machine learning-based prediction of blue straggler star populations in stellar clusters","authors":"Khawaja T. Tasneem , M. Umair Shahzad , Nusrat Perveen , Kamal M. Othman , Abdulfattah Noorwali , Esam Y.O. Zafar","doi":"10.1016/j.jheap.2025.100511","DOIUrl":"10.1016/j.jheap.2025.100511","url":null,"abstract":"<div><div>Blue straggler stars (BSSs) are intriguing anomalies in Globular Clusters (GCs) that challenge conventional stellar evolution models by appearing both younger and more luminous than their cluster counterparts. Accurately estimating their populations is crucial for understanding their formation mechanisms and the dynamic evolution of GCs. However, traditional photometric and spectroscopic methods are constrained by observational biases and computational limitations. In this study, we propose a machine learning (ML) framework to predict BSS populations in GCs using simulated data from the Monte Carlo Cluster simulator (MOCCA) Survey Database 1, which models 12 Gyr of GC evolution. We train three ML algorithms: XGBoost, Gradient Boosting, and Random Forest Regression on 12 dynamical and structural cluster properties to estimate BSS numbers. Model performance is assessed by utilizing normalized root mean square error (nRMSE), normalized mean absolute error (nMAE), and coefficient of determination (<span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span>). Among the tested models, XGBoost exhibits the most accurate model (<span><math><mi>n</mi><mi>R</mi><mi>M</mi><mi>S</mi><mi>E</mi><mo>=</mo><mn>0.037</mn></math></span>, <span><math><mi>n</mi><mi>M</mi><mi>A</mi><mi>E</mi><mo>=</mo><mn>0.024</mn></math></span>, <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>=</mo><mn>0.933</mn></math></span>), outperforming Gradient Boosting (<span><math><mi>n</mi><mi>R</mi><mi>M</mi><mi>S</mi><mi>E</mi><mo>=</mo><mn>0.041</mn></math></span>, <span><math><mi>n</mi><mi>M</mi><mi>A</mi><mi>E</mi><mo>=</mo><mn>0.027</mn></math></span>, <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>=</mo><mn>0.926</mn></math></span>) and Random Forest Regression (<span><math><mi>n</mi><mi>R</mi><mi>M</mi><mi>S</mi><mi>E</mi><mo>=</mo><mn>0.041</mn></math></span>, <span><math><mi>n</mi><mi>M</mi><mi>A</mi><mi>E</mi><mo>=</mo><mn>0.026</mn></math></span>, <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>=</mo><mn>0.927</mn></math></span>). Our results demonstrate that ML models can accurately predict BSS populations in real GCs, offering a robust alternative to traditional observational methods. This approach enables efficient, high-precision BSS estimation while mitigating the challenges posed by observational constraints, thereby advancing our understanding of GC stellar populations and their evolutionary pathways. Additionally, we compare our findings with literature and discover that ML outperforms conventional observational techniques by detecting noticeably more BSS in the majority of, especially in packed settings. This implies that ML is eeficient technique for examining star development and cluster dynamics and that earlier research may have understated BSS populations.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"50 ","pages":"Article 100511"},"PeriodicalIF":10.5,"publicationDate":"2025-11-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145571751","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}
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