Journal of High Energy Astrophysics最新文献

{"title":"Corrigendum to “Revisiting the 2021 outburst of the BHC MAXI J1803-298 using NICER, NuSTAR, and insight-HXMT data” [Journal of High Energy Astrophysics, Vol 53, Article 100640]","authors":"Kaushik Chatterjee, Sujoy K. Nath","doi":"10.1016/j.jheap.2026.100653","DOIUrl":"10.1016/j.jheap.2026.100653","url":null,"abstract":"","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"54 ","pages":"Article 100653"},"PeriodicalIF":6.1,"publicationDate":"2026-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148635363","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}

{"title":"Corrigendum to “Optical transients from non-explosive double white-dwarf mergers: the case of a central neutron star remnant” [JHEAP 53 (2026) 100600]","authors":"Ridha Fathima M․M․,&nbsp;Alexandre M.R. Almeida,&nbsp;M. Bulla,&nbsp;Jaziel G. Coelho,&nbsp;C. Guidorzi,&nbsp;J.A. Rueda","doi":"10.1016/j.jheap.2026.100647","DOIUrl":"10.1016/j.jheap.2026.100647","url":null,"abstract":"<div><div>The authors regret to report a numerical error that underestimated the spindown decay of the remnant neutron star (NS) from a double white-dwarf (DWD) merger in the paper JHEAP 53 (2026) 100600. The error significantly affects one of the examples reported in the article, namely the remnant NS with dipole factor <span><math><mrow><mi>log</mi><mi>D</mi><mo>=</mo><mi>log</mi><mo>(</mo><msup><mi>B</mi><mn>2</mn></msup><mo>/</mo><msubsup><mi>P</mi><mn>0</mn><mn>4</mn></msubsup><mo>)</mo><mo>=</mo><mn>40</mn></mrow></math></span>, corresponding to <span><math><mrow><mi>B</mi><mo>=</mo><msup><mn>10</mn><mn>14</mn></msup></mrow></math></span> G and <span><math><mrow><msub><mi>P</mi><mn>0</mn></msub><mo>=</mo><mn>1</mn></mrow></math></span> ms. The correction changes the late-time behaviour of the transient. Figures 1– 4, C.6 and <span><span>Tables 1</span></span>– <span><span>2</span></span> in the paper are updated here for this case (see <span><span>Fig. 1</span></span>, <span><span>Fig. 2</span></span>, <span><span>Fig. 3</span></span>, <span><span>Fig. 4</span></span>, <span><span>Fig. 5</span></span> below). This correction changes the upper limit of values (highlighted in <strong>bold</strong>) quoted in the abstract as follows: We find the LSST detection horizons upper limits ranging 30–<strong>820</strong> Mpc and corresponding detection rates 10²–10⁶ yr<span><math><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math></span> for <span><math><mrow><mi>log</mi><mi>D</mi><mo>=</mo><mn>24</mn></mrow></math></span>–40. Accounting for the survey cadence, we find that only configurations with <span><math><mrow><mi>log</mi><mi>D</mi><mo>=</mo><mn>36</mn></mrow></math></span>–40 are detectable within 240–<strong>760</strong> Mpc, with detection rates 10⁴–<strong>10</strong>⁵ yr<span><math><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math></span>. The conclusions of the paper hold. The authors would like to apologise for any inconvenience caused.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"54 ","pages":"Article 100647"},"PeriodicalIF":6.1,"publicationDate":"2026-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148635364","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}

{"title":"Growth of high-redshift quasars from fermion dark matter seeds","authors":"Yu Wang ,&nbsp;Remo Ruffini","doi":"10.1016/j.jheap.2026.100576","DOIUrl":"10.1016/j.jheap.2026.100576","url":null,"abstract":"<div><div>Quasars hosting  ≳ 10⁹ <em>M</em>_⊙ black holes at <em>z</em> &gt; 6 challenge growth scenarios that start from light seeds and assume accretion within already formed galaxies. Motivated by the James Webb Space Telescope (JWST) discovery of Little Red Dots (LRDs), which suggests that  ∼ 10⁶ <em>M</em>_⊙ black holes can be active in compact, pre-galactic environments, we revisit early black hole growth with a minimal cosmology-based framework. We model the accretion history as the smaller of the Bondi inflow rate and the Eddington-limited rate, where the Bondi rate is set by the supply of overdense primordial gas whose density declines with cosmic expansion, and the Eddington rate captures regulation by radiative feedback. By fitting the observed masses and luminosities of J0313–1806 (<span><math><mrow><mi>z</mi><mo>=</mo><mn>7.64</mn></mrow></math></span>) and J0100+2802 (<span><math><mrow><mi>z</mi><mo>=</mo><mn>6.30</mn></mrow></math></span>) with Bayesian inference, we infer initial conditions that favor massive seed black holes with initial mass <em>M</em>₀ ∼ 10⁶ <em>M</em>_⊙, formed at <span><math><mrow><mi>z</mi><mo>∼</mo><mn>20</mn><mo>−</mo><mn>30</mn></mrow></math></span> in environments with baryonic overdensity factors <em>f_ρ</em> ≳ 50 relative to the cosmic mean. The resulting growth histories include a prolonged supply-limited stage, and they reproduce the observed quasar masses without requiring sustained Eddington accretion or any super-Eddington episodes. The inferred seed mass scale is consistent with black holes produced by the collapse of quantum-degenerate fermion dark matter cores, providing a physically defined pathway to massive seeds at the redshifts implied by LRD phenomenology.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100576"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174573","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":"Exotic PeVatrons as sources of ultra-high-energy gamma rays","authors":"Andrea Addazi ,&nbsp;Salvatore Capozziello ,&nbsp;Qingyu Gan","doi":"10.1016/j.jheap.2026.100561","DOIUrl":"10.1016/j.jheap.2026.100561","url":null,"abstract":"<div><div>We explore novel classes of exotic astrophysical sources capable of producing ultra-high-energy gamma rays extending beyond the PeV scale, motivated by quantum gravity scenarios and dark matter phenomenology. These sources include: ultra-spinning black hole vortex-string systems; exotic compact objects such as boson star, axion star and Q-ball. Such <em>Exotica</em> generate powerful magnetic fields through interactions with millicharged dark matter, enabling particle acceleration mechanisms that surpass the energy limits of conventional astrophysical sources like pulsar wind nebulae and supernova remnants. We demonstrate that such exotic PeVatrons could be distributed throughout our Galaxy and may be detectable by current (LHAASO, HAWC) and next-generation (CTA) gamma-ray observatories.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100561"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146081843","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":"Constraints on cyclotron features and accretion regime in the high-mass X-ray binary 4U 1700–37 from NuSTAR","authors":"L. West-Ocampo ,&nbsp;F.A. Fogantini ,&nbsp;E.A. Saavedra ,&nbsp;J.A. Combi ,&nbsp;F. García ,&nbsp;P.L. Luque-Escamilla ,&nbsp;J. Martí ,&nbsp;S. Chaty ,&nbsp;J.F. Albacete-Colombo","doi":"10.1016/j.jheap.2026.100567","DOIUrl":"10.1016/j.jheap.2026.100567","url":null,"abstract":"<div><div>4U 1700–37 is a wind-fed high-mass X-ray binary comprising a compact object, most likely a neutron star, accreting from the O6.5 Iaf<span><math><msup><mrow></mrow><mo>+</mo></msup></math></span> supergiant HD 153919. Coherent pulsations have not been firmly detected and the magnetic field strength remains uncertain, with previous <em>NuSTAR</em> studies reporting only marginal candidate cyclotron resonant scattering features (CRSFs). We analyses all available <em>NuSTAR</em> observations of 4U 1700–37 to characterize its hard X-ray timing and broadband spectral properties, test the robustness of candidate CRSFs against different continuum models and epochs, and constrain the magnetic field and accretion regime of the compact object. We perform a homogeneous timing and spectral analysis of two <em>NuSTAR</em> observations, modeling time-averaged and intensity-resolved spectra with several continua commonly used for accreting pulsars, and use spectral simulations to quantify the significance and model dependence of putative CRSFs. No coherent pulsations are detected and we constrain the pulsed fraction to be &lt;1.5%. The spectra are well described by an absorbed blackbody plus cut-off power-law continuum, but show shallow absorption-like residuals around  ∼ 20 keV and at higher energies ( ∼ 40–50 keV). These features improve the fits and can reach high formal significances for some continua, yet do not constitute firm, model-independent CRSF detections in our baseline analysis. Intensity-resolved spectroscopy hints at shifts of the apparent line centroid with flux. Interpreted as cyclotron features, these results favour a neutron-star magnetic field <em>B</em> ∼ (1.7–4.4) × 10¹² G and a quasi-spherical subsonic accretion regime with an equilibrium spin period <em>P</em>_eq ∼ 1.9 ks. Even without a secure CRSF detection, the homogeneous multi-epoch analysis provides quantitative constraints on the magnetic field and accretion physics of 4U 1700–37 and helps reconcile previously discrepant line-energy measurements.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100567"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174572","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":"Observational constraints on new class dark energy parameterized EoS in Bianchi type-I universe","authors":"Sajal Mandal","doi":"10.1016/j.jheap.2026.100564","DOIUrl":"10.1016/j.jheap.2026.100564","url":null,"abstract":"<div><div>This study presents an extensive study of a class of time-evolving dark energy models defined by parametrized equations of state (EoS) parameter in the context of a spatially homogeneous yet anisotropic Bianchi type-I universe. In particular, we employ two distinct parametrization of the EoS parameter and thoroughly investigate their impact on the cosmic expansion history in the model. We utilize a diverse dataset composed of the cosmic chronometers, baryon acoustic oscillations (BAO), the cosmic microwave background (CMB), and the Pantheon+SH0ES supernova type Ia sample to impose constraints on the model parameters through the Bayesian analysis with the Markov Chain Monte Carlo (MCMC) approach. We also examine the crucial cosmological quantities such as the Hubble parameter, deceleration parameter, jerk parameter, and the effective EoS parameter to provide a comprehensive understanding of the cosmic evolution in the models. Moreover, we utilize the diagnostic parameters <em>Om</em>(<em>z</em>) and the statefinder (<em>r, s</em>) to examine the difference between the studied models and the ΛCDM model. To further strengthen the study, we assess the statistical performance of the models using the Akaike Information Criterion (AIC) and the Bayesian Information Criterion (BIC). The isotropic models and their anisotropic extensions exhibit the accelerating universe expansion, and we demonstrate different aspects of these models with reference to the ΛCDM model and CPL parametrization based dark energy model.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100564"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174568","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 acceleration to PeV energies in pulsar wind nebula: A two zone model","authors":"Gunindra Krishna Mahanta ,&nbsp;Nilay Bhatt ,&nbsp;Bitan Ghosal ,&nbsp;Subir Bhattacharyya","doi":"10.1016/j.jheap.2026.100562","DOIUrl":"10.1016/j.jheap.2026.100562","url":null,"abstract":"<div><div><em>PeVatrons</em> are the extreme galactic accelerators capable of producing PeV particles. Recent observation of Large High Altitude Air Shower Observatory have detected UHE photons ( ≥  100 TeV) from 43 galactic sources. Detection of UHE photons demands the presence of at least PeV particles in the acceleration site. Although the exact nature of most of the sources are still unknown, a large fraction of these sources have spatial association with pulsar wind nebula. In this work we investigate the acceleration mechanism in pulsar wind nebula by following a magnetohydrodynamics approach. Current study relates the MHD flow solution in immediate downstream with the particle spectrum and spectral energy distribution of photons. Our study shows that MHD description in the PWN environment reduces the parameter space and most of the parameters can be constrained in terms of a single parameter, <em>the magnetization parameter σ</em> only. Considering the effect of <em>σ</em>, we show that in low <em>σ</em> environment pulsar wind nebula can produce PeV particles. We have also investigate the role of turbulence in the nebular region in acceleration of particle to PeV energy. Current study shows that both low <em>σ</em> environment and turbulence environment is favorable for acceleration of particles up to PeV energy. We have also tested our model in two different LHAASO detected PeVatron 1LHAASO J1848-000u and 1LHAASO J1929+1846u.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100562"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174569","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":"Observational constraints on viscous cosmology in f(T, Lm) gravity","authors":"M. Koussour ,&nbsp;Alnadhief H.A. Alfedeel ,&nbsp;S. Muminov ,&nbsp;J. Rayimbaev","doi":"10.1016/j.jheap.2026.100578","DOIUrl":"10.1016/j.jheap.2026.100578","url":null,"abstract":"<div><div>We investigate the late-time cosmic acceleration within the framework of viscous <em>f</em>(<em>T, L_m</em>) gravity, where the gravitational action depends on both the torsion scalar <em>T</em> and the matter Lagrangian <em>L_m</em>. In this context, the Universe is modeled as a bulk viscous fluid, allowing for dissipative effects that generate an effective negative pressure capable of driving acceleration without invoking a cosmological constant. We adopt a simple linear model <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>T</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>)</mo></mrow><mo>=</mo><mi>α</mi><mi>T</mi><mo>+</mo><mi>β</mi><msub><mi>L</mi><mi>m</mi></msub></mrow></math></span> and assume a constant bulk viscosity coefficient <span><math><mrow><mi>ζ</mi><mo>=</mo><msub><mi>ζ</mi><mn>0</mn></msub><mo>&gt;</mo><mn>0</mn></mrow></math></span>. The model parameters are constrained using a joint analysis of recent observational datasets, including 31 Hubble parameter measurements, the Pantheon+ sample of 1701 Type Ia Supernovae, and the latest baryon acoustic oscillation data from DESI, employing a Markov Chain Monte Carlo (MCMC) approach. The best-fit results, <span><math><mrow><msub><mi>H</mi><mn>0</mn></msub><mo>=</mo><mn>68.16</mn><mo>±</mo><mn>0.65</mn></mrow></math></span>, <span><math><mrow><mi>α</mi><mo>=</mo><mn>1</mn><mo>.</mo><msubsup><mn>53</mn><mrow><mo>−</mo><mn>0.61</mn></mrow><mrow><mo>+</mo><mn>0.49</mn></mrow></msubsup></mrow></math></span>, <span><math><mrow><mi>β</mi><mo>=</mo><mn>0.40</mn><mo>±</mo><mn>0.96</mn></mrow></math></span>, and <span><math><mrow><msub><mi>ζ</mi><mn>0</mn></msub><mo>=</mo><mn>2</mn><mo>.</mo><msubsup><mn>15</mn><mrow><mo>−</mo><mn>0.81</mn></mrow><mrow><mo>+</mo><mn>0.69</mn></mrow></msubsup></mrow></math></span>, are consistent with current cosmological observations and indicate that bulk viscosity plays a significant role in the late-time dynamics. The deceleration parameter <span><math><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>0.33</mn><mo>±</mo><mn>0.41</mn></mrow></math></span> confirms the current accelerated expansion, while the effective equation of state (EoS) evolves from a matter-like regime at high redshift toward a quintessence phase at late times. The <em>Om</em>(<em>z</em>) diagnostic further supports this behavior, suggesting a mild deviation from ΛCDM toward a dynamical dark energy component. Although information criteria (<span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>AIC</mtext><mo>=</mo><mn>2.2</mn></mrow></math></span>, <span><math><mrow><mstyle><mi>Δ</mi></mstyle><mtext>BIC</mtext><mo>=</mo><mn>13.13</mn></mrow></math></span>) slightly favor the simpler ΛCDM model, the viscous <em>f</em>(<em>T, L_m</em>) framework remains a viable and physically motivated alternative capable of explaining cosmic acceleration through the combined effects of torsion-matter coupling and viscosity.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100578"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174988","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":"Van Allen Probe observations of the pitch angle evolutions of high-energy protons near the second peak of inner radiation belt","authors":"J.H. Zhang ,&nbsp;L.Y. Li ,&nbsp;Y.W. Yao ,&nbsp;K.X. Cheng ,&nbsp;L. Yang","doi":"10.1016/j.jheap.2026.100568","DOIUrl":"10.1016/j.jheap.2026.100568","url":null,"abstract":"<div><div>Utilizing the full pitch angle (<span><math><mi>α</mi></math></span>) measurements by the Relativistic Electron-Proton Telescope (REPT) onboard Van Allen Probe A, we analyzed the pitch angle distribution and storm-time variation mechanism of high-energy protons (&lt; 30MeV) near the second peak (<em>L</em>* = 1.84 – 1.98) of Earth’s inner radiation belt (<em>L</em>*≤ 2.5). We found that the fluxes of the <span><math><msup><mn>40</mn><mo>∘</mo></msup></math></span> to <span><math><msup><mn>140</mn><mo>∘</mo></msup></math></span> protons decrease during the main phase of storms and then gradually increase during the recovery phase, whereas those fluxes at smaller or larger pitch angles (<span><math><mrow><mi>α</mi><mo>&lt;</mo><msup><mn>40</mn><mo>∘</mo></msup></mrow></math></span> or &gt; <span><math><msup><mn>140</mn><mo>∘</mo></msup></math></span>) remain relatively stable during the whole storms. Theoretic calculations indicate that the bounce latitude (<span><math><mi>λ</mi></math></span> &gt; 26°) of the quasi-parallel or anti-parallel moving protons (<span><math><mrow><mi>α</mi><mo>&lt;</mo><msup><mn>40</mn><mo>∘</mo></msup></mrow></math></span> or &gt; <span><math><msup><mn>140</mn><mo>∘</mo></msup></math></span>) exceeds the influence range (<span><math><mrow><mi>λ</mi><mspace></mspace></mrow></math></span>≤ 20°) of storm-time ring currents in the inner belt region (<em>L</em>*≤ 2.5), but those of the oblique and quasi-perpendicular protons (<span><math><mrow><msup><mn>40</mn><mo>∘</mo></msup><mo>&lt;</mo><mi>α</mi><mo>&lt;</mo><msup><mn>140</mn><mo>∘</mo></msup></mrow></math></span>) overlap with the low-latitude ring currents. During the main/recovery phase of storms, the oblique and quasi-perpendicular protons are transported outwards/inwards and thus experience Fermi and Betatron decelerations/accelerations. The adiabatic decelerations/accelerations modify the pancake-like pitch angle distributions of the tens of MeV protons in the outer half part (<em>L</em>* = 1.6 – 2.5) of the inner radiation belt, whereas field line curvature scatterings become effective outside the proton radiation belt (<em>L</em>* &gt; 2.5).</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100568"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174570","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":"Loop quantum inflation with inverse volume corrections in light of ACT data","authors":"Farough Parvizi ,&nbsp;Soma Heydari ,&nbsp;Milad Solbi ,&nbsp;Kayoomars Karami","doi":"10.1016/j.jheap.2026.100563","DOIUrl":"10.1016/j.jheap.2026.100563","url":null,"abstract":"<div><div>Within the framework of loop quantum cosmology (LQC), we investigate the effect of inverse volume corrections on the low scale spontaneously broken supersymmetric (SB SUSY) and exponential inflationary potentials. The LQC modifications to the Friedmann equations and cosmological perturbation parameters are employed to assess the observational viability of these models against recent data from the Atacama Cosmology Telescope (ACT). Our results indicate that in contrast to the standard model of inflation, in the presence of inverse volume corrections in LQC, the predictions of SB SUSY and exponential potentials in the <span><math><mrow><mi>r</mi><mo>−</mo><msub><mi>n</mi><mrow><mi>s</mi></mrow></msub></mrow></math></span> plane lie inside the 68% confidence level interval of the ACT data.</div></div>","PeriodicalId":54265,"journal":{"name":"Journal of High Energy Astrophysics","volume":"52 ","pages":"Article 100563"},"PeriodicalIF":10.5,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146174571","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}