Astrophysics and Space Science最新文献

{"title":"Asymmetric cross-correlation functions with delays in Sco X-1: evidence of possible jet triggering","authors":"S. D. Gouse,&nbsp;M. V. R. Abhishek,&nbsp;K. Sriram","doi":"10.1007/s10509-025-04430-x","DOIUrl":"10.1007/s10509-025-04430-x","url":null,"abstract":"<div><p>The formation and origin of jets in Z sources are not understood very well, although a strong X-ray-radio correlation has been noticed. We analyzed seventeen observations of Sco X-1 observed by the Rossi X-ray Timing Explorer (RXTE) where radio jet emissions were detected. In five observations, we report the detection of asymmetric cross-correlation functions (CCF) with delays of a few tens of seconds between soft and hard energy bands light curves in the horizontal branch associated with a flat-topped noise in the power density spectrum (PDS). Interestingly, these five observations were connected to a ballistic-type radio emission. We performed simulations to confirm and robust the cross-correlation coefficients and the observed lags. The CCF was highly symmetric in the remaining twelve observations, exhibiting NBO (Normal Branch Oscillations) or NBO+HBO (Horizontal Branch Oscillations) in the PDS. During these X-ray observations, the radio observations were found to be associated with an ultra-relativistic flow (URF) radio emission. The X-ray spectrum analysis of the two observations that showed core radio emission and abrupt variations in the PDS and CCF revealed that the bbody fractional flux varied by 10–20%, but the spectral parameters did not vary. We suggest that the ballistic jet might have triggered the instability in the inner region of the accretion disk, viz., the boundary layer (BL) plausibly along with the corona, causing the asymmetry with delays observed in the CCFs, and it also explains the absence of any oscillation features in the PDS, leaving behind a flat-topped noise. During symmetric CCF, the accretion flow was steady, hence, NBO / NBO+HBO was persistent. However, connecting the URF either to NBO or HBO is difficult since the majority of PDS exhibit an NBO alone rather than a NBO+HBO. We hypothesize that URF is most likely related to the phenomenon that causes NBO. Overall, we conclude that the asymmetric CCF shows that the inner part of the accretion disk is unstable due to the triggering of a ballistic jet and constrains the inner accretion region’s size to about 20-30 km, which possibly causes the accretion ejection.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143883611","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":"Perihelion precession in non-Newtonian central potentials","authors":"Michele Andreoli","doi":"10.1007/s10509-025-04426-7","DOIUrl":"10.1007/s10509-025-04426-7","url":null,"abstract":"<div><p>High order corrections to the perihelion precession are obtained in non-Newtonian central potentials, via complex analysis techniques. The result is an exact series expansion whose terms, for a perturbation of the form, are calculated in closed form. To validate the method, the series is applied to the specific case of s = 3, and the results are compared with those presented in literature, which are relate to the Schwarzschild metric. As a further test, a numerical simulation was carried out for the case where s = 4. The algebraic calculations and numerical simulations were carried out via software with symbolic capabilities.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143871312","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Exploring cosmological effects of a constant jerk parameter in FLRW universe within (f(T)) gravity","authors":"Syed Mudassir Syed Iqbal,&nbsp;G. U. Khapekar","doi":"10.1007/s10509-025-04428-5","DOIUrl":"10.1007/s10509-025-04428-5","url":null,"abstract":"&lt;div&gt;&lt;p&gt;In this paper, we investigate the evolution of the FLRW universe by analyzing the constant jerk parameter &lt;span&gt;(j)&lt;/span&gt; within the framework of &lt;span&gt;(f(T))&lt;/span&gt; gravity. Using a model-independent parametrization approach, we assume &lt;span&gt;(j)&lt;/span&gt; as constant and derive an expression for the Hubble parameter as &lt;/p&gt;&lt;div&gt;&lt;div&gt;&lt;span&gt; $$begin{aligned} H(z)=H_{0}left [xi _{1}left (z+1right )^{frac{3+sqrt{8j+1}}{2}}+ left (1{-xi }_{1}right )left (z+1right )^{frac{3-sqrt{8j+1}}{2}} right ]^{frac{1}{2}} end{aligned}$$ &lt;/span&gt;&lt;/div&gt;&lt;/div&gt;&lt;p&gt; We estimate model parameters via a Chi-square test coupled with Markov Chain Monte Carlo (MCMC) simulations, based on 52 Observational Hubble Data (OHD) points and 1701 Pantheon+SHOES data points. This method yields the best fit values: &lt;span&gt;(xi _{1}={0.39}_{-0.08}^{+0.12})&lt;/span&gt;, &lt;span&gt;(j={0.67}_{-0.19}^{+0.19})&lt;/span&gt;, &lt;span&gt;(H_{0}={66.08}_{-2.78}^{+2.83} ; km/s/Mpc)&lt;/span&gt; for OHD dataset and &lt;span&gt;(xi _{1}={0.37}_{-0.03}^{+0.03})&lt;/span&gt;, &lt;span&gt;(j={0.67}_{-0.38}^{+0.40})&lt;/span&gt;, &lt;span&gt;(H_{0}={72.80}_{-0.29}^{+0.31})&lt;/span&gt; &lt;span&gt;(km/s/Mpc)&lt;/span&gt; for Pantheon+SHOES dataset. The value of &lt;span&gt;(H_{0})&lt;/span&gt; obtained in our analysis closely resembles the value estimated by the Planck Collaboration in 2018, &lt;span&gt;(H_{0}=67.4pm 0.5; km/s/Mpc)&lt;/span&gt;. Our analysis of the deceleration parameter &lt;span&gt;(q)&lt;/span&gt; reveals a transition from an early decelerating phase to a present accelerating expansion, with &lt;span&gt;(q_{0}approx -0.3887)&lt;/span&gt; &lt;span&gt;((OHD))&lt;/span&gt; and &lt;span&gt;(q_{0}approx -0.4139)&lt;/span&gt; &lt;span&gt;((Pantheon+SHOES))&lt;/span&gt;. Additionally, we examine dynamic parameter such as energy density, pressure, and equation of state parameter within the model &lt;span&gt;(fleft (Tright )=T+eta T^{beta })&lt;/span&gt;, where &lt;span&gt;(eta )&lt;/span&gt; and &lt;span&gt;(beta )&lt;/span&gt; are an arbitrary real constant. The equation of state parameter &lt;span&gt;(omega )&lt;/span&gt; in our model demonstrates a smooth transition from the radiation-dominated era to the matter-dominated era and finally to the dark energy era. The present-day values of &lt;span&gt;(omega _{0} approx -0.6196)&lt;/span&gt; &lt;span&gt;((OHD))&lt;/span&gt; and &lt;span&gt;(omega _{0} approx -0.6548)&lt;/span&gt; &lt;span&gt;((Pantheon+SHOES))&lt;/span&gt; suggests that the universe is currently in a quintessence phase, where dark energy behaves as a dynamical component rather than a cosmological constant &lt;span&gt;(omega = -1)&lt;/span&gt;. This behavior indicates that our model is physically acceptable and aligns with the general features of cosmic evolution. Notably, the strong energy condition (SEC) is violated at present &lt;span&gt;(left (z =0right ))&lt;/span&gt; and is projected to remain violated in the future &lt;span&gt;(left (z &lt; 0right ))&lt;/span&gt;, driving the observed accelerated expansion of the universe. Also, this study offers insights into the impact of a constant jerk parameter on cosmic evolution and expansion dynamics within the framework of modified gravity, with a specific focus on the &lt;span&gt;(fleft (Tright ))&lt;/span&gt; gravity ","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143865484","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The equilibrium configurations of neutron stars in the optimized (f(R,T)) gravity","authors":"J. T. Quartuccio,&nbsp;P. H. R. S. Moraes,&nbsp;G. N. Zeminiani,&nbsp;M. M. Lapola","doi":"10.1007/s10509-025-04429-4","DOIUrl":"10.1007/s10509-025-04429-4","url":null,"abstract":"<div><p>We construct equilibrium configurations for neutron stars using a specific <span>(f(R,T))</span> functional form, recently derived through gaussian process applied to measurements of the Hubble parameter. By construction, this functional form serves as an alternative explanation for cosmic acceleration, circumventing the cosmological constant problem. Here, we aim to examine its applicability within the stellar regime. In doing so, we seek to contribute to the modified gravity literature by applying the same functional form of a given gravity theory across highly distinct regimes. Our results demonstrate that equilibrium configurations of neutron stars can be obtained within this theory, with the energy density and maximum mass slightly exceeding those predicted by General Relativity. Additionally, we show that the value of some parameters in the <span>(f(R,T))</span> functional form must differ from those obtained in cosmological configurations, suggesting a potential scale-dependence for these parameters. We propose that further studies apply this functional form across different regimes to more thoroughly assess this possible dependence.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143845600","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":"Investigation of optimal transfers to retrograde co-orbital orbits in the Earth-Moon system","authors":"G. A. Caritá,&nbsp;M. H. M. Morais,&nbsp;S. Aljbaae,&nbsp;A. F. B. A. Prado","doi":"10.1007/s10509-025-04427-6","DOIUrl":"10.1007/s10509-025-04427-6","url":null,"abstract":"<div><p>Recent findings on retrograde co-orbital mean-motion resonances in the Earth-Moon system, highlight the potential use of spacecraft in retrograde resonances. Based on these discoveries, this study investigates retrograde co-orbital resonances within the Earth-Moon system, focusing on both optimal and sub-optimal orbital transfers to such configurations. The paper provides a comprehensive analysis of retrograde co-orbital resonances, optimization techniques to evaluate and enhance the performance of bi-impulsive transfers to these configurations. The results reveal the feasibility of low-cost transfers, which could support a range of future missions, including space exploration and satellite deployment. Combining advanced optimization processes, we obtained solutions for orbital transfers for different arrival points in retrograde co-orbitals improving mission efficiency and offering a cost-effective approach to interplanetary exploration.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143840513","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":"Tracing gravitational waves by integrating wavelet, PCA and clustering analysis using pulsar timing array data","authors":"Adityan S,&nbsp;A. Stanley Raj","doi":"10.1007/s10509-025-04425-8","DOIUrl":"10.1007/s10509-025-04425-8","url":null,"abstract":"<div><p>Pulsar Timing Arrays (PTAs) are a powerful tool to trace gravitational waves (GWs) signatures in the nanohertz frequency range by precisely monitoring timing residuals of millisecond pulsars. This study explores advancements in PTA methodologies, emphasizing machine learning (ML) techniques, wavelet analysis, and cross-correlation studies to enhance sensitivity to GW signals. Using data from the Indian Pulsar Timing Array (InPTA), we apply Principal Component Analysis (PCA), clustering algorithms, and wavelet-based time-frequency decomposition to improve the detection of the Stochastic Gravitational Wave Background (SGWB).Our analysis reveals a strong correlation (Pearson r = 0.872) between measured pulsar timing residuals and the Hellings-Downs curve, supporting the presence of an SGWB signal. Wavelet decomposition identifies significant low-frequency power, suggesting persistent timing residual structures consistent with GW signatures. PCA indicates that the first component captures ∼84.3% of the variance, highlighting a dominant common signal among pulsars. Clustering analysis reveals distinct pulsar groups, with some showing enhanced correlated noise features, likely linked to GW-induced fluctuations. Additionally, the estimated GW amplitude and spectral index for individual pulsars further reinforce the presence of a stochastic background. These findings demonstrate the effectiveness of dimensionality reduction and clustering techniques in isolating astrophysical signals, enhancing the reliability of GW detection. Our results provide strong support for the existence of an SGWB and showcase the potential of integrating machine learning with traditional pulsar timing analyses to refine GW detection strategies.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143835693","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":"Cometary observations in light-polluted environments: a case study of interstellar comet 2I/Borisov","authors":"Josep M. Trigo-Rodríguez,&nbsp;Damya Souami,&nbsp;Maria Gritsevich,&nbsp;Marcin Wesołowski,&nbsp;Gennady Borisov","doi":"10.1007/s10509-025-04424-9","DOIUrl":"10.1007/s10509-025-04424-9","url":null,"abstract":"<div><p>Comets and asteroids have long captured human curiosity, and until recently, all documented examples belonged to our Solar System. That changed with the discovery of the first known interstellar object, 1I/2017 U1 (‘Oumuamua), in 2017. Two years later, on August 30, 2019, Gennady Borisov discovered a second interstellar object, 2019 Q4, which was officially designated 2I/Borisov. From its initial images, the object’s diffuse appearance hinted at its cometary nature. To better understand the photometric evolution of comet 2I/Borisov as it traveled through the inner Solar System, we compiled observations using medium-sized telescopes. This data is crucial for gaining insights into its size and composition, as well as how such objects, after millions of years in interstellar space, behave when exposed to the Sun’s radiation. Given that 2I/Borisov is the first interstellar comet ever observed, constraining its behavior is of great scientific interest. In this paper, we present photometric data gathered from observatories in Crimea and Catalonia, highlighting the importance of systematic photometric studies of interstellar objects using meter-class telescopes. Our observations showed a steady increase in the comet’s brightness as it approached perihelion, likely due to the slow sublimation of ices. Over the five-month pre-perihelion observation period, we did not detect any significant changes in magnitude. The analysis of observations reveals a steady increase in comet 2I/Borisov brightness as it approached perihelion, likely due to the sublimation of ices, with no observable outbursts during the five-month pre-perihelion period. Additionally, we discuss the challenges in ground-based observation of comets posed by light pollution today, particularly in urban areas, where visual observations are severely limited. Using sample surface brightness measurements, we demonstrate the impact of light pollution and outline the importance of systematic photometric studies for interstellar objects.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 4","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10509-025-04424-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143749189","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":"Assessing the role of space weather indices in the prediction of total electron content at different latitudes during geomagnetic storms","authors":"Fei Xu,&nbsp;Dongjie Yue,&nbsp;Changzhi Zhai,&nbsp;Xin Gao,&nbsp;Yutian Chen","doi":"10.1007/s10509-025-04422-x","DOIUrl":"10.1007/s10509-025-04422-x","url":null,"abstract":"<div><p>The Total Electron Content (TEC) is an important parameter that describes the morphology and structure of the ionosphere. Deep learning is an important and effective tool for forecasting TEC, but the role of different solar activity indices and geomagnetic indices in TEC prediction remains unclear. The Long Short-Term Memory (LSTM) network has special structure design and good generalization ability, which is capable of learning the features of long-term sequence data and has been widely applied in the research of ionosphere prediction. Therefore, in this study, the LSTM network is used to achieve short-term forecasting of low, middle, and high latitudes TEC during geomagnetic storms that occurred in 2016. At the same time, the effects of four different index combinations, F10.7, Kp, Dst, and AE indices, on the prediction results at different latitudes were analyzed. The results show that the appropriate combination of index inputs effectively improves the prediction performance of the model. At low latitudes, the model incorporating Kp, Dst and F10.7 indices performed best, with a 51.3% average decrease in RMSE compared to the model without any additional indices. The best model is one that uses Kp and F10.7 indices at middle latitudes, compared to model without any indices, its average RMSE decreased by 57.0%. At high latitudes, the model using Kp, Dst, and AE indices performed best, with a 43.2% average decrease in RMSE compared to the model without any indices. However, more indices do not necessarily improve prediction accuracy.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 3","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143726611","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":"Karmarkar Bardeen anisotropic model for compact stars in (mathcal{F}(mathcal{R},mathcal{T})) gravity","authors":"Furqan Nazeer,&nbsp;Tooba Feroze","doi":"10.1007/s10509-025-04423-w","DOIUrl":"10.1007/s10509-025-04423-w","url":null,"abstract":"<div><p>This paper aims to obtain a new Class-I solution of the field equations in <span>(mathcal{F}(mathcal{R},mathcal{T}))</span> gravitational theory for the charged anisotropic spherically symmetric distribution. For this purpose, a new spacetime metric function is put forth and employed in the Karmarkar condition. The uniform charge distribution in the stellar interior is considered and the Class-I spacetime is seamlessly matched to Bardeen geometry at the boundary. Moreover, a detailed analysis is conducted to study the physical attributes of the stars Vela <i>X-1</i>, SMC <i>X-4</i>, SAX J<i>1808.4-3658</i>, Her <i>X-1</i> and Cen <i>X-3</i>, all obeying the essential conditions for a solution to be physically acceptable. A comprehensive review of stability criteria involving the energy conditions and adiabatic is provided complying with the requirement. In addition, an in-depth exploration of the Tolman-Oppenheimer-Volkoff’s (TOV) equation leads to the stellar configuration being in an equilibrium state.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 3","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143726610","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":"Design and analysis of abort orbits for manned missions to the Earth-Moon libration points","authors":"Yuebo Wang,&nbsp;Yamin Wang,&nbsp;Huichang Yu,&nbsp;Yonghe Zhang","doi":"10.1007/s10509-025-04421-y","DOIUrl":"10.1007/s10509-025-04421-y","url":null,"abstract":"<div><p>A libration-point orbit (LPO) offers low-cost access to space and may be the destination of future manned missions. Usually, a lunar flyby is required for short-term LPO missions, thus the transfer trajectory from the Earth to LPO is composed of an Earth–Moon two-body leg and a Moon–LPO three-body leg. The abort orbit associated with the Earth–Moon two-body leg has been thoroughly studied. In this paper, the abort orbit of the Moon–LPO three-body leg is designed and analyzed. Along the Moon–LPO three-body leg, the abort orbits of direct, lunar-flyby, and low-energy return are designed and discussed separately. For the direct return, the abort orbits are obtained based on an initial Kepler solution with reentry constraint. For the lunar-flyby return, the abort orbits are designed by pseudostate theory. For the low-energy return, the abort orbits are further optimized by introducing nontransit/transit orbits and lunar flyby. In the Earth–Lissajous transfer scenario, three types of abort orbits for the Moon–LPO three-body leg are numerically designed. For the direct or lunar-flyby return case, the total impulse of abort orbits is greater than 0.9 km/s. This is a significant burden for manned mission planning. For the low-energy return, the minimum total impulses are 0.302 km/s and save 20–60% total impulse at the cost of a limited increase in flight time. This abort orbit employs a nontransit/transit orbit to return to the vicinity of the Moon and quickly return to Earth after applying a second maneuver at perilune. Finally, return windows and trajectory types of abort orbits are classified based on a reference trajectory.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":"370 3","pages":""},"PeriodicalIF":1.8,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143716890","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}