New Astronomy最新文献

{"title":"Climate change impacts on ground-based solar astronomy: a case study Baikal Astrophysical Observatory, Eastern Siberia","authors":"Lidiia Bolbasova","doi":"10.1016/j.newast.2026.102518","DOIUrl":"10.1016/j.newast.2026.102518","url":null,"abstract":"<div><div>The ground-based solar telescopes are designed to reveal details of the Sun's surface, magnetic field, and plasma, which could help predict space weather and solar flares. The best resolution images of the Sun and spectral data offer great promise for how much we can learn about the Sun, our closest star. The quality of images from ground-based telescopes is determined by Earth's atmosphere. Adaptive optics systems are designed to obtain high-resolution images, but their effectiveness depends on atmospheric conditions. Climate changes, including anthropogenic impacts in the atmosphere, affect ground-based astronomy through changes in atmospheric conditions at the astronomical site. The present study investigated the long-term atmospheric parameters at the Baikal Astrophysical Observatory, Eastern Siberia, as a solar astronomical site. The non-parametric Sen’s slope and Mann-Kendall test are used to test the significance of trends.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"124 ","pages":"Article 102518"},"PeriodicalIF":2.1,"publicationDate":"2026-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145925272","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":"First photometric and orbital-period studies of the near-contact binary V0609 Aur","authors":"Yu Tan ,&nbsp;Pei-Ru Wu ,&nbsp;Zi-Bin Meng ,&nbsp;Yun-Xia Yu ,&nbsp;Ke Hu ,&nbsp;Fu-Yuan Xiang","doi":"10.1016/j.newast.2025.102512","DOIUrl":"10.1016/j.newast.2025.102512","url":null,"abstract":"<div><div>Near-contact binaries, recognized as the evolutionary bridge between detached binaries and contact systems, are critical targets for advancing our understanding of the formation and evolution of contact binaries. In this paper, we present the first photometric and orbital period analysis for the near-contact binary V0609 Aur. The light-curve solutions, derived from our ground-based multiple-band observations and TESS wide-band photometry, indicate that V0609 Aur is a non-thermal equilibrium and geometrically contact binary, characterized by an extremely low contact degree (<span><math><mrow><mi>f</mi><mo>=</mo><mn>3</mn><mo>.</mo><mn>27</mn><mtext>%</mtext></mrow></math></span>) and a substantial temperature difference (<span><math><mrow><mi>Δ</mi><mi>T</mi><mo>≃</mo><mn>2300</mn></mrow></math></span> K). The asymmetric light curves are well reproduced by modeling a hot spot on the secondary component. Orbital period investigation reveal that the orbital period of V0609 Aur is undergoing a long-term decrease at a rate of <span><math><mrow><mover><mrow><mi>P</mi></mrow><mrow><mo>̇</mo></mrow></mover><mo>=</mo><mo>−</mo><mn>1</mn><mo>.</mo><mn>25</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup></mrow></math></span> <span><math><mrow><mi>d</mi><mspace></mspace><msup><mrow><mi>yr</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>. This secular period decrease is likely driven by mass transfer from the more massive primary to the less massive secondary. By integrating the Roche-lobe model, the orbital period decrease, and thermal relaxation oscillation theory, we infer that V0609 Aur is evolving from the shallow contact phase toward the over-contact state.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"124 ","pages":"Article 102512"},"PeriodicalIF":2.1,"publicationDate":"2026-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145790662","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":"Magnetic Rossby waves under the generalized β-plane approximation","authors":"YuXin Wang,&nbsp;ShuWen Song,&nbsp;Jing Yu,&nbsp;Hui Liu,&nbsp;Jian Song","doi":"10.1016/j.newast.2025.102517","DOIUrl":"10.1016/j.newast.2025.102517","url":null,"abstract":"<div><div>Through linearization of the quasi-geostrophic shallow-water magnetohydrodynamic (QG-SWMHD) equations in a non-uniform background, this study investigates the energy dispersion dynamics of magnetic Rossby waves. The energy propagation follows a curved trajectory traced by wave packets moving along the group velocity direction. Asymmetric turning points occur when the meridional group velocity vanishes while the meridional wavenumber remains non-zero, whereas symmetric turning points arise when both the meridional wavenumber and group velocity simultaneously approach zero. The critical location corresponds to the asymptotic position of the ray where the meridional wavenumber becomes infinite. When a ray propagates between two symmetric turning points, it undergoes successive reflections between them, forming a waveform pattern; this zone is defined as the waveguide (WG) region. As the ray approaches its pivotal point, the magnetic Rossby wave smoothly transitions into a corresponding Alfvn wave, preserving energy continuitya region termed the energy dispersion (ED) zone. Furthermore, due to the presence of non-uniformly distributed transition points, a mixed (MX) region emerges, in which the ray exhibits hybrid characteristics of both WG and ED regions. The ED region reflects a general mechanism through which magnetic Rossby waves exchange energy with the background state characterized by <span><math><mrow><mi>β</mi><mrow><mo>(</mo><mi>y</mi><mo>)</mo></mrow></mrow></math></span>, thereby enabling mutual interactions.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"124 ","pages":"Article 102517"},"PeriodicalIF":2.1,"publicationDate":"2026-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145925271","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":"Cosmological dynamics of barrow holographic dark energy in f(G) gravity: An analytical and observational approach","authors":"A.Y. Shaikh ,&nbsp;A.P. Jenekar","doi":"10.1016/j.newast.2025.102497","DOIUrl":"10.1016/j.newast.2025.102497","url":null,"abstract":"<div><div>The presented study prioritizes the exploration of the cosmic model that integrates Barrow holographic dark energy (BHDE) within the confines of <span><math><mrow><mi>f</mi><mo>(</mo><mi>G</mi><mo>)</mo></mrow></math></span> gravity. The study proposes to resolve the field equations of the cosmic model by incorporating the temporal deceleration parameter (DP) in relation to the scale factor. We assessed the model's predictability using a Bayesian MCMC approach that draws on late-time cosmic observations, comprising 58 data values, and the SN Ia pantheon datasets involving 1048 data values, along with their combination, to set bounds around the free parameters. The Hubble threshold applies as an infrared (IR) threshold in the inspection of the BHDE. We thoroughly study the kinematical and physical aspects of the model. Our findings establish a seamless advance of the cosmos, moving from a decelerating era in earlier times to an accelerating era in both the immediate as well as distant future, as revealed by the trajectories of the equation of state <span><math><mrow><mo>(</mo><msub><mi>ω</mi><mi>b</mi></msub><mo>)</mo></mrow></math></span>, deceleration <span><math><mrow><mo>(</mo><mi>q</mi><mo>)</mo></mrow></math></span>, jerk <span><math><mrow><mo>(</mo><mi>j</mi><mo>)</mo></mrow></math></span>, snap <span><math><mrow><mo>(</mo><mi>s</mi><mo>)</mo></mrow></math></span>, and lerk <span><math><mrow><mo>(</mo><mi>l</mi><mo>)</mo></mrow></math></span> parameters. We investigate the phase diagnostics via statefinder and <span><math><mrow><mi>O</mi><mi>m</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math></span> analysis. The insight of energy conditions (ECs) further substantiates the predominance of BHDE following a speeding up Universe, while the model’s stability is predicted by the parameter of squared speed of sound. We concluded that our study's results comply with existing observational evidence, proving that our model demonstrates an effective alternative interpretation for the Universe's observed acceleration by accurately capturing the emergence of energy components while preserving stability.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102497"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520882","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":"Absolute parameters of the southern detached eclipsing binary DG Mic","authors":"Derya Sürgit ,&nbsp;Mücahit Kuz ,&nbsp;Volkan Bakış ,&nbsp;Chris Engelbrecht ,&nbsp;Fred Marang","doi":"10.1016/j.newast.2025.102496","DOIUrl":"10.1016/j.newast.2025.102496","url":null,"abstract":"<div><div>As part of an ongoing programme of observing detached eclipsing binary stars in the southern sky, we present the first analysis of spectroscopic observations of the Algol-type binary system DG Mic. A spectroscopic analysis of mid-resolution spectra allowed us to constrain the effective temperature of the primary component and to test the consistency of the system parameters with its spectral energy distribution (SED). Combined solutions of mid-resolution spectra and TESS, ASAS and WASP light curves imply a system of two almost identical components (<span><math><mi>q</mi></math></span> = 0.99) in circular orbits. Our final model shows that the system is a detached binary star. The masses and radii of the primary and secondary components of DG Mic were derived to be 1.65(<span><math><mo>±</mo></math></span>0.12) M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, 1.64(<span><math><mo>±</mo></math></span>0.18) M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> and 1.63(<span><math><mo>±</mo></math></span>0.10) R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, 1.91(<span><math><mo>±</mo></math></span>0.13) R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, respectively. According to Geneva evolution models, both components of the system are main-sequence stars and their age is approximately 713 Myr.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102496"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520916","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":"Probing dust and PAH chemistry in evolved carbon-rich nebulae through optical and infrared observations","authors":"Rahul Kumar Anand ,&nbsp;Atul Kumar Singh ,&nbsp;Saurabh Sharma ,&nbsp;Brijesh Kumar ,&nbsp;Shantanu Rastogi","doi":"10.1016/j.newast.2025.102494","DOIUrl":"10.1016/j.newast.2025.102494","url":null,"abstract":"<div><div>This study presents optical and near-infrared photometric observations, alongside mid-infrared spectroscopic data from the ISO SWS instrument, to examine potential correlations between Aromatic Infrared Band (AIB) features and the optical properties of carbon-rich evolved stars. Identifying such correlations can provide valuable constraints on the evolutionary pathways of low- to intermediate-mass stars beyond the asymptotic giant branch (AGB) phase. Photometric measurements in the U, B, V, R, I, J, H, K, and L bands were obtained for five well-known carbon-rich objects at various post-AGB or planetary nebula (PN) stages: CRL 2688, PN M 2-43, NGC 7027, BD<span><math><mrow><mo>+</mo><mn>3</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span>3639, and AFGL 2132. Our analysis reveals that all five objects exhibit prominent AIB features; however, their spectral profiles show notable variation. These differences are attributed to variations in the chemical composition and physical conditions of the surrounding circumstellar material. In particular, the <span><math><mrow><mn>3</mn><mo>.</mo><mn>28</mn><mspace></mspace><mi>μ</mi><mi>m</mi></mrow></math></span> polycyclic aromatic hydrocarbon (PAH) feature is detected in all objects except AFGL 2132, indicating a potentially distinct PAH population or environmental condition in its vicinity. Although these sources share broadly similar evolutionary stages, the observed diversity in AIB characteristics underscores the complexity and heterogeneity of their circumstellar environments.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102494"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520958","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":"Investigating star formation scenarios in the Milky Way using YSO distributions—A pilot study","authors":"Annarien G. Headley ,&nbsp;James O. Chibueze","doi":"10.1016/j.newast.2025.102482","DOIUrl":"10.1016/j.newast.2025.102482","url":null,"abstract":"<div><div>We investigated the distributions of classified young stellar object (YSO) in nine star-forming regions associated with <span>Hii</span> regions, namely Sh2-22, Sh2-19, Sh2-17, M16, M8, IC5070, Sh2-252, NGC2467 and M42, as a means of exploring the star formation scenarios (triggered or spontaneous) in the various regions. The YSO distributions of nine regions along the galactic longitudes and across different spiral arms were explored. It is noted that Sh2-22 and Sh2-19 may have evidence of localized triggered star formation, whereas Sh2-17 may be a spontaneous star forming region. The results showed that the location within the Milky Way may influence localized triggered star formation within individual regions. There is strong evidence that there are fewer older stars (Transition Disks) within the Outer regions of the Galaxy (<span><math><mrow><mn>2</mn><mo>.</mo><mn>91</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>74</mn><mtext>%</mtext></mrow></math></span>), accompanied by a higher number of Class I (<span><math><mrow><mn>32</mn><mo>.</mo><mn>49</mn><mo>±</mo><mn>10</mn><mo>.</mo><mn>77</mn><mtext>%</mtext></mrow></math></span>). This is different from the Inner Galactic regions where the Transition Disks are higher (<span><math><mrow><mn>32</mn><mo>.</mo><mn>93</mn><mo>±</mo><mn>13</mn><mo>.</mo><mn>78</mn><mtext>%</mtext></mrow></math></span>) as compared to low Class I sources (<span><math><mrow><mn>11</mn><mo>.</mo><mn>01</mn><mo>±</mo><mn>4</mn><mo>.</mo><mn>81</mn><mtext>%</mtext></mrow></math></span>). The number of Class II stars is relatively high and increases from the Inner regions (<span><math><mrow><mn>52</mn><mo>.</mo><mn>64</mn><mo>±</mo><mn>10</mn><mo>.</mo><mn>07</mn><mtext>%</mtext></mrow></math></span>) to Outer regions (<span><math><mrow><mn>64</mn><mo>.</mo><mn>54</mn><mo>±</mo><mn>11</mn><mo>.</mo><mn>09</mn><mtext>%</mtext></mrow></math></span>). These nine star-forming regions are not an accurate representation of locations throughout the Galaxy and the results may be biased.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102482"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520959","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":"Insights on gas distribution and dynamics in massive proto-cluster G358.46−0.39: Possible multiplicity in G358.46−0.39 MM1a","authors":"Chukwuebuka J. Ugwu ,&nbsp;James O. Chibueze ,&nbsp;Willice O. Obonyo ,&nbsp;Mavis Seidu","doi":"10.1016/j.newast.2025.102498","DOIUrl":"10.1016/j.newast.2025.102498","url":null,"abstract":"<div><div>This work explored the spatial distribution of C¹⁷O, SiO, HC₃N and SO₂ molecules, as well as the energetics of outflows in G358.46<span><math><mo>−</mo></math></span>0.39 proto-cluster using ALMA band 7 archival data, with the aim of providing an improved understanding of its protostellar nature, gas kinematics and dynamics. G358.46<span><math><mo>−</mo></math></span>0.39 is previously known to consist of 4 dust continuum cores (MM1a, MM1b, MM1c and MM2). The integrated intensity map of C¹⁷O reveals filamentary and dumbbell-shaped structures that are probably compressed gases from the expansion of the HII region MM2. The SiO emission reveals spatially overlapped blue and red outflow lobes, likely driven by an unresolved young stellar object (YSO) in MM1a. The spatial distribution of HC₃N and SO₂ molecules in MM1a shows a compact morphology, with no detectable HC₃N and SO₂ emissions in the other cores. The SO₂ emission reveals a clear velocity gradient in MM1a, as well as large velocity dispersion (<span><math><mo>∼</mo></math></span> 3<!--> <!-->km<!--> <!-->s<span><math><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math></span>) within the inner core of MM1a, which are consistent with rotating structures. We estimated the mass, momentum and energy outflow rate, as well as other outflow parameters. The SiO outflow exhibits a different morphology compared to the ¹²CO outflow morphology previously observed in MM1a. The SiO and ¹²CO outflows are probably associated with disks of separate cores with one face-on and the other edge-on, pointing to multiplicity of YSOs in MM1a. The properties of MM1a indicate that it is a massive protostar that is actively accreting and undergoing star formation.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102498"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145618207","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A systematic north-south asymmetry in the steady-state climate of rapidly-rotating oblique water worlds","authors":"Yiqi Wu (吴艺琪) ,&nbsp;Simon Portegies Zwart ,&nbsp;Henk A. Dijkstra","doi":"10.1016/j.newast.2025.102483","DOIUrl":"10.1016/j.newast.2025.102483","url":null,"abstract":"<div><div>Planetary obliquity (axial tilt) plays an important role in regulating the climate evolution and habitability of water-covered planets. Despite the suspicion of large obliquities in several exoplanetary systems, this phenomenon remains hard to observe directly.</div><div>We aimed to study the effect of mass, obliquity, and rotation on the steady state climate of water-covered planets. We simulated the climate evolution of such planets with varying obliquities, rotational speed, and mass using a general circulation model (GCM) of intermediate complexity, assuming aqua-planet configurations.</div><div>High obliquity supports an asymmetry between the equilibrium climatological conditions in the northern and southern hemispheres. The polar temperature ratio deviates further from unity with increasing obliquity and rotation rate. Cloud coverage patterns also shift with obliquity, displaying distinct latitudinal bands and increased cloudiness in the warmer hemisphere.</div><div>The climate of habitable-zone aqua-planets turns out to be sensitive to changes in obliquity and rotation rate, but are independent of planet mass. Our results highlight the importance of considering these factors when assessing the surface conditions of exoplanets. As a consequence, surface condition asymmetries in water-world exo-planets can be used to infer the planet’s obliquity and rotation rate.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102483"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145420229","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":"Low-frequency observations of low-mass binary systems with neutron star candidates","authors":"Elena Brylyakova ,&nbsp;Marina Afonina ,&nbsp;Gayane Tyul’basheva ,&nbsp;Sergei B. Popov ,&nbsp;Sergei Tyul’bashev","doi":"10.1016/j.newast.2025.102500","DOIUrl":"10.1016/j.newast.2025.102500","url":null,"abstract":"<div><div>Recently, astrometric and spectroscopic observations resulted in the discovery of several low-mass binaries with invisible components, which are expected to be compact objects. In about two dozen cases, the masses of these components are consistent with neutron stars. We use low-frequency archival data obtained with the Large Phased Array in Pushchino to search for radio emission from five of these systems. For all the systems, we do not detect persistent or periodic emission. In one case (2MASS J1527+3536), we identify a single radio burst with a flux of 13 Jy and a duration of 0.13 s. However, the dispersion measure of the burst does not correspond to an expected value for the source. We discuss several possibilities to explain the properties of this burst.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102500"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520957","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}