New Astronomy最新文献

{"title":"Gravitational instability in Plummer sphere profile: A Jeans analysis","authors":"Abdelhakim Benkrane","doi":"10.1016/j.newast.2025.102493","DOIUrl":"10.1016/j.newast.2025.102493","url":null,"abstract":"<div><div>We investigate the gravitational instability of self-gravitating systems characterized by the Plummer sphere profile. Using Jeans analysis, we derive modified expressions for the Jeans mass and Jeans radius, revealing that the presence of the Plummer radius <span><math><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> increases both critical parameters, thereby suppressing gravitational collapse. In the classical regime, we obtain a modified dispersion relation incorporating the Fourier transform of the Plummer potential. Our results show that <span><math><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> reduces the growth rate of perturbations and shifts the critical wavenumber to lower values, favoring the development of instability at longer wavelengths. We also extend the analysis to the quantum regime, where quantum pressure introduces a stabilizing <span><math><msup><mrow><mi>k</mi></mrow><mrow><mn>4</mn></mrow></msup></math></span>-term in the dispersion relation. We find that at large wave numbers, quantum effects dominate and the influence of the <span><math><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> becomes negligible. These findings highlight the role of Plummer sphere profile in modulating the onset and scale of gravitational collapse, with implications for star formation and structure formation in dark matter (DM)-rich environments.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102493"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145469089","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":"Stellar kinematics of the Milky Way Galaxy in post-Newtonian gravity","authors":"Shubhen BISWAS","doi":"10.1016/j.newast.2025.102499","DOIUrl":"10.1016/j.newast.2025.102499","url":null,"abstract":"<div><div>The recent Gaia data confirm that the Milky Way’s outer stellar disk shows a tangible Keplerian decline in rotation curve. The data also reveal that the stellar velocity maintains a positive correlation with the surface gravity. These revelations present scope for revisiting our understanding of galactic stellar dynamics. Herein, we use the recent interaction model over the post-Newtonian theory of gravity to study celestial dynamics considering the stellar body as an extended object rather than a point particle in space. By jointly considering the central super massive black hole and galactic stellar disk, a rotating stellar body around this combination is theoretically modeled as a two-body system. The model predicts a galactocentric solar rotational speed of <span><math><mrow><mn>226</mn><mspace></mspace><mtext>km</mtext><mo>.</mo><mspace></mspace><msup><mrow><mi>s</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span> for the Milky Way, consistent with the observations.</div><div>Classification codes: 04.00; 95.10.Ce</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102499"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520883","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":"Calibrating machine learning with multi-band photometry: Resolving parameter degeneracies in contact binary NSVS 4803568","authors":"Xu-Zhi Li ,&nbsp;Xue-Tong Liu ,&nbsp;Wei Liu ,&nbsp;Xu-Dong Zhang","doi":"10.1016/j.newast.2025.102484","DOIUrl":"10.1016/j.newast.2025.102484","url":null,"abstract":"<div><div>Contact binary stars are crucial for studying stellar evolution and merger events, but precise determination of their physical parameters (mass ratio <span><math><mi>q</mi></math></span>, inclination <span><math><mi>i</mi></math></span>, fill-out factor <span><math><mi>f</mi></math></span>) is challenging. While large-scale, single-band surveys coupled with machine learning enable rapid population studies, discrepancies arise between solutions derived from such automated pipelines due to inherent degeneracies and limited wavelength constraints. In this work, we resolve the conflicting parameters reported for contact binary system NSVS 4803568 through comprehensive multi-band photometric observations. We conducted follow-up <span><math><mi>B</mi></math></span>, <span><math><mi>V</mi></math></span>, <span><math><mi>R</mi></math></span>, and <span><math><mi>I</mi></math></span>-band observations and analyzed the light curves using PHOEBE, refined via Markov Chain Monte Carlo. Our solution confirms the system as a W-subtype contact binary and reveals a significant third-light contribution. The parameter inconsistencies between single-band studies highlight limitations in machine learning training data sensitivity and the need for multi-dimensional flux constraints. We advocate a hybrid approach: machine learning pre-screening of survey data to identify high-priority targets (e.g., extreme <span><math><mi>q</mi></math></span> or short period systems) followed by multi-band validation to calibrate models and mitigate systematic errors. This synergy is essential for unlocking the full potential of astronomical big data in stellar astrophysics.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102484"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145469090","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":"Analysis of the effect of bars on environmental dependence of disc galaxies with MaNGA survey data","authors":"Pius Privatus ,&nbsp;Umananda Dev Goswami","doi":"10.1016/j.newast.2025.102492","DOIUrl":"10.1016/j.newast.2025.102492","url":null,"abstract":"<div><div>Bars are fundamental structures in disc galaxies, although their role in galaxy evolution is still not fully known. This study investigates the effect of the presence of bars on the environmental dependence of disc galaxies’ properties using the volume-limited sample from Mapping Nearby Galaxies at APO (MaNGA) survey. The disc galaxies with and without bars samples were obtained using the Galaxy Zoo 2 project then assigned into isolated and non-isolated sub-samples. These sub-samples were used to compare the stellar mass, star formation rate, <span><math><mrow><mi>g</mi><mo>−</mo><mi>r</mi></mrow></math></span> colour, concentration index and gas phase metallicity, and their relationships between isolated and non-isolated environments. Then these are used to investigate if there is an existence of any difference between galaxies with and without bars. A one-to-one correspondence between isolated and non-isolated galaxy properties was observed, and a strong dependence on the environment for properties of unbarred galaxies was observed when compared to barred. The stellar mass against star formation rate, <span><math><mrow><mi>g</mi><mo>−</mo><mi>r</mi></mrow></math></span> colour against concentration index and stellar mass against gas phase metallicity of unbarred galaxies strongly depend on environment while for barred these relations weakly depend on environment. The study concludes that bars in disc galaxies decrease the dependence of analysed properties and their relations on the environment.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102492"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145469125","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":"Statistical analysis of eclipsing binaries with monotonic orbital-period variations: A-type W UMa contact systems","authors":"Shinjirou Kouzuma","doi":"10.1016/j.newast.2025.102495","DOIUrl":"10.1016/j.newast.2025.102495","url":null,"abstract":"<div><div>On the basis of monotonic orbital-period variations, this study aims to identify genuine relationships between binary parameters and the rates of mass transfer (MT), mass loss (ML), and angular momentum loss (AML). Sample binaries with monotonic period variations are collected from the literature, together with well-determined binary parameters. Assuming the monotonic variations are responsible for any one of the MT, ML, and AML, their rates are calculated with the rates of change of period. After selecting crucial parameters using partial least-squares analysis, a parameter that exhibits the closest correlation with any one of the derived rates is further selected using partial regression plots. Moreover, power-law relationships are found for the discovered correlations. The properties of the sample binaries are also investigated by examining associations between binary parameters. In the systems with negative period variations, it is found that the rate of MT from more- to less-massive stars is a function of the primary radius; the AML rate is a function of the fill-out factor. In addition, the relationships between the mass ratio and stellar masses indicate that the ML rate relative to the MT rate decreases with increasing mass ratio below <span><math><mrow><mo>∼</mo><mn>0</mn><mo>.</mo><mn>46</mn></mrow></math></span>. Meanwhile, in the systems with positive variations, it is found that the rate of MT from less- to more-massive stars is a function of the luminosity ratio and/or mass ratio; the ML rate is a function of the secondary temperature. The discussion also addresses possible processes occurring in the sample binaries.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102495"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145520956","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":"Modelling the scattering by porous aggregate dust grains in the Far-Ultraviolet halos of Spica and Achernar","authors":"Nilanjana Dey Choudhury ,&nbsp;P. Shalima ,&nbsp;Keerthana U. ,&nbsp;J. Murthy","doi":"10.1016/j.newast.2025.102485","DOIUrl":"10.1016/j.newast.2025.102485","url":null,"abstract":"<div><div>Far-Ultraviolet (FUV) halos have been detected around six bright stars by Murthy and Henry (2011) using GALEX observations. These halos are thought to be caused by forward scattering of the starlight by dust grains present in thin foreground clouds. The optical constants of grains producing such halos have been constrained earlier by using a single scattering model, that considered the Henyey-Greenstein empirical phase function instead of theoretical phase functions for the scattering grains. In this work, we have modelled the FUV halos for two stars, Spica and Achernar, by considering the realistic porous aggregates of different sizes and compositions. As the Henyey-Greenstein phase function is known to deviate from theoretical predictions, we have utilized theoretical scattering phase functions for modelling. The dust is placed in a double-layered plane-parallel sheet with its distance and optical depth varied to get the best fit. We find that the halo intensities are dominated by scattering due to <span><math><mrow><mn>0</mn><mo>.</mo><mn>05</mn><mspace></mspace><mi>μ</mi><mi>m</mi></mrow></math></span> sized porous dust aggregates made of amorphous silicate and carbonaceous aggregates for Spica and Achernar, respectively. We find that the medium in front of Achernar has a lower optical depth (<span><math><mi>τ</mi></math></span>) of 0.032 compared to Spica which has a value of <span><math><mi>τ</mi></math></span> = 0.1. This low value is close to the optical depth of the local ISM (0.01) within 40 pc of the Sun. This study demonstrates an effective method to constrain the dust grain properties in the local interstellar medium.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"123 ","pages":"Article 102485"},"PeriodicalIF":2.1,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145420230","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":"Near-IR spectroscopy of the gravitationally lensed quasar PS J0147+4630","authors":"Luis J. Goicoechea ,&nbsp;Vyacheslav N. Shalyapin","doi":"10.1016/j.newast.2025.102479","DOIUrl":"10.1016/j.newast.2025.102479","url":null,"abstract":"<div><div>The quadruply-imaged gravitationally lensed quasar PS J0147+4630 at redshift <span><math><mrow><mi>z</mi><mo>&gt;</mo></mrow></math></span> 2 is a good candidate for time delay cosmography and microlensing-based source structure studies. In this paper, new spectra of its four images are derived from archive data of two 10-m class telescopes. We focus on the unexplored near-IR spectral region including the Mg<!--> <span>ii</span>, H<span><math><mi>β</mi></math></span>, [O<!--> <span>iii</span>] and H<span><math><mi>α</mi></math></span> emission lines (0.9<span><math><mrow><mo>−</mo><mn>2</mn><mo>.</mo><mn>4</mn><mspace></mspace><mi>μ</mi><mi>m</mi></mrow></math></span>), and measure image flux ratios for the emission lines and their underlying continua, as well as a reliable quasar redshift of 2.357 ± 0.002. We also find evidence of an outflow in the H<span><math><mi>α</mi></math></span> emission and estimate a quasar black-hole logarithmic mass <span><math><mrow><mo>log</mo><mfenced><mrow><msub><mrow><mi>M</mi></mrow><mrow><mi>BH</mi></mrow></msub><mo>/</mo><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></mfenced></mrow></math></span> = 9.34 ± 0.30.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"122 ","pages":"Article 102479"},"PeriodicalIF":2.1,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145227244","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 detection of ethylene oxide and acetaldehyde in hot core G358.93–0.03 MM1: Tracing prebiotic oxygen chemistry","authors":"Arijit Manna,&nbsp;Sabyasachi Pal","doi":"10.1016/j.newast.2025.102465","DOIUrl":"10.1016/j.newast.2025.102465","url":null,"abstract":"<div><div>Ethylene oxide (c- <figure><img></figure> ) and its isomer, acetaldehyde (CH₃CHO), are important complex organic molecules owing to their potential role in the formation of amino acids (R–CH(NH₂)-COOH) in interstellar medium. The detection of c- <figure><img></figure> in hot molecular cores suggests the possible existence of larger ring-shaped molecules containing more than three carbon atoms, such as furan (c- <figure><img></figure> ), which shares structural similarities with ribose (C₅H₁₀O₅), the sugar component of DNA. In this study, we report the first detection of the rotational emission lines of c- <figure><img></figure> and CH₃CHO towards the hot molecular core G358.93–0.03 MM1, based on observations from the Atacama Large Millimeter/Submillimeter Array (ALMA) in band 7. The fractional abundances of c- <figure><img></figure> and CH₃CHO relative to H₂ are <span><math><mrow><mrow><mo>(</mo><mn>2</mn><mo>.</mo><mn>1</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>2</mn><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>9</mn></mrow></msup></mrow></math></span> and <span><math><mrow><mrow><mo>(</mo><mn>7</mn><mo>.</mo><mn>1</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>9</mn><mo>)</mo></mrow><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>9</mn></mrow></msup></mrow></math></span>, respectively. The column density ratio between CH₃CHO and c- <figure><img></figure> is <span><math><mrow><mn>3</mn><mo>.</mo><mn>4</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>7</mn></mrow></math></span>. A Pearson correlation heat map reveals strong positive correlations (<span><math><mi>r</mi></math></span> <span><math><mo>&gt;</mo></math></span> 0.5) between the abundances and excitation temperatures of c- <figure><img></figure> and CH₃CHO, suggesting a possible chemical connection between those two molecules. To investigate this further, we conducted a two-phase warm-up chemical model using the gas-grain chemical code UCLCHEM. A comparison between our derived abundances and the predictions from our chemical model and existence model demonstrates good agreement within factors of 0.73 and 0.74, respectively. We propose that c- <figure><img></figure> may form in G358.93–0.03 MM1 via the grain surface reaction between C₂H₄ and O, but CH₃CHO may be produced through the surface reaction between CH₃ and HCO.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"122 ","pages":"Article 102465"},"PeriodicalIF":2.1,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144934279","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":"Photometric studies of the Short-period Eclipsing Binary J075102.16+342405.3 and CP Psc","authors":"Lin-yan Jiang ,&nbsp;Li-yun Zhang ,&nbsp;Xianming L. Han ,&nbsp;Prabhakar Misra ,&nbsp;Josh Wanninger ,&nbsp;Hong-peng Lu ,&nbsp;Qing-Feng Pi ,&nbsp;Jun-Tao Wan","doi":"10.1016/j.newast.2025.102478","DOIUrl":"10.1016/j.newast.2025.102478","url":null,"abstract":"&lt;div&gt;&lt;div&gt;We obtained new light curves of two eclipsing binaries 1SWASP J075102.16+342405.3 and CP Psc on eleven nights from 2013 to 2017 using two optical telescopes. We analyzed the orbital period variation using all collected minima, including our eleven new minima. We found that the periods of the systems J075102 and CP Psc are increasing at rates of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mover&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;̇&lt;/mo&gt;&lt;/mrow&gt;&lt;/mover&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;55&lt;/mn&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;7&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; days/yr and &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mover&gt;&lt;mrow&gt;&lt;mi&gt;p&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;̇&lt;/mo&gt;&lt;/mrow&gt;&lt;/mover&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;mn&gt;6&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;32&lt;/mn&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mn&gt;8&lt;/mn&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;8&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; days/yr, respectively. Subsequently, we updated the orbital parameters of J075102 using the Wilson–Devinney program and obtained the orbital parameters of CP Psc for the first time. The result shows that J075102 is an contact binary with the contact factor of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;28&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;64&lt;/mn&gt;&lt;mrow&gt;&lt;mo&gt;(&lt;/mo&gt;&lt;mo&gt;±&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;03&lt;/mn&gt;&lt;mo&gt;)&lt;/mo&gt;&lt;/mrow&gt;&lt;mtext&gt;%&lt;/mtext&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, the mass ratio &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;q&lt;/mi&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; of 1.9, the mass as &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;766&lt;/mn&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;⊙&lt;/mo&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;459&lt;/mn&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;⊙&lt;/mo&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, the mass transfer from the secondary component to the primary component of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mover&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;̇&lt;/mo&gt;&lt;/mrow&gt;&lt;/mover&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;2&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;6&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;59&lt;/mn&gt;&lt;mo&gt;×&lt;/mo&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;−&lt;/mo&gt;&lt;mn&gt;7&lt;/mn&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;⊙&lt;/mo&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;/&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;y&lt;/mi&gt;&lt;mi&gt;e&lt;/mi&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;. For CP Psc, we conducted a simultaneous analysis of our light curves and spectroscopic observations obtained by LAMOST. The spectral type determined by the LAMOST stellar spectra survey was approximately G3. The results indicate that it is a detached binary star system composed of &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;=&lt;/mo&gt;&lt;mn&gt;0&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;940&lt;/mn&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;M&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;⊙&lt;/mo&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; and &lt;spa","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"122 ","pages":"Article 102478"},"PeriodicalIF":2.1,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145267106","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":"Solar energetic particle transport via the heliospheric current sheet: Evidence of a ground-level response on All Saints Day, 2014","authors":"Marcel Nogueira de Oliveira ,&nbsp;Carlos E. Navia ,&nbsp;Andre Asevedo Nepomuceno","doi":"10.1016/j.newast.2025.102468","DOIUrl":"10.1016/j.newast.2025.102468","url":null,"abstract":"<div><div>We investigate the physical mechanisms responsible for the solar energetic particle (SEP) event observed on 1 November 2014, during which several ground-based detectors in both hemispheres, specifically those located on the sunlit western side of Earth, recorded simultaneous enhancements in counting rates. The event is attributed to Active Region (AR) 2192, one of the most active sunspot groups of Solar Cycle 24, which at the time was situated near the western limb of the solar disk, approaching the far side of the Sun. A plausible scenario involves a combination of solar eruptive activity, particle acceleration by a shock wave driven by a coronal mass ejection (CME), and the presence of a heliospheric current sheet (HCS) sector crossing, which may have enhanced magnetic connectivity between the Sun and Earth. We emphasize data from the New-Tupi muon detector, operating in scaler mode and located near the central region of the South Atlantic Anomaly (SAA). The particle excess detected on 1 November 2014 by ground-based instruments spanning different rigidity regimes, in conjunction with satellite observations, indicates that the signal was not a localized phenomenon. Assuming a power-law energy spectrum for the SEP population, we find that its high-energy tail in the GeV range is consistent with proton flux measurements reported by GOES-13. We present and discuss the details of these observations.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"122 ","pages":"Article 102468"},"PeriodicalIF":2.1,"publicationDate":"2026-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144934278","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}