New Astronomy最新文献

{"title":"Orbital period study of two contact W UMa-type contact binaries: V551 Dra and CN Hyi","authors":"Xuan-Qi Tang , Chao-Yue Li , Lin-Qiao Jiang , Jie Wei , Jie Zheng , Kai Huang , Jia-Xing Wang , Hao-Yi Yang , Jing-Zhou Li , Xiao-Man Tian , Jian-Hui Yang","doi":"10.1016/j.newast.2025.102357","DOIUrl":"10.1016/j.newast.2025.102357","url":null,"abstract":"<div><div>V551 Dra and CN Hyi are both W UMa-type contact binaries. Basing on TESS data, we conduct analyses of their orbital period variations. The results indicate that the O - C curve of V551 Dra shows a long-term upward trend, with <span><math><mrow><mi>d</mi><mi>P</mi><mo>/</mo><mi>d</mi><mi>t</mi><mo>=</mo><mn>2</mn><mo>.</mo><mn>80</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>7</mn></mrow></msup><mi>d</mi><mi>a</mi><mi>y</mi><mi>⋅</mi><mi>y</mi><mi>e</mi><mi>a</mi><msup><mrow><mi>r</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>, which could be attributed to mass transfer from the less massive component to the more massive one. Additionally, a periodic variation with an amplitude of <span><math><mrow><mi>A</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>000954</mn><mi>d</mi><mi>a</mi><mi>y</mi><mi>s</mi></mrow></math></span> and a period of <span><math><mrow><mi>P</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>31</mn><mi>y</mi><mi>e</mi><mi>a</mi><mi>r</mi><mi>s</mi></mrow></math></span> was superimposed. The periodic variation in the orbital period may be due to the light-travel time effect caused by a third body. We estimate the minimum mass of the third body to be <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>48</mn><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>. The primary of V551 Dra, although less massive, is oversized and overluminous compared to standard mainsequence stars, suggesting it has evolved through substantial mass loss, while the more massive secondary remains on the main sequence, indicating a stable mass transfer phase. In contrast, The O - C curve of CN Hyi exhibits a long-term decreasing trend, with <span><math><mrow><mi>d</mi><mi>P</mi><mo>/</mo><mi>d</mi><mi>t</mi><mo>=</mo><mo>−</mo><mn>1</mn><mo>.</mo><mn>09</mn><mo>×</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup><mi>d</mi><mi>a</mi><mi>y</mi><mi>⋅</mi><mi>y</mi><mi>e</mi><mi>a</mi><msup><mrow><mi>r</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>. Due to the intermediate contact nature of the binary system, this long-term period decrease is likely to be caused by mass transfer from the more massive primary star to the less massive secondary star. The primary of CN Hyi resides on the main sequence, while the oversized and overluminous secondary suggests significant material accretion. These findings suggest differing evolutionary pathways for W-subtype and A-subtype contact binaries. V551 Dra appears to exhibit stable mass transfer dynamics, whereas CN Hyi may potentially experience more dynamic structural changes as it evolves. In addition to these evolutionary considerations, we hypothesize that the period variation of CN Hyi may also be attributed by the light-travel time effect of a third body, given the common occurrence of third bodies in contact systems. Considering","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102357"},"PeriodicalIF":1.9,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153394","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 the halo occupation distribution for moderate X-ray luminosity active galactic nuclei in the EAGLE cosmological simulation","authors":"Liliana Altamirano-Dévora ,&nbsp;Héctor Aceves ,&nbsp;Angel Castro ,&nbsp;Takamitsu Miyaji","doi":"10.1016/j.newast.2025.102361","DOIUrl":"10.1016/j.newast.2025.102361","url":null,"abstract":"<div><div>The hydrodynamical cosmological simulation <em>EAGLE</em> is used to model the Halo Occupation Distribution (HOD) of moderate X-ray luminosity active galactic nuclei (mXAGN), extending previous work using only dark matter simulations and empirical relations. By examining mergers as a triggering mechanism, we focus on halos typical of galaxy groups and cluster-like systems with masses <span><math><mrow><mo>≥</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>12</mn><mo>.</mo><mn>75</mn></mrow></msup><mspace></mspace><mi>M</mi><mo>⊙</mo><mspace></mspace><msup><mrow><mi>h</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>. We analyze simulation data to create catalogs of central and satellite galaxies. We study their merger history we quantify the percentage of minor and major mergers in the mXAGN sample. We obtain the HOD for central and satellite mXAGN across a redshift interval from <span><math><mrow><mi>z</mi><mo>=</mo><mn>2</mn></mrow></math></span> to the present epoch. Our results indicate that, across most redshifts, minor mergers slightly predominate as the primary mechanism for triggering mXAGN.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102361"},"PeriodicalIF":1.9,"publicationDate":"2025-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153395","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":"Corrigendum to “Gravitational interaction signatures in isolated galaxy triplet systems: a photometric analysis” [New Astronomy, 2021,87, 101603]","authors":"Amira A. Tawfeek ,&nbsp;Kanak Saha ,&nbsp;Kaustubh Vaghmare ,&nbsp;A.K. Kembhavi ,&nbsp;Ali Takey ,&nbsp;Bernardo Cervantes-Sodi ,&nbsp;Jacopo Fritz ,&nbsp;Zainab Awad ,&nbsp;Gamal B. Ali ,&nbsp;Z.M. Hayman","doi":"10.1016/j.newast.2025.102359","DOIUrl":"10.1016/j.newast.2025.102359","url":null,"abstract":"","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102359"},"PeriodicalIF":1.9,"publicationDate":"2025-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143474367","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":"The first study of the short period contact binary GY Psc","authors":"Bin Zhang ,&nbsp;Yidan Gao","doi":"10.1016/j.newast.2025.102358","DOIUrl":"10.1016/j.newast.2025.102358","url":null,"abstract":"<div><div>In this paper, we present the first investigation of the short period eclipsing binary GY Psc. We find that GY Psc is a shallow W-subtype binary with a mass ratio of <span><math><mi>q</mi></math></span> = 2.522. We also find that its light curves show different O’Connell effect, which can be explained by the evolution of the cool star-spots. At the same time, the <span><math><mrow><mi>O</mi><mo>−</mo><mi>C</mi></mrow></math></span> diagram reveals a cyclic oscillation with a period of <span><math><mrow><mi>P</mi><mo>=</mo><mn>3</mn><mo>.</mo><mn>85</mn></mrow></math></span> years and an amplitude of 0.033883 days. The cyclic oscillation is interpreted as the light travel-time effect via the presence of a stellar black hole candidate. The minimum mass of the tertiary companion is estimated to be <span><math><msub><mrow><mi>M</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> = 12.99 <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. All the results reveal that GY Psc may be a triple system with active star-spot activity.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102358"},"PeriodicalIF":1.9,"publicationDate":"2025-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153390","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":"Galactic magnetic field and spiral arms against gas quenching due to Ram pressure","authors":"Meenu Prajapati,&nbsp;Mamta Gulati","doi":"10.1016/j.newast.2025.102356","DOIUrl":"10.1016/j.newast.2025.102356","url":null,"abstract":"<div><div>Interaction between the intracluster medium (ICM) and the interstellar medium (ISM) plays a crucial role in galaxy evolution. Surveys of galaxy clusters have shown that ram pressure stripping (RPS) is a dominant mechanism that removes the cold gas reservoir from cluster galaxies. We extend the analytical model for ram pressure stripping by Singh et al. (2019) to include asymmetries in the disc, such as spiral arms and regular magnetic fields along the spiral arms. Non-thermal pressure from magnetic fields acts against the ram pressure and leads to greater gas retention in galaxies. Our analytical modelling of spiral galaxies with magnetic fields shows that a strong magnetic field, with a strength of <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>5</mn></mrow></msup></mrow></math></span> G, significantly enhances gas retention at the centre of a galaxy as it approaches the core of a cluster, thereby suppressing the stripping rates. We find that magnetic fields stronger than <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup></mrow></math></span> G are critical for retaining gas all the way to the cluster centre. While both magnetic fields and galaxy mass contribute to the retention of gas, the influence of magnetic fields is particularly significant, especially in typical spiral galaxies where unusually high masses are not present. Our results may help in explaining why gas-rich galaxies can still be observed in dense cluster environments despite the strong stripping forces.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102356"},"PeriodicalIF":1.9,"publicationDate":"2025-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143152959","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":"Modified Chaplygin gas solutions of f(Q) theory of gravity","authors":"Bhupendra Kumar Shukla ,&nbsp;R.K. Tiwari ,&nbsp;A. Beesham ,&nbsp;Değer Sofuoğlu","doi":"10.1016/j.newast.2025.102355","DOIUrl":"10.1016/j.newast.2025.102355","url":null,"abstract":"<div><div>In this study, we investigate Modified Chaplygin gas solutions within the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> theory of gravity, a modified gravitational theory that seeks to address the limitations of the conventional Lambda cold dark matter model. <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity offers a novel perspective on cosmic dynamics by incorporating a non-minimal coupling between the geometry and the matter, allowing for a richer understanding of the expansion of the universe. We explore the implications of modified Chaplygin gas, characterized by its unique equation of state (eos), which transitions from a matter-dominated phase to a dark energy-dominated phase, thereby influencing the evolution of the energy density and pressure across cosmic redshifts. Our findings reveal significant insights into the interplay between different energy components, highlighting the transition from positive to negative pressure as a hallmark of the role of dark energy in driving the accelerated expansion of the universe. This research not only enhances our comprehension of cosmic evolution, but also provides a compelling framework for future investigations into the nature of dark energy and its impact on the ultimate fate of the universe.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102355"},"PeriodicalIF":1.9,"publicationDate":"2025-01-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153389","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 investigation of V517 Cam combined with ground-based and TESS data","authors":"Neslihan Alan ,&nbsp;Fahri Aliçavuş ,&nbsp;Mehmet Alpsoy","doi":"10.1016/j.newast.2025.102352","DOIUrl":"10.1016/j.newast.2025.102352","url":null,"abstract":"<div><div>The observations of eclipsing binary systems are of great importance in astrophysics, as they allow direct measurements of fundamental stellar parameters. By analysing high-quality space-based observations with ground-based photometric data, it becomes possible to detect these fundamental parameters with greater precision using multicolour photometry. Here, we report the first photometric analysis results of the V517 Cam eclipsing binary system by combining the Transiting Exoplanet Survey Satellite (<em>TESS</em>) light curve and new CCD observations in <em>BVRI</em> filters, obtained with a 60 cm robotic telescope (T60) at the TÜBİTAK National Observatory. By means of photometric analyses, the masses and radii of the primary and secondary stars were carefully determined to be <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>47</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>06</mn><mspace></mspace><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>, <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>79</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>05</mn><mspace></mspace><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>, and <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>43</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>03</mn><mspace></mspace><msub><mrow><mi>R</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>75</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>04</mn><mspace></mspace><msub><mrow><mi>R</mi></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>, respectively. Furthermore, the distance to V517 Cam was calculated to be <span><math><mrow><mn>284</mn><mo>±</mo><mn>20</mn></mrow></math></span> pc. The overall age of the system is estimated to be around <span><math><mrow><mn>63</mn><mo>±</mo><mn>15</mn></mrow></math></span> Myr. At this age, the primary component stands near the onset of its main-sequence evolution, near the ZAMS, whereas the secondary component remains in the pre-main-sequence evolutionary phase. To better understand the evolutionary status and nature of V517 Cam, the mass ratio and temperature values, obtained with relatively low sensitivity by photometric measurements, need to be confirmed by spectral analysis.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102352"},"PeriodicalIF":1.9,"publicationDate":"2025-01-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143152960","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":"Prediction of solar cycles 26 and 27 based on LSTM-FCN","authors":"Shuguang Zeng ,&nbsp;Shuo Zhu ,&nbsp;Yao Huang ,&nbsp;Xiangyun Zeng ,&nbsp;Sheng Zheng ,&nbsp;Linhua Deng","doi":"10.1016/j.newast.2025.102353","DOIUrl":"10.1016/j.newast.2025.102353","url":null,"abstract":"<div><div>Predicting solar activity changes is crucial for Earth’s climate, communication systems, and aerospace technology. This study employs the Long Short-Term Memory Fully Convolutional Network (LSTM-FCN) deep learning method to predict the amplitudes and peak times of Solar Cycles (SCs) 26 and 27 for both the entire solar disk and the northern and southern hemispheres. The experimental data comprises the monthly mean total Sunspot Number (SSN) data and the monthly mean northern and southern Hemispheric Sunspot Number (HSN) data, provided by the World Data Center — Sunspot Index and Long-term Solar Observations (WDC-SILSO). The experimental process tested the Input–Output Window Ratio (IOWR) from 4:1 to 14:1, and the results indicate that when the IOWR is 10:1, the normalized Relative RMSE (RRMSE) is minimized at 0.078. According to the prediction, SC 26 is expected to peak in June 2034 with an amplitude of 194.4, and SC 27 is expected to peak in July 2045 with an amplitude of 244.2. It was also found that SC 26 and SC 27 have northern and southern hemisphere asymmetry. This study demonstrates the potential application of the LSTM-FCN deep learning method in forecasting SCs, providing a new tool and approach for solar physics research.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"117 ","pages":"Article 102353"},"PeriodicalIF":1.9,"publicationDate":"2025-01-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143153391","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 distortion solution for the 1-m telescope at Yunnan Observatory and its application to the positional measurement of four main-belt asteroids Eugenia(45), Roma(472), Lundmarka(1334) and Autonoma(1465)","authors":"Na Wang ,&nbsp;Kai-Rui Liu ,&nbsp;Zheng-Yang Xue ,&nbsp;Biao-Biao Zhang ,&nbsp;Yi-Cheng Du","doi":"10.1016/j.newast.2024.102351","DOIUrl":"10.1016/j.newast.2024.102351","url":null,"abstract":"<div><div>Four main-belt asteroids Eugenia, Roma, Lundmarka and Autonoma were observed at Yunnan Observatory 1-m telescope in 2022–2023. A total of 66 CCD frames for the four asteroids are observed. In order to improve the astrometry, the geometric distortion (called GD hereafter) of the 1-m telescope is solved. After GD correction, the precision of Eugenia and Autonoma has improved significantly and the standard deviation of the (O-C) residuals is improved by a maximum of 20 mas. The theoretical position of the asteroid is retrieved from the Jet Propulsion Laboratory Horizons system. Our results show that the mean O-Cs(observed minus computed) of the residuals is better than 0.1 arcsec in each direction. The dispersion is better than 0.071 arcsec in each direction.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"116 ","pages":"Article 102351"},"PeriodicalIF":1.9,"publicationDate":"2025-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143095021","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":"Corrigendum to “A comprehensive study on the K2-type binary V1393 Tau in four-year observations” [Volume 115, NEASPA_102330]","authors":"Ligang Yu ,&nbsp;Shuang Wang ,&nbsp;Michel Raúl ,&nbsp;Liyun Zhang","doi":"10.1016/j.newast.2024.102350","DOIUrl":"10.1016/j.newast.2024.102350","url":null,"abstract":"","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"116 ","pages":"Article 102350"},"PeriodicalIF":1.9,"publicationDate":"2024-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143095022","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}