New Astronomy最新文献

{"title":"V455 Car: An oscillating eclipsing Algol-type binary in triple star system","authors":"Zhao-Long Deng ,&nbsp;Wen-Ping Liao ,&nbsp;Li-Ying Zhu ,&nbsp;Xiang-Dong Shi ,&nbsp;Nian-Ping Liu ,&nbsp;Ping Li","doi":"10.1016/j.newast.2025.102412","DOIUrl":"10.1016/j.newast.2025.102412","url":null,"abstract":"<div><div>V455 Car is a southern oscillating eclipsing Algol-type system with an orbital period of 5.132888 days. Our first photometric solutions based on the Transiting Exoplanet Survey Satellite indicate that it is a semi-detached binary with the secondary star is almost filling its Roche lobe. The noticeable O’Connell effect in light curve could be explained by hot spot on the primary component, which may be attributed to the mass transfer from the secondary component to the primary one. The absolute parameters are determined as: <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>5</mn><mo>.</mo><mn>30</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>10</mn><mspace></mspace></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>3</mn><mo>.</mo><mn>17</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>22</mn><mspace></mspace></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> for the primary, and <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>58</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>32</mn><mspace></mspace></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>6</mn><mo>.</mo><mn>66</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>46</mn><mspace></mspace></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span> for the secondary. <strong>Based on <em>O − C</em> analysis, we find a periodic variation of</strong> <span><math><mrow><msub><mrow><mi>P</mi></mrow><mrow><mn>3</mn></mrow></msub><mo>=</mo><mn>26</mn><mo>.</mo><mn>62</mn></mrow></math></span> (<span><math><mrow><mo>±</mo><mn>1</mn><mo>.</mo><mn>66</mn></mrow></math></span>), <span><math><mrow><mi>y</mi><mi>r</mi></mrow></math></span>. <strong>The periodic oscillation suggests a possible third body with a minimal mass of</strong> <span><math><mrow><mn>0</mn><mo>.</mo><mn>59</mn><mrow><mo>(</mo><mo>±</mo><mn>0</mn><mo>.</mo><mn>13</mn><mo>)</mo></mrow><mspace></mspace></mrow></math></span> <strong>M</strong><span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. It is speculated that the secondary star has undergone a longer evolution, leading to a mass ratio reversal being experienced in the binary system. Our frequency analysis finds that the primary of V455 Car may be an SPB/SLF star. This study reports a novel example of an oscillating eclipsing Algol-type system featuring an SPB/SLF primary star and a red giant star, which suggest that strong observational results for a high incidence of third bodies in massive binaries.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102412"},"PeriodicalIF":1.9,"publicationDate":"2025-04-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143859409","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":"Few EURONEAR NEA mini-surveys observed with the INT, KASI and T80S telescopes during the ParaSOL synthetic tracking project","authors":"O. Vaduvescu ,&nbsp;M. Stanescu ,&nbsp;M. Popescu ,&nbsp;M. Predatu ,&nbsp;L. Curelaru ,&nbsp;D. Bertesteanu ,&nbsp;C. Boldea ,&nbsp;F. Ursache ,&nbsp;C. Fotin ,&nbsp;C. de la Fuente Marcos ,&nbsp;R. de la Fuente Marcos ,&nbsp;E. Unda-Sanzana ,&nbsp;F. Barwell ,&nbsp;K. Jhass ,&nbsp;S. Shenoy ,&nbsp;A. Santos-Garcia ,&nbsp;J. Bishop ,&nbsp;J. Munday ,&nbsp;J. de Leon ,&nbsp;C.-U. Lee ,&nbsp;C. Mendes de Oliveira","doi":"10.1016/j.newast.2025.102410","DOIUrl":"10.1016/j.newast.2025.102410","url":null,"abstract":"<div><div>The modern synthetic tracking technique (ST) can make use of small and medium-sized telescopes to detect asteroids fainter than the classic blinking methods, by arbitrary shifting and co-adding more images of the same survey field, if GPU computing resources are available. In the framework of the Romanian ParaSOL project, we developed and tested an innovative ST algorithm capable of detecting in near-real-time very faint near-Earth asteroids (NEAs), which likely became the first ST pipeline developed in Europe. To test our pipeline, we conducted several mini-surveys using three large-field telescopes, namely the ING’s INT, the Korean KASI and the Brazilian T80S telescopes. Most images were processed using our <em>Umbrella Image Processing Pipeline</em> (IPP) module. The ST search was conducted using our <em>Synthetic Tracking via Umbrella</em> (STU) module and the commercial <em>Tycho Tracker</em> software, which allowed to compare and complement the findings. The source validation was supported by reducers using our new <em>Webrella</em> platform. Most of the nights were reduced in near-real-time, demonstrating the ability to process, sort, and report large volumes of data. We discovered 5 credited and 4 one-night NEAs, co-discovered other 3 NEAs and recovered 3 poorly known NEAs. We flagged 59 NEA candidates for recovery and orbital classification, discovering, co-discovering and recovering other 18 orbitally related NEAs, additionally improving the orbits of 23,428 known asteroids and reporting 1,374 unknown objects. A comparison between ST and traditional blinking detection using the new EURONEAR tool <em>MagLim</em> shows improvements of two magnitudes and a two-fold increase in the number of detections. A preliminary comparison between STU and Tycho shows that STU detects about 70% of Tycho findings, however STU detects rapid objects much faster than Tycho, 7 NEAs with speeds between 2-10<span><math><msup><mrow></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup></math></span>/min being found exclusively by STU. Based on our surveys, we assessed the current NEA discovery rate using 1-2-m class telescopes and ST methods, finding that one NEA candidate can be discovered in every 9-12 square degrees up to magnitude <span><math><mrow><mo>∼</mo><mn>23</mn></mrow></math></span>.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102410"},"PeriodicalIF":1.9,"publicationDate":"2025-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143843971","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":"Superstatistics and stellar rotation: Modeling velocity distributions in six stellar groups","authors":"Mahsa Iranmanesh ,&nbsp;Hamid Arjomand Kermani ,&nbsp;Kamel Ourabah","doi":"10.1016/j.newast.2025.102408","DOIUrl":"10.1016/j.newast.2025.102408","url":null,"abstract":"<div><div>In the present study, we investigate the observed distribution of the projected rotational velocity for six different stellar groups: young-type and late-type (including the spectral classes F, G, and K), OB-type, A-type, B-type, and M-type. Our analysis shows that the distribution of projected rotational velocities for these stellar groups deviates from a Maxwellian distribution. Instead, it is better captured by a generalized statistical mechanics framework known as superstatistics. Within this framework, the distribution is modeled as a superposition of a locally Maxwellian distribution, whose width fluctuates over a large spatiotemporal scale according to a <span><math><msup><mrow><mi>χ</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> distribution. We identify a correlation between the mean rotational velocity and the parameters defining the distribution, specifically the number of degrees of freedom contributing to the fluctuations. This dependency highlights the intricate relationship between the rotational dynamics and the generalized statistical mechanics properties of stellar systems.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102408"},"PeriodicalIF":1.9,"publicationDate":"2025-04-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143829860","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 numerical scheme to obtain periodic three-body orbits with finite angular momentum","authors":"Xiaoming Li ,&nbsp;Yueyan Tao ,&nbsp;Xiaochen Li ,&nbsp;Shijun Liao","doi":"10.1016/j.newast.2025.102407","DOIUrl":"10.1016/j.newast.2025.102407","url":null,"abstract":"<div><div>The three-body problem is ubiquitous in various physical systems. Thousands of periodic orbits for the three-body problem with zero angular momentum were obtained in recent years. In this paper, we present a numerical scheme to obtain periodic orbits for the three-body problem with finite angular momentum. The proposed approach combines a continuation method and the Newton–Raphson method, which are implemented using Clean Numerical Simulation (CNS) for the integration of the equations of motion. The figure-eight periodic orbit and another newly found periodic orbit are taken to generate periodic orbits by continuously varying the angular momentum. The linear stability of these periodic orbits are investigated through Floquet theory. It is suggested that angular momentum plays a significant role in influencing the linear instability of periodic orbits. Our proposed numerical approach inspires the further research in the intricate dependence of the periodic orbits on the angular momentum, providing a powerful tool for investigating the nonlinear dynamics of the three-body problem.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102407"},"PeriodicalIF":1.9,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143738329","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":"TESS light curves and period changes in low-mass eclipsing binary BB Persei","authors":"Marek Wolf ,&nbsp;Petr Zasche ,&nbsp;Miloslav Zejda ,&nbsp;Martin Mašek ,&nbsp;Andrej Mudray ,&nbsp;Hana Kučáková ,&nbsp;Waldemar Ogłoza ,&nbsp;Jaroslav Merc ,&nbsp;Jan Kára ,&nbsp;Vojtěch Dienstbier","doi":"10.1016/j.newast.2025.102406","DOIUrl":"10.1016/j.newast.2025.102406","url":null,"abstract":"<div><div>We present a detailed analysis of the low-mass detached eclipsing binary system BB Persei, which contains two K-type stars in a circular orbit with a short period of 0.4856 d. We used light curves from the Transiting Exoplanet Survey Satellite (<span>Tess</span>), which observed BB Per in five sectors, to determine its photometric properties and a precise orbital ephemeris. The solution of the <span>Tess</span> light curve in <span>Phoebe</span> results in a detached configuration, where the temperature of the primary component was fixed to <span><math><mrow><msub><mrow><mi>T</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>5</mn><mspace></mspace><mn>300</mn></mrow></math></span> K according to <span>Lamost</span>, which gives us <span><math><mrow><msub><mrow><mi>T</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>5</mn><mspace></mspace><mn>050</mn><mo>±</mo><mn>50</mn></mrow></math></span> K for the secondary. The spectral type of the primary component was derived as K0 and the photometric mass ratio was estimated <span><math><mrow><mi>q</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>90</mn></mrow></math></span>. Slow period changes on the current O-C diagram spanning the past 25 years indicate the presence of a third body orbiting the eclipsing pair with an orbital period of about 22 years. The companion could be a red dwarf of spectral type M6–M7 with a minimal mass of about 0.1 M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. The characteristics and temporal variation of the dark region on the surface of the secondary component were estimated.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102406"},"PeriodicalIF":1.9,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143686669","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 young stellar cluster towards IRAS 03523+5343","authors":"João L. Yun ,&nbsp;Pedro M. Martins ,&nbsp;Gorka Zubiri-Elso ,&nbsp;Anlaug Amanda Djupvik","doi":"10.1016/j.newast.2025.102405","DOIUrl":"10.1016/j.newast.2025.102405","url":null,"abstract":"<div><div>We present a study of the star formation occurring in the most active region of a molecular cloud in the second quadrant of the (outer) Galaxy towards IRAS 03523+5343. Near-infrared <span><math><mrow><mi>J</mi><mi>H</mi><msub><mrow><mi>K</mi></mrow><mrow><mi>S</mi></mrow></msub></mrow></math></span> images and <span><math><mi>K</mi></math></span>-band spectroscopy were obtained with NOTCam at the Nordic Optical Telescope at the Roque de Los Muchachos Observatory. Mid-infrared <em>WISE</em> satellite images and submm <em>JCMT/SCUBA-2</em> catalogue sources were also explored. In addition, millimetre line CS spectra were obtained with the Yebes 40 m telescope.</div><div>Within the region of the molecular cloud covered by our CS <span><math><mrow><mo>(</mo><mi>J</mi><mo>=</mo><mn>1</mn><mo>−</mo><mn>0</mn><mo>)</mo></mrow></math></span> maps, the line is strong and extends over all the mapped region of <span><math><mrow><mn>3</mn><mo>.</mo><msup><mrow><mn>7</mn></mrow><mrow><mo>′</mo></mrow></msup><mo>×</mo><mn>3</mn><mo>.</mo><msup><mrow><mn>7</mn></mrow><mrow><mo>′</mo></mrow></msup></mrow></math></span>. This high-density molecular gas defines a molecular core exhibiting an angular size FWHM of about <span><math><msup><mrow><mn>1</mn></mrow><mrow><mo>′</mo></mrow></msup></math></span> (0.7 pc at 2.4 kpc distance). We estimate a lower limit to the mass of the molecular gas in this region to be about 995 <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. A SCUBA-2 core was detected with an estimated total mass of 250 <span><math><msub><mrow><mi>M</mi></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>.</div><div>We identify a young stellar cluster with a few hundred sources with colours compatible to YSOs at the location of a strong enhancement of the stellar density coincident with the IRAS position. The main counterpart of the IRAS source is a very red and bright source with radio jets likely to be a high-mass young stellar object. A second bright source is a Herbig Be candidate source displaying a blue nebula with a morphology that suggests the dissipation of a collimated flow.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102405"},"PeriodicalIF":1.9,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143643107","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":"CCD photometric studies of two Primitive C-type main-belt asteroids: (51) Nemausa and (52) Europa","authors":"Shuang Wang,&nbsp;Yuangui Yang,&nbsp;Huiyu Yuan,&nbsp;Ligang Yu","doi":"10.1016/j.newast.2025.102391","DOIUrl":"10.1016/j.newast.2025.102391","url":null,"abstract":"<div><div>We present new CCD photometry for primitive C-type main-belt asteroids (51) Nemausa and (52) Europa performed on several nights of 2016, by using the 60-cm telescope at Xinglong station of NAOC. From our new data, the rotation periods are determined as 7.784840 h for (51) Nemausa and 5.629960 h for (52) Europa. Based on the convex inversion method, the pole ambiguity was removed, and we refined pole directions and triaxial ratios as follows, (168 °, <span><math><mrow><mo>−</mo><mn>6</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>∘</mo></mrow></msup></mrow></math></span>) with <span><math><mrow><mi>a</mi><mo>/</mo><mi>b</mi><mo>=</mo><mn>1</mn><mo>.</mo><mn>09</mn></mrow></math></span> and <span><math><mrow><mi>b</mi><mo>/</mo><mi>c</mi><mo>=</mo><mn>1</mn><mo>.</mo><mn>03</mn></mrow></math></span> for (51) Nemausa, and a pole is derived as (256°, 32°) with <span><math><mrow><mi>a</mi><mo>/</mo><mi>b</mi><mo>=</mo><mn>1</mn><mo>.</mo><mn>04</mn></mrow></math></span> and <span><math><mrow><mi>b</mi><mo>/</mo><mi>c</mi><mo>=</mo><mn>1</mn><mo>.</mo><mn>33</mn></mrow></math></span> for (52) Europa. From the parameters of 49 asteroids, a statistic study was carried out. All these results will help us to understand the physical properties of pristine small objects in the solar system.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102391"},"PeriodicalIF":1.9,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143636413","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":"Anisotropic compact stellar models under the condition of zero complexity","authors":"Shyam Das ,&nbsp;Saibal Ray ,&nbsp;Amit Das ,&nbsp;Shyamal Kumar Pal","doi":"10.1016/j.newast.2025.102393","DOIUrl":"10.1016/j.newast.2025.102393","url":null,"abstract":"<div><div>In this article, we introduce a new exact solution of the Einstein field equations that characterizes static, spherically symmetric anisotropic compact stars. In our approach the solution of the system of field equations have been obtained under the constraint of vanishing complexity, in addition to specifying the metric potential corresponding to the <span><math><msub><mrow><mi>g</mi></mrow><mrow><mi>r</mi><mi>r</mi></mrow></msub></math></span> component. The class of generalized solutions has been smoothly matched with the Schwarzschild solutions describing the exterior across the boundary. The model parameters are fixed by using this matching conditions and additionally from the condition of the vanishing of the radial pressure at the surface. We have employed recent measurements of the mass and radius from the observed pulsars to validate and justify the physical applicability of our model.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102393"},"PeriodicalIF":1.9,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143636414","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 role of Finsler-Randers geometry in shaping anisotropic metrics and thermodynamic properties in black holes theory","authors":"J Praveen,&nbsp;S K Narasimhamurthy","doi":"10.1016/j.newast.2025.102404","DOIUrl":"10.1016/j.newast.2025.102404","url":null,"abstract":"<div><div>In this research paper, we delve into the study of black hole (BH) structure within the context of Finsler geometry, a novel approach not previously explored by other researchers. We focused on developing the Finsler-Randers metric tensor for black holes, with the aid of the Barthel connection along with the osculating Riemannian method. This newly derived metric demonstrates significant departures from the conventional black hole metrics found in General Relativity (GR) by the presence of Finslerian term <span><math><mi>η</mi></math></span>, thereby shedding new light on the geometry and nature of black holes. To comprehensively understand the characteristics of black holes, we calculated the metric components under both vacuum and non-vacuum conditions. Our findings indicate that the metric structure aligns well with the known Riemannian limits, reinforcing the compatibility of our model with established theories. Moreover, we extended our analysis to include the thermodynamics of black holes in a Finslerian framework in brief. The results from this exploration affirm that the fundamental laws of black hole thermodynamics remain valid, reinforcing the viability and consistency of our Finslerian model. This study not only contributes to our understanding of black hole physics but also opens new avenues for further research in the realm of Finsler geometry and its implications for astrophysics<strong>.</strong></div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102404"},"PeriodicalIF":1.9,"publicationDate":"2025-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143643106","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":"Evolution of neutron stars in wide eccentric low-mass binary systems","authors":"Marina Afonina ,&nbsp;Sergei Popov","doi":"10.1016/j.newast.2025.102401","DOIUrl":"10.1016/j.newast.2025.102401","url":null,"abstract":"<div><div>Precise astrometric measurement with <em>Gaia</em> satellite resulted in the discovery of tens of wide binary systems consisting of a Sun-like star and an invisible component. The latter can be a white dwarf, a neutron star, or a black hole. In this paper, we model magneto-rotational evolution of neutron stars in wide low-mass binaries accounting for the orbital eccentricity. We aim to calculate when neutron stars in such systems can start to accrete matter from the stellar wind of the companion. We show that the transition from the ejector to the propeller stage occurs earlier in more eccentric systems, thus increasing the time that neutron stars can spend accreting matter. Our calculations show that in the case of efficient spin-down at the propeller stage, a neutron star in an eccentric orbit with <span><math><mrow><mi>e</mi><mo>≳</mo><mn>0</mn><mo>.</mo><mn>6</mn></mrow></math></span> and a standard magnetic field <span><math><mrow><mi>B</mi><mo>=</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>12</mn></mrow></msup></mrow></math></span> G can start accreting within a few Gyr. For neutron stars with <span><math><mrow><mi>B</mi><mo>=</mo><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>13</mn></mrow></msup></mrow></math></span> G the onset of accretion occurs earlier regardless of the orbital eccentricity. Otherwise, with a lower spin-down rate, such a neutron star will remain at the propeller stage for most of its life.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"119 ","pages":"Article 102401"},"PeriodicalIF":1.9,"publicationDate":"2025-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143631794","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}