Astronomy Reports最新文献

Dynamics of the Elliptic Sitnikov Problem under Kite Configuration 风筝构型下椭圆Sitnikov问题的动力学

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S106377292560030X

M. Shahbaz Ullah, M. Javed Idrisi

{"title":"Dynamics of the Elliptic Sitnikov Problem under Kite Configuration","authors":"M. Shahbaz Ullah, M. Javed Idrisi","doi":"10.1134/S106377292560030X","DOIUrl":"10.1134/S106377292560030X","url":null,"abstract":"In this manuscript, we explore the elliptic Sitnikov problem to elliptic Sitnikov kite problem within the framework of Newtonian mechanics, where four massive masses occupy the vertices of a kite and move along elliptical orbits around their common center of mass. An infinitesimal particle is constrained to oscillate along the (zeta )-axis, perpendicular to the orbital plane of the primary masses and passing through the center of mass (O). The primary aim of this study is to investigate how reflected radiation, or albedo effects, influence the dynamics of an infinitesimal mass within this problem. The influence of key physical parameters including the albedo factor (alpha ) and orbital eccentricity (e) on the dynamical behavior of the system is explored using time series analysis, first return map (FRM), families of periodic orbits, and Newton–Raphson basins of convergence (N–R BoC). Numerical simulations reveal that increasing (alpha ) enhances the stability and persistence of periodic oscillations, while increasing (e) leads to complex transitions, including quasi-periodic and chaotic behaviors. The convergence analysis using Newton–Raphson schemes highlights the sensitivity of initial conditions and the fractal nature of the phase space. These findings provide new insights into the long-term stability and complexity of celestial systems influenced by radiation and geometrical configurations.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1396 - 1406"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579325","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}

引用次数: 0

Period Change of the Binary System WR + O V444 Cyg: Updated Ephemeris Formula 双星系统WR + O V444 Cyg的周期变化：更新的星历公式

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702403

I. I. Antokhin

引用次数: 0

Rotating Polytropic Twins and the Fragmentation Problem 旋转多向孪晶与破碎问题

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772926700034

V. E. Valiulin, K. V. Manukovskiy, T. L. Razinkova, A. V. Yudin

引用次数: 0

Old Open Clusters NGC 188 and M 67 in Gaia DR3 盖亚DR3中的旧疏散星团NGC 188和m67

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702488

A. F. Seleznev, M. V. Kulesh

{"title":"Old Open Clusters NGC 188 and M 67 in Gaia DR3","authors":"A. F. Seleznev, M. V. Kulesh","doi":"10.1134/S1063772925702488","DOIUrl":"10.1134/S1063772925702488","url":null,"abstract":"We performed a statistical study of two old open clusters NGC 188 and M 67 using Gaia DR3 data. No tidal tails of the clusters were detected, which most likely had been destroyed when the cluster passed through the Galactic plane. The size estimates of the clusters depend on the range of astrometric parameters and stellar magnitudes of the stars used for star counts. The mass spectra of two clusters differ significantly. NGC 188 shows a deficit of low-mass stars compared to M 67. In the halo region of NGC 188 (compared to the core region of the cluster), there is a relative excess of the low-mass stars (just as in the case of M 67) and a deficit of stars in the mass range from 0.66 to 0.9 solar masses. Comparison with the Hunt and Reffert samples showed that almost all the stars from these samples are contained among the stars we selected for counting. Moreover, the group probability of these stars belonging to clusters, estimated by the uniform field method, is higher than 60%. It is shown that the velocity dispersion of single stars (selected according to the {stellar magnitude–color index} diagrams) is significantly smaller than the velocity dispersion of unresolved binary stars. The work is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1241 - 1259"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579321","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}

引用次数: 0

AS 357 Is a New Symbiotic Star AS 357是一颗新的共生恒星

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702440

M. A. Maslennikova, A. M. Tatarnikov, A. A. Tatarnikova, A. V. Dodin, B. S. Safonov

引用次数: 0

Kinematics of Brown Dwarfs in the Solar Vicinity 太阳附近褐矮星的运动学

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702452

E. S. Postnikova, M. D. Sizova, T. Bugra Keskin, N. V. Chupina, S. V. Vereshchagin

引用次数: 0

Pulsar Emission Recorders of Low-Frequency Radio Telescopes at the PRAO ASC LPI PRAO ASC LPI低频射电望远镜脉冲星发射记录仪

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772926700058

S. V. Logvinenko

引用次数: 0

Investigation of Long-Period Eclipsing Binaries: Absolute Parameters and the Evolutionary Status of the V891 Mon System 长周期食双星的研究：V891星系统的绝对参数和演化状态

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702427

A. Yu. Kniazev, O. Yu. Malkov, L. N. Berdnikov, I. Yu. Katkov

{"title":"Investigation of Long-Period Eclipsing Binaries: Absolute Parameters and the Evolutionary Status of the V891 Mon System","authors":"A. Yu. Kniazev, O. Yu. Malkov, L. N. Berdnikov, I. Yu. Katkov","doi":"10.1134/S1063772925702427","DOIUrl":"10.1134/S1063772925702427","url":null,"abstract":"In this paper, we present the results of a study of a long-period eclipsing binary system V891 Mon having a period of (P = {31.42050^d}). The presented study is based on spectral data obtained during 2020–2022 on the echelle spectrograph HRS of the SALT telescope and TESS photometric data. The constructed radial velocity curve is based on 11 spectra covering all phases of this binary system. The orbital parameters of this binary system have been determined for the first time. The constructed model for the light curve according to TESS data converges with an accuracy of 0.01%. The effective temperatures of both components, their rotational velocities, as well as the metallicity of the system and the interstellar reddening value are directly determined from the spectra. Our analysis of photometric and spectral data allowed us to directly calculate the luminosities of both components, their radii and masses with accuracy of less than one percent. A comparison with the evolutionary tracks shows that the age of the system is 325 Myr, component A has already left the main sequence (MS), and component B is still on MS. Both components are not synchronized, and the system is not circularized. The kinematic characteristics, together with the metallicity determined in this work, indicate that the V891 Mon system is a typical representative of the “kinematically cold” component of a thin disk, which is consistent with its evolutionary status as a young system. Despite the large eccentricity, the orbit of the system is oriented to the line of sight in such a way that it can only be determined using spectral data. The work is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1326 - 1341"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579218","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}

引用次数: 0

Minimal Model of Supernova Neutrino Distribution Function Taking into Account Neutrino Halo 考虑中微子晕的超新星中微子分布函数最小模型

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772926700083

A. A. Dobrynina, E. A. Koptyaeva, I. S. Ognev

{"title":"Minimal Model of Supernova Neutrino Distribution Function Taking into Account Neutrino Halo","authors":"A. A. Dobrynina, E. A. Koptyaeva, I. S. Ognev","doi":"10.1134/S1063772926700083","DOIUrl":"10.1134/S1063772926700083","url":null,"abstract":"The paper examines the possibility of analytically approximating the neutrino distribution function in a core-collapse supernova. A minimal model of this distribution function, dependent on four parameters, was constructed. Three approximations of the spectral and angular neutrino distributions within the model are considered. The parameters of these approximations were obtained using the results of numerical simulations of Prometheus-Vertex code. Analysis of their accuracy made it possible to construct two neutrino distribution functions with higher accuracy, respectively, inside and outside of the protoneutron star. This model was extended by adding to the main neutrino radiation a contribution from a neutrino halo, which appears in the supernova in the region behind the shock wave. Its minimal model required the introduction of two additional parameters for the overall distribution function in this part of the supernova. Based on the results obtained for a minimal model of the neutrino distribution function in the supernova envelope, radial fits of its parameters, including parameters of neutrino halo, were obtained. An attempt was made to find a correlation of these parameters with the characteristic spatial scales of the supernova. Within this problem, a fairly complete set of these quantities was calculated. Analysis of their correlation with the radial approximation of neutrino parameters was performed. An expression for the distribution of main neutrino emission in the supernova envelope was obtained as a function of luminosity, neutrino average energy, and the radii of the protoneutron star core and the neutrinosphere for electron neutrinos. The contribution of the neutrino halo is presented as a function of the shock wave position and the obtained coefficient of halo amplitude, which depends on the supernova model.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1442 - 1461"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579326","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}

引用次数: 0

On the Possibility of Eliminating the Time Parallax Effect in Registration of Moving Objects on CMOS Matrices in Rolling Shutter Mode 滚动快门模式下CMOS矩阵运动目标配准中消除时间视差效应的可能性

IF 0.7 4区物理与天体物理

Astronomy Reports Pub Date : 2026-04-01 DOI: 10.1134/S1063772925702464

M. E. Prokhorov, A. I. Zakharov, N. L. Kroussanova, V. G. Moshkalev, M. S. Tuchin

引用次数: 0