Astrophysical Bulletin最新文献

{"title":"OPTIMus—Survey of Massive Star-Forming Regions at Optical, Infrared, and Millimeter Wavelengths","authors":"M. S. Kirsanova,&nbsp;A. V. Moiseev,&nbsp;A. M. Tatarnikov,&nbsp;A. S. Gusev,&nbsp;A. D. Yarovova,&nbsp;D. S. Wiebe","doi":"10.1134/S199034132660016X","DOIUrl":"10.1134/S199034132660016X","url":null,"abstract":"<p>This work presents a description of the scientific goals and objectives of OPTIMus (OPTical, Infrared, Millimeter survey of massive star-forming regions), a survey of massive star-forming regions in the optical, infrared, and millimeter wavelengths. The survey is aimed at constructing a comprehensive characterization of the multicomponent and structurally complex interstellar medium in the vicinity of young massive stars combining both observational and theoretical aspects. Using multiwavelength observational data, we will reconstruct the three-dimensional structure and determine the physical parameters of H II regions, photodissociation regions, and the surrounding molecular clouds. The paper describes the observational data obtained with the 6-m BTA and Zeiss-1000 telescopes of the Special Astrophysical Observatory of the Russian Academy of Sciences, the 2.5-m telescope of the Caucasian Mountain Observatory of the Sternberg Astronomical Institute of Moscow State University, and the 20-m telescope of the Onsala Space Observatory.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 2","pages":"317 - 339"},"PeriodicalIF":1.0,"publicationDate":"2026-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148822973","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":"Start of Orbit Librations and the Bar Growth Timescale","authors":"E. N. Podzolkova,&nbsp;A. M. Melnik","doi":"10.1134/S1990341326600092","DOIUrl":"10.1134/S1990341326600092","url":null,"abstract":"<p>We study a dynamical model of the Galaxy with an analytical bar that reproduces the radial-velocity <span>(V_{R})</span> profiles as a function of the Galactocentric distance <span>(R)</span> obtained from the Gaia DR3 data. The model radial-velocity profiles show a periodic increase in <span>(V_{R})</span> caused by orbits trapped into libration near the outer Lindblad resonance (OLR). To determine the moment when the librations start, we built a set of additional models differing only in the bar growth time <span>(T_{g})</span>. The temporal dependences of the radial velocity <span>(V_{R}(t))</span> in the models with different <span>(T_{g})</span> retain their shape but are shifted relative to each other in time <span>(t)</span>. The shift providing the best agreement between the model dependences is proportional to <span>(T_{g})</span> with the coefficient <span>(k=0.54pm 0.02)</span>. Orbit librations start not when the bar reaches its full strength, but when it attains only 54<span>(%)</span> of its maximum strength. Since the maximum bar strength in the models is <span>(Q_{b}=0.314)</span>, the librations start when the bar strength reaches <span>(Q_{b}^{*}=0.170)</span>.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 2","pages":"291 - 302"},"PeriodicalIF":1.0,"publicationDate":"2026-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148823020","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":"Effect of Spitzer/IRAC Systematic Noises on Secondary Eclipses of the Exoplanet HD 209458 b","authors":"A. A. Fedotov,&nbsp;R. V. Baluev","doi":"10.1134/S1990341325600462","DOIUrl":"10.1134/S1990341325600462","url":null,"abstract":"<p>We analyze infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b obtained by Spitzer/IRAC in the 3.6 <span>(mu)</span>m channel. We find that in addition to the well-known effect of intra-pixel sensitivity variations, inducing quasiperiodic noise, these data also contain red noise which in turn consists of two subcomponents that differ by their correlation timescale, 10–20 s and 5–10 min. We also show that a global model of the intra-pixel sensitivity effect can be constructed such that it can fit all 13 light curves at once but uses only a few parameters (e.g., 12 or so). Finally, we tried to measure the systematic time shift of the exoplanetary secondary eclipse, which appeared consistent with zero, <span>(-4pm 40)</span> s. This corresponds to a spatial shift of <span>(0.007pm 0.060)</span> in units of planet radius, or to the orbital eccentricity <span>(ecosomega)</span> of <span>((-0.2pm 2.1)times 10^{-4})</span>.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 2","pages":"340 - 359"},"PeriodicalIF":1.0,"publicationDate":"2026-08-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148823024","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":"Does Intergalactic Clouds Fall Affect the Stellar Population of Galaxies?","authors":"N. A. Tikhonov,&nbsp;O. A. Galazutdinova,&nbsp;G. M. Karataeva","doi":"10.1134/S1990341325600449","DOIUrl":"10.1134/S1990341325600449","url":null,"abstract":"<p>Stellar photometry of 70 irregular galaxies was performed using archival Hubble Space Telescope images. The resulting Hertzsprung–Russell diagrams were used to distinguish the red supergiant and giant branches. The distances to the galaxies and the metallicity of the red giants were determined using the TRGB method. The <span>((V-I))</span> color index of the supergiant branch at the luminosity level <span>(M_{I}=-7overset{textrm{m}}{.}0)</span> was chosen as the metallicity index of red supergiants. The measurements showed that no galaxy exhibits a metallicity inversion between young and old stars, which would occur if clouds of the low-metallicity intergalactic gas fall onto the galaxy. This means that the infall of intergalactic clouds, if it occurred, did not significantly affect the evolution of the stellar population of galaxies over the past billions years. Over billions of years of evolution, each galaxy underwent random processes that could alter the metallicity of its interstellar medium and stars. However, the linear relationship we have found between the metallicities of young and old stars in galaxies of different masses indicates that the bulk of galaxies’ metal accumulation has occurred in the distant past. Modern processes are increasing the metallicity of galaxies but at a significantly slower rate than during galaxy formation. Otherwise, the linear relationship between the metallicities of stars of different ages in galaxies of different masses and star formation histories would not be observed.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"1 - 11"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021052","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":"Synchronization of Solar and Economic Activity Indices","authors":"D. R. Japaridze,&nbsp;T. Paatashvili,&nbsp;T. G. Mdzinarishvili,&nbsp;B. B. Chargeishvili","doi":"10.1134/S1990341322600260","DOIUrl":"10.1134/S1990341322600260","url":null,"abstract":"<p>Forecasts of economic indices are important for mitigating the risks of unexpected stresses in the global or local economy. However, the numerous factors that influence the resulting economic index create a complex picture that complicates determining a cyclical pattern. We studied the relationship between solar activity and the Dow Jones Industrial Average from 1896 to 2021. We used correlation and cross-correlation methods with a sliding time window and a wavelet coherency approach to analyze the data. The study revealed that the relationship between the events is not simple and evolves over time. Various synchronization periods, as well as variation in the coherence of these synchronizations over time, were identified. We discovered that the correlation with the 11-year periodicity is greater than 0.5 during the 1906–1936 and 1964–2000 time periods and is visible with a 95<span>(%)</span> confidence level during the 1910–1930 and 1990–1994 time periods. This correlation is supported by the found 95<span>(%)</span> confidence in the coherence between the cosmic ray data and the Dow Jones index during the same time periods (1964–2000), when the correlation between the sunspot number and this index is high, albeit with other phase differences. Furthermore, the correlation between the cosmic ray data and the Dow Jones is stronger. This could imply that the influence of solar activity on global economy fluctuations is mediated by the Sun’s modulation of cosmic rays.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"154 - 162"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021058","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":"Indicatives of Early Stages of Star Formation in the Universe","authors":"I. A. Acharova,&nbsp;M. E. Sharina","doi":"10.1134/S1990341326600055","DOIUrl":"10.1134/S1990341326600055","url":null,"abstract":"<p>The paper analyzes formation conditions for globular clusters (GCs) in circumgalactic clouds. The similarity between the metallicity distributions of GCs in the nearby Universe and of circumgalactic clouds is substantiated in detail over a wide range of redshifts: from 0.2 to 5.9. The distributions of the number of circumgalactic clouds and GCs both contain a sequence of four local maxima at the metallicity values: <span>([textrm{X/H}]simeq-2.6,-2.0,-1.4,-0.5)</span>. The sequential enrichment of a circumgalactic cloud with a mass of <span>(10^{8},M_{odot})</span> is calculated starting the extremely low metallicity <span>([textrm{X/H}]&lt;-2.3)</span>, then following through the stages of <span>(-2.3leq[textrm{X/H}]&lt;-1.7)</span> and <span>(-1.7leq[textrm{X/H}]&lt;-0.9)</span> to the high metallicity <span>([textrm{X/H}]geq-0.9)</span>, where the boundaries of these ranges coincide with the local minima of the number of objects in the distributions. It is shown that for the reproduction of such distributions, it is sufficient that at each stage of enrichment of a part of a cloud in metals, one or more GCs with a total mass of <span>(3times 10^{6},M_{odot})</span> are formed. It is shown that the maximum mass of stars capable of leading to supernova explosions increases with the increase of metallicity. Possible values of this mass are calculated for the metallicities corresponding to the maxima in the distributions of clouds and GCs.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"12 - 22"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021047","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":"Analytical Approaches to Modeling Thick Photon Rings","authors":"S. V. Chernov","doi":"10.1134/S1990341326600067","DOIUrl":"10.1134/S1990341326600067","url":null,"abstract":"<p>General relativity predicts the existence of an infinite number of nested photon rings around black holes, each containing information about the properties of curved space-time. In this paper, analytical models of a thick Gaussian asymmetric photon ring are developed and the visibility function with baselines up to six Earth diameters is calculated.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"146 - 153"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021056","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":"Erratum to: Special Features of the Magnetic Field Structure of the He-r Star HD 37479 (boldsymbol{sigma}) Ori E","authors":"Yu. V. Glagolevskij,&nbsp;A. F. Nazarenko","doi":"10.1134/S1990341326550018","DOIUrl":"10.1134/S1990341326550018","url":null,"abstract":"","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"163 - 163"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021057","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":"Orbital and Astrophysical Parameters of Spectroscopic Binary Cepheids V496 Aql, V1344 Aql, V1334 Cyg, and AW Per","authors":"A. S. Rastorguev,&nbsp;M. V. Zabolotskikh,&nbsp;N. A. Gorynya","doi":"10.1134/S199034132560070X","DOIUrl":"10.1134/S199034132560070X","url":null,"abstract":"<p>We present the results of a comprehensive study of four spectroscopic binary Cepheids with long orbital periods. The study makes use of all the available photometric, spectroscopic, and astrometric information and previously developed analysis techniques. The paper is based on a new catalog containing 702 radial velocity measurements of V496 Aql (232 measurements), V1344 Aql (194 measurements), V1334 Cyg (138 measurements), and AW Per (138 measurements). All the measurements were obtained over 1997–2021 with the Zeiss-1000 telescope of the Institute of Astronomy of the Russian Academy of Sciences Simeiz Observatory using the correlation Radial Velocity Meter (RVM) designed by A.A. Tokovinin. Using other published observations, the orbital periods and other orbital parameters were significantly refined: V496 Aql: <span>(P_{textrm{orb}}approx 1351overset{textrm{d}}{.}text{}3pm 0overset{textrm{d}}{.}text{}7)</span>; V1344 Aql: <span>(P_{textrm{orb}}approx 635overset{textrm{d}}{.}8pm 30^{textrm{d}})</span>; V1344 Cyg: <span>(P_{textrm{orb}}approx 1934overset{textrm{d}}{.}text{}4pm 0overset{textrm{d}}{.}text{}8)</span>; AW Per: <span>(P_{textrm{orb}}approx 13,663pm 128^{textrm{d}})</span>. Using the mass function, we have found additional constraints on the companion masses and the orientation of the orbital plane. For V496 Aql and V1344 Aql, a complete set of astrophysical parameters was found including the color excess, pulsational radii, luminosity, and mass estimates based on the evolutionary tracks (for V496 Aql, <span>(Msim 5.6{-}5.8M_{odot})</span>; for V1334 Aql, <span>(Msim 5.8{-}6.0M_{odot})</span>). For the V1334 Cyg Cepheid with a massive companion, the strong constraint <span>(isim 56^{circ}{-}60^{circ})</span> on the inclination of its orbital plane was found based on the high mass function. AW Per, with an orbital period of over 37 years and a high mass function, has a companion of a comparable mass. The calculated pulsational radius and luminosity of the Cepheid are in good agreement with the evolutionary mass estimate <span>(Msim 5.6{-}5.9,M_{odot})</span>. We show that at inclination angles smaller than <span>(63^{circ}{-}65^{circ})</span>, the companion can only be a close binary system consisting of two hot stars near the main-sequence turnoff point.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"83 - 99"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021070","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":"Kinetic Parameters of the Fractal Stellar Medium in the Vicinity of the Sun","authors":"M. L. Ostashova,&nbsp;A. S. Rastorguev","doi":"10.1134/S1990341325600577","DOIUrl":"10.1134/S1990341325600577","url":null,"abstract":"<p>This paper estimates the kinetic parameters of the fractal stellar medium in the vicinity of the Sun. In this regard, the main stages in the development of ideas about fractal structures in the stellar medium of galaxies are presented. This study is based on investigation of the spatial distribution of 200 000 stars of all spectral types at distances from 1 to 100 pc from the Sun based on the Gaia DR2 data. The results indicate the presence of fractal structures in the solar neighborhood with the fractal dimension <span>(Dapprox 2.41)</span>. Based on these data, the kinetic properties of the fractal stellar medium are studied. The role of irregular forces and paired stellar encounters in the collisional kinetics of stellar systems is considered. It has been shown that kinetic parameters such as the effective interparticle (interstellar) distance, correlation length, dynamic friction coefficient, and impact parameter for a fractal stellar medium differ significantly from the corresponding parameters for a quasi-homogeneous medium with limited density fluctuations and depend on the fractal dimension. It has been found that the fractal structure of the stellar medium leads to shortening the relaxation time in the Galaxy.</p>","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"81 1","pages":"100 - 106"},"PeriodicalIF":1.4,"publicationDate":"2026-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148021050","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}