Astronomy Reports最新文献

{"title":"Search for the Possible Members of the Open Cluster NGC 3532 with Poor Astrometric Solutions of GAIA DR3","authors":"D. I. Tagaev,&nbsp;A. F. Seleznev","doi":"10.1134/S1063772925701884","DOIUrl":"10.1134/S1063772925701884","url":null,"abstract":"<p>We performed star counts in the region of the open cluster NGC 3532. The ranges of trigonometric parallaxes and proper motions containing all the stars of the cluster were determined using the stars with 5‑and 6-parameter Gaia DR3 solutions. The estimated radius of the cluster was <span>({{R}_{c}} = 178{'} pm 3{'} )</span> and the number of cluster stars was <span>({{N}_{c}} = 2200 pm 40)</span>. We estimate the number of stars with poor astrometric solutions that may be members of the cluster. For this purpose, we analyze the surface density distribution of stars with two-parameter Gaia DR3 solutions, stars with the parameter <span>(operatorname{RUWE} &gt; 1.4)</span>, and stars with large relative errors of trigonometric parallaxes in the vicinity of the cluster. We are looking for stars that fall within the area of the color–magnitude diagram occupied by probable members of the NGC 3532 cluster from the Hant–Reffert sample. The radial surface density profile plotted with such stars shows the concentration of stars toward the cluster center. An analysis of the profile yields an estimate of <span>(2150 pm 230)</span> stars that may be cluster members. Thus, nearly one half of cluster members can be lost when the probable members are selected only by exact astrometric data of Gaia DR3. Among these lost stars, there may be a significant number of unresolved binary and multiple systems.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 6","pages":"457 - 468"},"PeriodicalIF":0.7,"publicationDate":"2025-08-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161189","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":"Aspects of Optimization of the Transit Light Curve of the Binary System with a Single Minimum by the Eccentricity Components","authors":"M. K. Abubekerov,&nbsp;N. Yu. Gostev","doi":"10.1134/S1063772925701847","DOIUrl":"10.1134/S1063772925701847","url":null,"abstract":"<p>A high-precision algorithm for interpreting transit light curves in the model of an eclipsing classical binary star–exoplanet system for interpretation moving from the eccentricity (<span>(e)</span>)–periastron longitude (<span>(omega )</span>) variables to the (<span>(ecos omega ,;{kern 1pt} esin omega )</span>) eccentricity components has been improved. The possibilities of interpretation by eccentricity components have been studied. It has been shown that the dependence of the minimum’s shape on <span>(esin omega )</span> alone is clearly expressed at small <i>e</i> values and weakens with increasing <span>(e)</span>. The linear correlation between the radius value, which is characteristic of any <i>e</i> values, has been shown.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 6","pages":"469 - 479"},"PeriodicalIF":0.7,"publicationDate":"2025-08-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161669","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 Effect of Luminosity Outbursts on the Abundance of Pebbles and Their Ice Mantles in Protoplanetary Disks","authors":"A. P. Topchieva,&nbsp;T. S. Molyarova,&nbsp;E. I. Vorobyov","doi":"10.1134/S1063772925701896","DOIUrl":"10.1134/S1063772925701896","url":null,"abstract":"<p>Dust growth is one of the key processes leading to planet formation in protoplanetary disks. Centimeter-sized dust grains, pebbles, are essential for the formation of planetesimals through streaming instability and play a crucial role in the formation of protoplanetary cores, giant planets, and the enrichment of their atmospheres with chemical elements. In this paper, the impact of luminosity outbursts on the amount of pebbles and icy mantles in a protoplanetary disk has been studied. We have performed global simulations of the formation and evolution of a self-gravitating, viscous protoplanetary disk using the two-dimensional thin-disk hydrodynamic code FEOSAD, which self-consistently produces luminosity outbursts. The model includes thermal balance, dust evolution and its interaction with gas, the development of magnetorotational instability, adsorption and desorption of four volatile species (H₂O, CO₂, CH₄, and CO), and the effect of icy mantles on the fragmentation properties of dust aggregates. Our results have shown that luminosity outbursts have a stronger impact on the CO₂, CH₄, and CO ice lines than on the water ice line. This is because the H₂O ice line resides in a region dominated by viscous heating during the early stages of disk evolution, whereas the ice lines of the other molecules lie in regions where stellar irradiation dominates the thermal structure, making them more sensitive to temperature variations induced by the outbursts. Nevertheless, luminosity outbursts lead to a twofold reduction in the total amount of pebbles in the disk due to the disintegration of dust aggregates into monomers following the loss of water ice, which acts as a binding agent. The reformation of pebbles occurs over several thousand years after the outburst, primarily through collisional coagulation. The characteristic timescales for pebble recovery significantly exceed the freezing timescales of water ice. The desorption of icy mantles occurs in a highly non-axisymmetric and intrinsically two-dimensional region of the disk due to the formation of spiral substructures during the early evolution of a gravitationally unstable disk.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 6","pages":"532 - 546"},"PeriodicalIF":0.7,"publicationDate":"2025-08-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161672","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":"Absolute Parameters and Apsidal Motion of the Eclipsing System V501 Mon","authors":"A. S. Volkova,&nbsp;I. M. Volkov","doi":"10.1134/S1063772925701859","DOIUrl":"10.1134/S1063772925701859","url":null,"abstract":"<p>Our photoelectric measurements over the past 30 years and a new solution of the radial velocity curve of the eclipsing star with an elliptical orbit V501 Mon (A8 + F2) allowed us to determine with high accuracy all the main parameters of the system: <span>({{T}_{1}} = 7380 pm 60)</span> K, <span>({{M}_{1}} = 1.66 pm 0.03{kern 1pt} {{M}_{ odot }})</span>, <span>({{R}_{1}} = 1.90 pm 0.02{kern 1pt} {{R}_{ odot }})</span>, <span>({{T}_{2}} = 6920 pm 30)</span> K, <span>({{M}_{2}} = 1.47 pm 0.02{kern 1pt} {{M}_{ odot }})</span>, <span>({{R}_{2}} = 1.58 pm 0.01{kern 1pt} {{R}_{ odot }})</span>. The photometric parallax determined in the study coincides with the Gaia value <span>(pi =0.00103{''} )</span> within the error limits. For the first time, the apsidal motion rate <span>({{dot {omega }}_{{{text{obs}}}}} = 0.022^circ )</span>/year was accurately measured, which, within the error limits, matches the theoretical value: <span>({{dot {omega }}_{{{text{theor}}}}} = 0.024^circ )</span>/year; 70% of this value is a relativistic contribution. The system possibly satisfies the condition of synchronism between rotational and orbital angular momenta. The age of the stars was determined to be 0.95 billion years. The main component is probably a pulsating variable star of the <span>(delta )</span> Scuti type (DSCT).</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 6","pages":"480 - 499"},"PeriodicalIF":0.7,"publicationDate":"2025-08-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145161083","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":"On the Nature of Spiral Arms in the Interacting Galaxy M51","authors":"F. Kh. Sakhibov,&nbsp;V. S. Kostiuk,&nbsp;A. S. Gusev,&nbsp;E. V. Shimanovskaya","doi":"10.1134/S1063772925701811","DOIUrl":"10.1134/S1063772925701811","url":null,"abstract":"<p>In this study, we investigated the radial variation of the azimuthal propagation of star formation across the spiral arms in the nearby galaxy NGC 5194 (M51a) by analysing the spatial separation between young star clusters and their nearest H II regions. The significant differences in the radial profiles of the mean azimuthal offsets in the M51a arms were found when the southern and northern arms were studied separately. The northern arm analysis showed that its radial profile is consistent with the predictions of stationary density wave theory for trailing spirals, while the explanation of the radial profile for the southern arm required its pattern speed to be higher than the rotation velocity of disc matter within the corotation circle, and lower than that outside of it. At the same time, these different radial profiles of the mean azimuthal offset in the two arms are joined by a common localization of corotation resonances, confirmed by independent studies using different methods.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"348 - 362"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164579","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":"Kinematics of Stars with Radially Elongated Orbits Located within 100 pc from the Sun","authors":"E. S. Postnikova,&nbsp;N. V. Chupina,&nbsp;S. V. Vereshchagin","doi":"10.1134/S1063772925701793","DOIUrl":"10.1134/S1063772925701793","url":null,"abstract":"<p>The motion of stars whose spatial velocities have radial directions of motion in the galactic disk has been studied using numerical modeling. For this purpose, stars located within 100 pc from the Sun with spatial velocities directed approximately to the galactic Center (or anticenter) have been selected from the Gaia DR3 catalog. The sample included 13 stars with characteristics of halo stars: the eccentricities of their spatial orbits are close to unity and metallicity is significantly less than zero. An axisymmetric model of the Galaxy, including the bulge, disk, and halo, has been used. It has been found that the orbital apsides of the stars in our sample show a retrogradely directed precession with a velocity of 15–20 pc/million years in the interval from 10 to 20 kpc from the CG.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"391 - 397"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164575","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":"Four Years of Wide-Field Search for Nanosecond Optical Transients with the TAIGA-HiSCORE Cherenkov Array","authors":"A. D. Panov,&nbsp;I. I. Astapov,&nbsp;G. M. Beskin,&nbsp;P. A. Bezyazykov,&nbsp;A. V. Blinov,&nbsp;E. A. Bonvech,&nbsp;A. N. Borodin,&nbsp;N. M. Budnev,&nbsp;A. V. Bulan,&nbsp;P. Busygina,&nbsp;D. V. Chernov,&nbsp;A. Chiavassa,&nbsp;A. N. Dyachok,&nbsp;A. R. Gafarov,&nbsp;A. Yu. Garmash,&nbsp;V. M. Grebenyuk,&nbsp;E. O. Gress,&nbsp;O. A. Gress,&nbsp;T. I. Gress,&nbsp;A. A. Grinyuk,&nbsp;O. G. Grishin,&nbsp;A. L. Ivanova,&nbsp;A. D. Ivanova,&nbsp;M. A. Ilyushin,&nbsp;N. N. Kalmykov,&nbsp;V. V. Kindin,&nbsp;S. N. Kiryuhin,&nbsp;R. P. Kokoulin,&nbsp;K. G. Kompaniets,&nbsp;E. E. Korosteleva,&nbsp;V. A. Kozhin,&nbsp;E. A. Kravchenko,&nbsp;L. A. Kuzmichev,&nbsp;A. P. Kryukov,&nbsp;A. A. Lagutin,&nbsp;M. V. Lavrova,&nbsp;Yu. Lemeshev,&nbsp;B. K. Lubsandorzhiev,&nbsp;N. B. Lubsandorzhiev,&nbsp;A. D. Lukanov,&nbsp;S. D. Malakhov,&nbsp;R. R. Mirgazov,&nbsp;R. D. Monkhoev,&nbsp;E. A. Okyneva,&nbsp;E. A. Osipova,&nbsp;A. L. Pakhorukov,&nbsp;A. Pan,&nbsp;L. V. Pankov,&nbsp;A. A. Petrukhin,&nbsp;D. A. Podgrudkova,&nbsp;I. A. Poddubny,&nbsp;E. G. Popova,&nbsp;E. B. Postnikov,&nbsp;V. V. Prosin,&nbsp;A. A. Pushnin,&nbsp;R. I. Raikin,&nbsp;A. Yu. Razumov,&nbsp;E. Rjabov,&nbsp;G. I. Rubtsov,&nbsp;V. S. Samoliga,&nbsp;A. V. Shaikovsky,&nbsp;A. Yu. Sidorenkov,&nbsp;A. A. Silaev,&nbsp;A. A. Silaev Jr,&nbsp;A. V. Skurikhin,&nbsp;I. Satyshev,&nbsp;A. V. Sokolov,&nbsp;L. G. Sveshnikova,&nbsp;V. A. Tabolenko,&nbsp;A. B. Tanaev,&nbsp;M. Ternovoy,&nbsp;L. G. Tkachev,&nbsp;N. Ushakov,&nbsp;P. A. Volchugov,&nbsp;N. V. Volkov,&nbsp;D. M. Voronin,&nbsp;I. I. Yashin,&nbsp;A. V. Zagorodnikov,&nbsp;D. P. Zhurov,&nbsp;V. N. Zirakashvili","doi":"10.1134/S106377292570177X","DOIUrl":"10.1134/S106377292570177X","url":null,"abstract":"<p>It has been previously demonstrated by Panov et al. (2021) that the TAIGA-HiSCORE Cherenkov array, originally built for cosmic ray physics and ultrahigh-energy gamma-ray astronomy studies using the extensive air shower method, can be used in conventional optical astronomy for wide-field searches for rare nanosecond optical transients of astrophysical origin. The field of view of the facility is on the scale of 1 ster, and it is capable of detecting very rare transients in the visible light range with fluxes greater than approximately 3000 quanta/m²/10 ns (10 ns is the apparatus integration time) and pulse durations of 10 ns. Among the potential sources of distant nanosecond optical transients are the evaporation of primary black holes, magnetic reconnection in the accretion disks of black holes, and signals from distant lasers of extraterrestrial civilizations. The paper describes the methods and results of the search for optical transients using the TAIGA-HiSCORE Cherenkov array from 2018 to 2022 (four winter seasons of data collection). No reliable astrophysical candidates for optical transients were found. We set an upper bound on the flux of the searched events as <span>( sim {kern 1pt} 1 times {{10}^{{ - 3}}})</span> events/ster/h.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"433 - 456"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164574","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":"Planetary Systems in Star Clusters","authors":"A. V. Tutukov,&nbsp;S. V. Vereshchagin,&nbsp;N. V. Chupina","doi":"10.1134/S1063772925701823","DOIUrl":"10.1134/S1063772925701823","url":null,"abstract":"<p>About a third of stars in open star clusters of the Galaxy may have planetary systems. The increased density of stars in clusters introduces its own peculiarities into the evolution of their planetary systems. An analysis of the evolution conditions of planetary systems in star clusters has shown that close passages of cluster stars during its lifetime of ~3 × 10⁸ years destroy the peripheral structures of planetary systems: asteroid–comet–planetary (ACP) spears, Kuiper belts. At the same time, the parts of planetary systems close to the star are not affected. As a result of the ACP, objects with major semi-axes of orbits exceeding ~17 AU are lost by planetary systems, forming the ACP of the cluster spear. The result of the cluster evolution after its disintegration is the formation of the ACP flow, coinciding with the stellar flow. The observed displacement of massive clusters of the Galaxy relative to the center of their stellar copies is a consequence of the gravitational braking of the clusters. It can be used to estimate the rotation parameters of the dark halo of the Galaxy with allowance for the asymmetry of the stellar copies of massive clusters caused by the gravitational braking of the nuclei.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"375 - 390"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164576","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 Pulkovo Catalog of the Orbits Obtained for Visual Binary and Multiple Stars by the Apparent Motion Parameters Method","authors":"L. G. Romanenko,&nbsp;O. V. Kiyaeva,&nbsp;I. S. Izmailov,&nbsp;N. A. Shakht,&nbsp;D. L. Gorshanov","doi":"10.1134/S106377292570180X","DOIUrl":"10.1134/S106377292570180X","url":null,"abstract":"<p>The paper presents orbits of 69 wide pairs of visual binary and multiple stars (belonging to 65 systems) obtained by the Apparent Motion Parameters (AMP) method. The possibility of determining the AMP orbits of these pairs using Gaia DR3 data at the time point 2016.0 is considered. (1) Orbits according to Gaia DR3 were obtained for 45 pairs. (2) For another 20 pairs, the quasi-instantaneous motion according to Gaia data contradicts the mean motion from all available observations. A possible reason is the presence of inner subsystems. (3) AMP orbits were also determined for 3 bright stars (ADS 2080, ADS 7724, and ADS 9173) and 3 close pairs (angular separation less than <span>(2'' )</span>: ADS 2416, ADS 5570, and T Tau NS) that do not have the Gaia DR3 positional observations. The basis for the study in cases 2 and 3 is the Pulkovo series of observations on the 26-inch refractor and/or data from the literature. Of the 69 pairs of stars studied, 59 have semi-major axes of the orbit greater than 100 AU. Among them, families of orbits with minimum periods from 5000 to 730 000 years and minimum semi-major axes of more than 400 AU were obtained for 17 pairs. Unique solutions were obtained for the orbits of 28 pairs. Of these, 20 pairs have a semi-major axis of the orbit greater than 100 AU and periods from 600 to 6000 years. Relative errors in determining the elements are generally about 15–20%. The orientation of the resulting orbits in the Galactic coordinate system is also determined.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"398 - 432"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164577","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":"On the Angular Anisotropy of the Distribution Function of Radiating Particles in Relativistic Jets","authors":"T. I. Khalilov,&nbsp;V. S. Beskin,&nbsp;V. I. Pariev","doi":"10.1134/S1063772925701835","DOIUrl":"10.1134/S1063772925701835","url":null,"abstract":"<p>The observed power-law spectra of relativistic jets from active galactic nuclei clearly indicate a synchrotron mechanism of radiation by particles that similarly possess a power-law energy spectrum. However, the issue of their angular anisotropy has not been given sufficient attention until recently, although the example of the solar wind (where a strongly magnetized wind is realized in a similar way) shows the importance of taking this circumstance into account. In this paper, we study the evolution of an initially isotropic power-law spectrum of radiating particles as they propagate along expanding relativistic jets. It is shown that for relativistic flows in which the electric field plays a crucial role, the preservation of the first adiabatic invariant does not lead to a decrease in the pitch angles of radiating particles as they enter the region of weak magnetic fields. This is due to the drift nature of the particle motion.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 5","pages":"335 - 347"},"PeriodicalIF":0.7,"publicationDate":"2025-07-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145164578","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}