Astronomy Reports最新文献

{"title":"Onboard Information Hub Concept for the Russian Orbital Station","authors":"S. F. Likhachev,&nbsp;A. G. Rudnitsky,&nbsp;P. R. Zapevalin,&nbsp;M. A. Shchurov,&nbsp;D. M. Rudkovsky","doi":"10.1134/S1063772926700046","DOIUrl":"10.1134/S1063772926700046","url":null,"abstract":"<p>This paper presents the concept of an onboard information hub as a part of the Russian Orbital Station (ROS). The hub is intended for receiving, storing, processing, and transmitting large volumes of data. The general structure of the hub is described. Additionally, analysis of the optimal orbital configuration of the station is investigated. Three different orbital inclinations are compared to satisfy both the requirements of the proposed concept and other potential tasks of the ROS. A concept of the information hub will integrate the Russian satellite constellation with the orbital station. The main load of data transmission and processing could be moved from the satellites to the station itself, which will significantly increase the efficiency of data exchange for satellites, constellations, and the scientific experiments to be conducted onboard the Russian Orbital Station.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1514 - 1533"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579214","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 Pushchino Multibeams Pulsar Search. VIII. Pulsar with a Period of 40.9 s in Observations of the LPA LPI","authors":"S. A. Tyul’bashev,&nbsp;G. E. Tyul’basheva,&nbsp;S. A. Andrianov,&nbsp;M. A. Kitaeva","doi":"10.1134/S106377292570252X","DOIUrl":"10.1134/S106377292570252X","url":null,"abstract":"<p>A search has been carried out for the pulsar J0311+1402, which has a period <span>(P = 40.9)</span> s, in the data archive of the Large Phased Array (LPA) radio telescope. When searching using fast folding algorithms (FFA), periodic pulsar radiation at a frequency 111 MHz was not detected. In 3321 observation sessions lasting 5 minutes, 35 strong pulses were detected with a signal-to-noise ratio (S/N) greater than 10. Some of the pulses have a complex multi-peak structure consisting of narrow details, while some of the pulses are single-component. The peak flux densities of the details of these strong pulses are from 2 to 11 Jy. The peak value (<span>({S_p} = 2)</span> Jy) and the integral (<span>({S_i} = 7)</span> mJy) flux density in the average profile obtained from strong pulses. It is shown that pulsar pulses in the meter wavelength range arrive sporadically, and the pulsar is similar in its properties to a rotating radio transient (RRAT). The pulsar has the minimum dispersion measure, the minimum distance from the Sun, and the minimum pseudo-luminosity of all known pulsars. The timing made it possible to improve the previously obtained value of the period <span>(P)</span> and to estimate the period derivative <span>(dot P)</span>. Depending on the residual deviations from the time of arrival (TOA) of pulses, discontinuities are visible when no pulses were observed. The duration of these breaks can be hundreds of days.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1364 - 1372"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579336","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":"Mathematical Insights into Triangular Configurations of the Sitnikov Four-Body Dynamics","authors":"M. Shahbaz Ullah,&nbsp;M. Javed Idrisi","doi":"10.1134/S1063772925600323","DOIUrl":"10.1134/S1063772925600323","url":null,"abstract":"<p>This paper extends the classical Sitnikov problem by considering three primary bodies of equal mass positioned at the vertices of a triangle, each moving in circular orbit around their common center of mass. The equations of motion are derived for an infinitesimal mass constrained to move along the <i>z</i>-axis, with the plane of motion rotating at a constant unit angular velocity. The analysis includes the determination of zero-velocity regions on the <i>xy</i>, <i>yz</i>, and <i>zx</i> planes. The coordinates of the equilibrium points are calculated, and their stability is examined in detail. The study also explores the motion of the fourth body using Poincaré surfaces of section to reveal the system’s dynamic behavior. Over time, the emergence of regular orbital patterns is observed, highlighting the interplay between symmetry and stability in the system’s evolution.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1407 - 1415"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579122","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":"Activity of the K4 Dwarf HAT-P-11 and Mass Loss of the Atmosphere of Its Exoplanet HAT-P-11 b","authors":"I. S. Savanov,&nbsp;A. D. Kalinkin","doi":"10.1134/S1063772926700095","DOIUrl":"10.1134/S1063772926700095","url":null,"abstract":"<p>In this paper, the results of an analysis of photometric activity of the star HAT-P-11, which hosts two planets, have been presented. This analysis has been based on archival data from the KWS, DASCH, and ASAS-SN sky surveys, as well as the Kepler telescope archive. S-index variability data have also been examined. Evidence of long-term cycles of 500–600 and 600–700^<i>d</i> has been found. The DASCH archive data have supported this conclusion by suggesting longer cycles. Based on the ASAS-SN survey data, the cyclicity on scales of approximately 1500 days has been suggested. Based on the S-index data, the cycle length (3848^<i>d</i>) is close to the estimated orbital period of 3299 days for the exoplanet HAT-P-11 c. Using an approximation formula corresponding to the energy-limited atmosphere loss model, we have estimated the mass outflow from the atmosphere of planet b. These estimates range from <span>(1.7 times {{10}^{9}})</span> g/s for <span>(log {{R}^{'}_{{HK}}}, = - 4.67)</span> to <span>(3.3 times {{10}^{9}})</span> g/s for <span>(log {{R}^{'}_{{HK}}}, = - 4.51)</span>. Based on 261 estimates of the parameter S, we have calculated the mass loss from the atmosphere of HAT-P-11 b in the interval of 6152 days (16.85 years).</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1488 - 1496"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579344","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":"Statistic of Stars with Poor Astrometric Solutions of Gaia DR3 in Open Star Clusters","authors":"D. I. Tagaev,&nbsp;A. F. Seleznev","doi":"10.1134/S1063772925702518","DOIUrl":"10.1134/S1063772925702518","url":null,"abstract":"<p>We performed counts of stars with poor astrometric solutions of Gaia DR3 in the regions of open star clusters: NGC 188, NGC 1039, NGC 2287, NGC 2301, NGC 2360, NGC 2420, NGC 2527, NGC 2548, NGC 2682 (M 67), NGC 3114, NGC 3766, NGC 5460, NGC 6649. The selection of the possible cluster members is based on the Gaia photometry using the Hess diagram. We look for stars that fall within the region of the Hess diagram plotted from probable cluster members based on Hunt and Reffert data. We take stars with two-parameter solutions, with the parameter RUWE &gt; 1.4, as well as with large relative parallax errors that fall within the Hess diagram region for probable cluster members. The radii of clusters based on stars with poor astrometric solutions and the number of such possible cluster members were estimated. The number of stars with poor astrometric solutions relative to the number of stars from the Hunt and Reffert sample <span>({N_{{text{bad}}}}{text{/}}N)</span> varies very widely with a median average of approximately 30%. This means that when one selects probable cluster members based on precise astrometric data from Gaia DR3, an average of about 23% of cluster members may be lost. Among the lost stars there may be a significant number of unresolved binary and multiple systems. We investigated the dependence of the relative number of stars with poor astrometric solutions on the galactic latitude and on the average number density of stars. The brightness functions with and without stars with poor solutions differ significantly in the region of faint stars, <span>(G in {[14^m}{,18^m}])</span>, for clusters with a relative number of possible cluster members with poor astrometric solutions of <span>({N_{{text{bad}}}}{text{/}}N gtrsim 0.15)</span>. The work is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1295 - 1306"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579291","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":"Monitoring of the Scintillation Parameters of PSR B1133+16 and B1237+25 at 111 MHz","authors":"T. V. Smirnova,&nbsp;M. V. Popov","doi":"10.1134/S106377292570249X","DOIUrl":"10.1134/S106377292570249X","url":null,"abstract":"<p>We consider long-term measurements of the scattering parameters of radio emission of pulsars B1133+16 and B1137+25 at a frequency of 111 MHz. The observations were carried out with the Large Phased Array (LPA) at the Pushchino Radio Astronomy Observatory of the Lebedev Physical Institute. Pulsars B1133+16 and B1237+25 were observed for 810 and 552 days, respectively. We analyze the dynamic spectra, from which the following parameters and their time variations were measured: the time and frequency scales of diffractive scintillations, the signal amplitude, and the Faraday rotation period (for PSR B1133+16). For both pulsars, rapid variations in the signal amplitude on a scale of 1−3 days were observed. They are mainly caused by refractive scintillations. For PSR B1133+16, variations on a scale of 50−100 days were observed. Among them, the most pronounced are frequency variations in the decorrelation bandwidth over time. Apparently, they are also caused by refractive scintillations on spatial scales of (3−6) × 10¹⁴ cm. For all of the parameters analyzed, modulation indices were measured. For both pulsars, the modulation indices of the peak flux density significantly exceed the estimates obtained with theoretical models. A significant anticorrelation has been found between variations in the peak flux density of PSR B1237+25 and in the decorrelation bandwidth: the correlation coefficient is –0.59. For PSR B1133+16, no correlation is observed. From the behavior of fluctuations in the relative flux density over time and from the variability of the decorrelation band width for pulsar B1237+25, extreme scattering events (ESEs) were revealed. Regular components were found in the structure function of the time variations of the decorrelation band for pulsar B1133+16, which can be interpreted as an indication of regular structures of interstellar plasma inhomogeneities on spatial scales of about three astronomical units.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1351 - 1363"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579124","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":"Stability of the Milky Way Satellite Galaxy Plane under the Influence of Neighbors","authors":"S. V. Pilipenko,&nbsp;N. R. Arakelyan","doi":"10.1134/S1063772926700071","DOIUrl":"10.1134/S1063772926700071","url":null,"abstract":"<p>Trajectories of test particles in a time-varying nonspherical gravitational potential model of our Galaxy have been considered. The role of the quadrupole component of the potential, which at distances greater than 50 kpc is associated with the distribution of matter in the Galaxy’s neighborhood (mainly with the influence of the galaxy M31), has been studied. It has been shown that perturbations of the potential created by the environment can significantly change the trajectories of particles at distances greater than 100 kpc from the Galactic center, but the magnitude of this effect depends on the still poorly known trajectory of the galaxy M31. For some variants of this trajectory, structures resembling a “thin plane” of satellite galaxies cannot exist for more than 2–3 billion years.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1416 - 1423"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579215","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":"Mutual Observations of Cosmic Gamma Ray Bursts with the Moscow University CubeSat Constellation and Master Network Robotic Telescopes","authors":"A. F. Iyudin,&nbsp;S. I. Svertilov,&nbsp;V. M. Lipunov,&nbsp;V. V. Bogomolov,&nbsp;A. V. Bogomolov,&nbsp;V. E. Eremeev,&nbsp;V. V. Kalegaev,&nbsp;M. V. Korzhik,&nbsp;A. S. Kuznetsov,&nbsp;I. A. Kucherenko,&nbsp;V. I. Osedlo,&nbsp;I. V. Yashin","doi":"10.1134/S1063772926700022","DOIUrl":"10.1134/S1063772926700022","url":null,"abstract":"<p>Since January 25, 2005, Moscow State University has been implementing its own space program. At present, it is mainly associated with the implementation of the Sozvezdie-270 project, which should result in the deployment of a group of nanosatellites of the CubeSat format in near-Earth space. To date, 20 satellites of the 1U, 1.5U, 3U, and 6U formats have been launched with instruments developed and manufactured at the Skobeltsyn Institute of Nuclear Physics of Moscow State University (SINP MSU), of which 9 continue to operate in sun-synchronous orbits at an altitude of 400–600 km. For use as a payload on CubeSat satellites, SINP MSU has developed a number of instruments that include miniature detectors of gamma quanta and electrons with energies in the ranges of 0.02–2.0 and 0.3–10.0 MeV, respectively. These instruments can be used, among other goals, to detect gamma-ray bursts (GRBs) at a fairly good sensitivity level (~10^–7 erg/cm² at burst duration 1 s). To date, 32 GRBs have been detected with their help. This paper discusses the results of mutual observations of GRBs using the orbital Moscow University nanosatellite constellation and robotic telescopes of the MASTER Global Network. The upper limits of the intensity of the prompt and afterglow emission of detected GRBs are presented, and the results of the search for optical sources in the regions of GRB localization are analyzed.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1424 - 1441"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579216","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":"Search for Luminous Emission Stars in the Galaxy NGC 2835","authors":"O. N. Sholukhova,&nbsp;Yu. N. Solovyeva,&nbsp;A. S. Vinokurov,&nbsp;V. S. Frolova","doi":"10.1134/S1063772925702531","DOIUrl":"10.1134/S1063772925702531","url":null,"abstract":"<p>Based on archived data from the MUSE (Multi Unit Spectroscopic Explorer) spectrograph of the VLT telescope, 40 candidates for luminous stars with their own emission in the H_α line in the galaxy NGC 2835 were selected. Based on the results of analysis of the candidate spectra and direct images of galaxies with high angular resolution from the Hubble Space Telescope archive, a classification was carried out. It is shown that eight objects in NGC 2835 are Wolf–Rayet stars or compact stellar associations that include them. The five sources in NGC 2835, which have the spectra of supergiants with surrounding compact nebulas, are classified by us as OB clusters. Another ten objects showed wide H_α lines and a weak continuum, and we labeled them as unclassified. Of the greatest interest for further observations in order to more accurately classify and evaluate the fundamental parameters are ten stars previously classified as yellow supergiants/hypergiants and one B[e]-supergiant. One of the important results is the detection of five candidates for luminous blue variables (LBVs) and one probable supernova impostor. The study is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1260 - 1268"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579292","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":"Мeasurements of the Faraday Rotation Measure in the Direction of Pulsar B0531+21 in the Crab Nebula at a Frequency of 111 MHz at the LPA","authors":"B. Ya. Losovsky","doi":"10.1134/S1063772925702439","DOIUrl":"10.1134/S1063772925702439","url":null,"abstract":"<p>The results of monitoring of radio pulsar B0531+21 in the Crab Nebula at the Pushchino Radio Astronomy Observatory of the Astrospace Center of the Physics Institute of the Russian Academy of Sciences at a frequency of 111 MHz are analyzed on a Large Phased Array (LPA) from September 2002 to December 2024. Giant pulsar pulses (GPs) are observed. GPs are analyzed using special programs that make it possible to determine the magnitude of the Faraday rotation measure (<i>RM</i>) and pulse broadening by scattering time τ_sc simulating the passage of a pulse through a magnetically active plasma. The measured values of <i>RM</i> and GPs scattering are compared with the values of the dispersion measure according to the data of the Jodrell Bank Observatory (Great Britain). Unsteady processes were recorded, characterized by increased scattering in 2009–2013 and anomalous in 2020–2024. The correlation coefficient between the dispersion measure and the scattering time τ_sc = 0.8 ± 0.1. The observed phenomena can be explained by eclipsing the pulsar by filaments and increasing turbulence in the plasma structures of the nebula. The correlation coefficient between the <i>RM</i> in filaments and the dispersion measure <i>dm</i> = –0.4 ± 0.2, between the magnetic induction in filaments and the dispersion measure <i>dm</i> = 0.2 ± 0.2, between the <i>RM</i> in filaments and the magnetic induction is 0.8 ± 0.1. Data processing showed that the <i>RM</i> value varied from ≈–47 rad/m² in 2006 to ≈–52 rad/m² in 2010. Since 2011, <i>RM</i> began to change dramatically and in 2012 amounted to ≈–44 rad/m². Long-term <i>RM</i> variations are caused by magnetic field inhomogeneities and filaments density variations in the Crab Nebula. The magnetic induction in the interstellar medium in the direction of the pulsar was –0.96 ± 0.01 µG and in the nebula’s filaments it ranged within 130µG. Seasonal variations of the observed <i>RM</i> with the amplitude of 0.7 ± 0.1 rad/m² caused by the Earth’s ionosphere have been measured.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"69 12","pages":"1342 - 1350"},"PeriodicalIF":0.7,"publicationDate":"2026-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147579332","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}