Astronomy Reports最新文献

{"title":"Asteroid and Comet Hazard","authors":"B. M. Shustov,&nbsp;M. E. Prokhorov","doi":"10.1134/S1063772925701422","DOIUrl":"10.1134/S1063772925701422","url":null,"abstract":"<p>The paper presents an overview of modern concepts about the asteroid-comet hazard. It describes the types of hazardous celestial bodies, as well as the methods and tools of detecting and monitoring near-Earth objects.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 2 supplement","pages":"S126 - S153"},"PeriodicalIF":1.1,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143629688","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 Problem of Planetary Bioprotection","authors":"B. M. Shustov,&nbsp;M. E. Prokhorov","doi":"10.1134/S106377292570146X","DOIUrl":"10.1134/S106377292570146X","url":null,"abstract":"<p>The paper is dedicated to space hazards related to biological contamination and includes recommendations or organizing planetary quarantine.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 2 supplement","pages":"S205 - S211"},"PeriodicalIF":1.1,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143629744","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 Dark and Quiet Sky Problem","authors":"B. M. Shustov,&nbsp;M. E. Prokhorov","doi":"10.1134/S1063772925701483","DOIUrl":"10.1134/S1063772925701483","url":null,"abstract":"<p>The paper discusses scientific, technical and organizational aspects of the problem of dark and quiet skies. The categories of artificial interference that negatively affect astronomical observations are described.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 2 supplement","pages":"S236 - S248"},"PeriodicalIF":1.1,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143629689","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":"Global Warming (Climate Catastrophe)","authors":"B. M. Shustov,&nbsp;M. E. Prokhorov","doi":"10.1134/S1063772925701471","DOIUrl":"10.1134/S1063772925701471","url":null,"abstract":"<p>An overview of the global warming problem is presented. The physics of the greenhouse effect is described, and a comparative analysis of this effect on various planets of the Solar System is given. Possible measures to counteract climate disasters are described.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 2 supplement","pages":"S212 - S235"},"PeriodicalIF":1.1,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143628724","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":"Application of a New Formula for Angular Velocity of Rotation to the Planetoid Haumea","authors":"B. P. Kondratyev","doi":"10.1134/S1063772925701392","DOIUrl":"10.1134/S1063772925701392","url":null,"abstract":"<p>The study has been aimed to test a new formula for the <span>({{Omega }})</span> angular velocity of rotation of inhomogeneous equilibrium figures using the model of a unique rapidly rotating trans-Neptunian dwarf planet Haumea. The three-axis two-component model of Haumea consists of an ellipsoidal rocky core and a thick confocal ice shell. The parameters of this model have been determined from a system of eight algebraic equations that take into account the complete kinematic-photometric information about the planetoid. Using the methods of potential theory, the components of the internal and external gravitational energy of the model on which this <span>({{Omega }})</span> depends have been found. For this purpose, a refined expression for the gravitational energy of a homogeneous confocal shell and a formula for the mutual energy of the core and the shell have been used. It has been found that in order to be consistent with the observed rotation period of Haumea of <span>({{tau }_{{{text{rot}}}}} = {{3}^{{text{h}}}}{text{.915}}{text{,}})</span> this model must be considered as a polytrope with the index of <span>(n approx 0.{text{984}})</span>. This result has confirmed the relevance of the developed method for studying inhomogeneous equilibrium figures.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1449 - 1456"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143621828","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":"Acceleration Potential and Density Profile of Secondary Plasma in the Magnetosphere of Orthogonal Pulsars","authors":"A. Yu. Istomin,&nbsp;F. A. Kniazev,&nbsp;V. S. Beskin","doi":"10.1134/S1063772925701264","DOIUrl":"10.1134/S1063772925701264","url":null,"abstract":"<p>A new method for determining the accelerating potential above the polar caps of radio pulsars with an arbitrary inclination angle of the magnetic axis to the rotation axis has been proposed. The approach has been based on the concept of a vacuum gap, the height and shape of the upper boundary of which are found self-consistently together with the solution of the corresponding Poisson equation. In turn, knowledge of the accelerating potential has made it possible to determine the transverse profiles of the secondary plasma de-nsity. It has also been shown that the effect of inverse Compton scattering on the considered processes is insignificant.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1271 - 1285"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143622071","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 Different Factors on the Solar Flare Energy","authors":"V. L. Merzlyakov","doi":"10.1134/S1063772925701276","DOIUrl":"10.1134/S1063772925701276","url":null,"abstract":"<p>The factors affecting the energy of the solar flare are being studied. The model of particle acceleration in the magnetic X-singularity has been studied. It has been found that the flare energy depends mainly on the flow of electrons into the acceleration zone. The change in such a flow is determined by the size of the acceleration zone. It has been calculated that for a chromospheric flare source, the vertical length of the acceleration zone has varied from ∼100 to ≈2 × 10³ km and its diameter varies from ∼1 to ≈100 km.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1286 - 1290"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143622072","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":"Light Curve Synthesis for Colliding-Wind Binary Systems","authors":"I. I. Antokhin,&nbsp;E. A. Antokhina","doi":"10.1134/S1063772925701239","DOIUrl":"10.1134/S1063772925701239","url":null,"abstract":"<p>The synthesis method which allows one to compute light curves of binary systems in the Roche model is a powerful and widely used analysis tool. However, in its original form, it is not suitable for the analysis of light curves of binary systems in which one or both components have powerful stellar winds. Previously, we proposed a model of a binary system based on the synthesis method and including one component with a wind. In the current paper, we propose a generalization of the model to the case when both components of the binary system have winds. The surface separating the two winds (the contact surface) is calculated within the framework of a steady state model of stellar wind collision. When calculating the light curve, the absorption of stellar radiation in the winds, as well as in the cooling layers located on both sides of the contact surface, is taken into account. The structure of the cooling layers and their surface density are calculated in the radiative shock limit. The algorithm allows one to take into account the asymmetry of the contact surface caused by the Coriolis force, as well as (using pre-calculated tables) the radiative inhibition of the winds in close binary systems. The results of numerical calculations in various test models are presented, clearly demonstrating the need to take into account the influence of the winds on optical light curves in WR + WR, WR + O, and O + O systems.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1239 - 1251"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143622196","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":"Spectroscopic Searches for Evolutionary Orbital Period Changes in WR + OB Binaries: the Case of WR 141","authors":"I. A. Shaposhnikov","doi":"10.1134/S106377292470104X","DOIUrl":"10.1134/S106377292470104X","url":null,"abstract":"<p>The results of new low-resolution spectroscopic observations of the short-period system WR 141 (WN5o + O5V–III, <span>(P approx {{21.7}^{d}})</span>), as well as the results of their comparison with the material of previous studies in order to search for an evolutionary change in the orbital period, are presented. A secular increase in the orbital period of WR 141 with a rate <span>(dot {P} = 1.6 pm 0.9)</span> s/yr, corresponding to a mass loss rate <span>({{dot {M}}_{{{text{WR}}}}} = (3.1 pm 1.9) times {{10}^{{ - 5}}} ;{{M}_{ odot }})</span>/yr with the masses of the stars in the system <span>({{M}_{{{text{WR}}}}} = 39 pm 10 ;{{M}_{ odot }})</span> and <span>({{M}_{{text{O}}}} = 37 pm 10; {{M}_{ odot }})</span>, is reported. A correlation between the mass loss rate of WR stars and their mass is discussed.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1145 - 1152"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143621766","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":"Study of the Interplanetary Coronal Mass Ejection (ICME) Disturbances of Different Structure Types between 1995 and 2022 and Their Relative Geoeffectiveness: Superposed Epoch Analysis","authors":"W. Alotaibi,&nbsp;B. Badruddin","doi":"10.1134/S1063772924600353","DOIUrl":"10.1134/S1063772924600353","url":null,"abstract":"<p>This study presents an analysis of the solar wind plasma and field parameters and geomagnetic indices response to 255 events between 1995 and 2022 with Disturbance storm time <i>Dst</i> ≤ –30 nT. The events were divided into nine groups and structures. Superposed epoch analysis was performed on the selected events to study the effect based on each group. We also performed a correlation analysis between geomagnetic indices, solar wind plasma and field parameters. We found that <i>Dst</i> has a strong correlation with Planetary Kp index (<i>Ap</i>) and a moderate correlation with Auroral Electrojet index (<i>AE</i>), while ap has a strong correlation with <i>Dst</i> and <i>AE</i>. Duskward electric field (<i>Ey</i>) is consistently better related to all three geomagnetic indices (<i>Dst</i>, <i>Ap</i> and <i>AE</i>), <i>Dst</i> relation is relatively stronger with <i>Bz</i> than <i>Ey</i>. Other two indices (<i>Ap</i> and <i>AE</i>) correlation is relatively weaker with <i>Bz</i> than <i>Ey</i>. In addition to <i>Ey</i>, another interplanetary parameter, the interplanetary electric field (<i>BV</i>), correlates reasonably well with the <i>Ap</i> and <i>AE</i> indices. Thus, <i>Ey</i> can be universally used as coupling function in all three domains (equatorial, mid-latitude and polar), represented by <i>Dst</i>, <i>Ap</i>, and <i>AE</i> indices, respectively. However, <i>Bz</i> in the equatorial, and <i>BV</i> in the mid-latitude and equatorial regions, may also be considered as alternate coupling functions. Best-fit linear equations obtained between geomagnetic indices and best-related field parameters can be utilized to estimate the expected strength of geomagnetic disturbances in the equatorial, mid-latitude and polar regions using plasma/field observations during passage of ICME associated structures. Furthermore, we investigated the recovery phase of each parameter within each group. We observed a strong correlation between the time constants of the geomagnetic indices, both amongst themselves and with <i>Bz</i>.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 12","pages":"1303 - 1316"},"PeriodicalIF":1.1,"publicationDate":"2025-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143621974","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}