Astrophysical Bulletin最新文献_第2页

On the Problems of Classification of Globular Cluster Systems 关于球状星团系统分类的若干问题

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-08-21 DOI: 10.1134/S1990341323600448

I. U. Tadjibaev, S. N. Nuritdinov, A. U. Omonov

引用次数: 0

Fractal Distribution of Stars in the Solar Neighborhood and Random Forces 太阳附近恒星的分形分布和随机力

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-08-21 DOI: 10.1134/S1990341325600152

M. L. Ostashova, A. S. Rastorguev

引用次数: 0

Special Features of the Magnetic Field Structure of the He-r Star HD 37479 (boldsymbol{sigma})Ori E He-r星HD 37479磁场结构的特殊特征(boldsymbol{sigma}) Ori E

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-08-21 DOI: 10.1134/S1990341325600231

Yu. Yu. Glagolevskij, A. F. Nazarenko

引用次数: 0

Deep Photometric and Astrometric Investigation of the Non-relaxed Star Cluster Stock 3 Using Gaia DR3 基于Gaia DR3的非松弛星团3的深度光度和天体测量研究

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-08-21 DOI: 10.1134/S1990341324600704

A. M. H. Ahmed, A. R. Youssef, M. S. El-Nawawy, W. H. Elsanhoury

引用次数: 0

Parameters of Formation of Rayleigh Laser Guide Star System of Adaptive Optics for Zeiss-2000 Telescope of Terskol Peak Observatory Terskol峰天文台蔡司-2000望远镜自适应光学瑞利激光导星系统形成参数

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-08-21 DOI: 10.1134/S1990341325600176

A. V. Larichev, E. A. Kopylov, A. S. Goncharov, L. A. Bolbasova, V. P. Lukin, N. G. Iroshnikov, M. E. Sachkov

引用次数: 0

Optical and X-Ray Variability of Be Stars: (omega) Ori Be星的光学和x射线变异性：(omega) Ori

IF 1.3 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-05-26 DOI: 10.1134/S1990341324600777

A. F. Kholtygin, A. V. Dodin, I. A. Yakunin

引用次数: 0

Kinetic Modeling of Non-Thermal Processes in the Upper Atmosphere of Sub-Neptune (pi) Men c 亚海王星上层大气非热过程的动力学模拟(pi)

IF 1.3 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-05-26 DOI: 10.1134/S1990341324600674

A. A. Avtaeva, V. I. Shematovich

{"title":"Kinetic Modeling of Non-Thermal Processes in the Upper Atmosphere of Sub-Neptune (pi) Men c","authors":"A. A. Avtaeva, V. I. Shematovich","doi":"10.1134/S1990341324600674","DOIUrl":"10.1134/S1990341324600674","url":null,"abstract":"Observations of exoplanets in the ultraviolet (UV) wavelength range provide data about the structure of the exoplanetary atmosphere, as well as the atmospheric escape rate. Observations by the Hubble Space Telescope (HST) carried out in the spectral H Ly(alpha) line for the exoplanet (pi) Men c did not reveal any absorption in the blue and red wings of the line. However, due to the peculiarities of the HST orbit, these observations do not allow us to speak unambiguously about the presence or absence of hydrogen in the exoplanetary atmosphere; they only provide an estimate of the upper limit of the mass velocity for hydrogen in the atmosphere. The exoplanet (pi) Men c falls on the outer boundary of the Fulton division from the sub-Neptune side, which implies the presence of hydrogen in the exoplanetary atmosphere. Based on the assumption that (pi) Men c has a primary hydrogen-helium envelope, we performed kinetic modeling of non-thermal processes in the upper atmosphere of the exoplanet (pi) Men c. We considered the processes of suprathermal particle production in exothermic photochemistry under the action of hard ultraviolet (UV) radiation from the host star, as well as the effect of the stellar wind proton flux penetrating the atmosphere. The non-thermal atmospheric escape caused by the exposure to the hard radiation of the host star turned out to be comparable with the estimates of the escaping atmospheric flux due to the thermal processes. The energy of the stellar wind protons penetrating into the atmosphere is completely spent on heating the atmosphere.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 1","pages":"83 - 93"},"PeriodicalIF":1.3,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144140299","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

Monochromatic X-ray Observations of Solar Cusps 太阳尖角的单色x射线观测

IF 1.3 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-05-26 DOI: 10.1134/S1990341324600911

A. A. Reva, S. A. Bogachev, A. S. Kirichenko, I. P. Loboda

{"title":"Monochromatic X-ray Observations of Solar Cusps","authors":"A. A. Reva, S. A. Bogachev, A. S. Kirichenko, I. P. Loboda","doi":"10.1134/S1990341324600911","DOIUrl":"10.1134/S1990341324600911","url":null,"abstract":"In this work, we investigate the possibility of observing cusps—hot, pointed structures above solar flare loops—using the Mg XII spectroheliograph onboard the ‘‘CORONAS-F’’ satellite. This instrument produced monochromatic images of the solar corona in the Mg XII (lambda) 8.42 (text{AA}) line, which is formed at temperatures exceeding 4 MK. Observations of cusp tips, which are otherwise challenging due to the dominance of the cool coronal background, can aid in the analysis of reconnection dynamics and magnetic field topology. We examined three cusps observed using the Mg XII spectroheliograph and compared them with observations from the Extreme Ultraviolet Imaging Telescope (EIT) and the Soft X-ray Telescope (SXT). We concluded that EIT can observe cusps only when they are located on the limb, while the visibility of cusps in SXT images depends on the relative positioning of the cusps and adjacent coronal structures. In contrast, Mg XII images are free from these issues and are the most suitable for studying cusps. The characteristic sizes and lifetimes of the analyzed cusps are 300–500 Mm and 4–16 hours, respectively. For two cusps, motion of the cusp tip (i.e., the X-point) was observed over 2–3 hours, with characteristic speeds of 10–40 km s({}^{-1}). This suggests that reconnection can occur on timescales of several hours after the impulsive phase of the flare. Using the measured cusp tip velocities, we estimated the magnetic reconnection rate: (M_{A}approx 0.13).","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 1","pages":"104 - 121"},"PeriodicalIF":1.3,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144140301","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

The Nature of S0 Galaxies: an Unusual Case of the Isolated Lenticular Galaxy NGC 6798—a Gas Reservoir without Accretion 50个星系的性质：孤立透镜状星系NGC 6798的一个不寻常的例子——一个没有吸积的气藏

IF 1.3 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-05-26 DOI: 10.1134/S1990341324600935

O. K. Sil’chenko, A. V. Moiseev, D. V. Oparin, A. A. Smirnova, E. A. Maleeva, A. V. Silchenko

{"title":"The Nature of S0 Galaxies: an Unusual Case of the Isolated Lenticular Galaxy NGC 6798—a Gas Reservoir without Accretion","authors":"O. K. Sil’chenko, A. V. Moiseev, D. V. Oparin, A. A. Smirnova, E. A. Maleeva, A. V. Silchenko","doi":"10.1134/S1990341324600935","DOIUrl":"10.1134/S1990341324600935","url":null,"abstract":"We investigated the velocity field of the ionized gas and a star-formation ring in the lenticular galaxy NGC 6798 with a global counter-rotating gas disk. 3D spectroscopy data from the scanning Fabry–Perot interferometer of the 6-m BTA telescope of SAO RAS, as well as the data of narrow-band photometry in the emission lines H(alpha) and [N II] (lambda) 6583 from the MaNGaL mapper of the 2.5-m KGO telescope of SAI MSU were obtained and analyzed. We come to a conclusion that the case of NGC 6798 is consistent with one of the scenarios proposed earlier to explain the origin of lenticular galaxies—the orbital angular momentum of the cold outer gas accreted by the galaxy is too high, preventing it from penetrating into the central disk of the galaxy, where, being compressed by gravitation inside the stellar disk, it could begin to form stars. The weak current star formation that we did detect in NGC 6798 obviously began much later than the event of the formation of a large gas disk. The bar in the center of NGC 6798, and possibly the associated wave of radial gas contraction that we are now detecting in the ring complex of H II regions, is a consequence of a particular event in the life of the galaxy that took place no more than 1.5–2 Gyr ago.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 1","pages":"1 - 13"},"PeriodicalIF":1.3,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144140324","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

Far-Infrared Emission from a Late Supernova Remnant in an Inhomogeneous Medium 非均匀介质中晚期超新星遗迹的远红外辐射

IF 1.3 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2025-05-26 DOI: 10.1134/S199034132460090X

S. A. Drozdov, S. Yu. Dedikov, E. O. Vasiliev

{"title":"Far-Infrared Emission from a Late Supernova Remnant in an Inhomogeneous Medium","authors":"S. A. Drozdov, S. Yu. Dedikov, E. O. Vasiliev","doi":"10.1134/S199034132460090X","DOIUrl":"10.1134/S199034132460090X","url":null,"abstract":"Interstellar dust particles are swept up during the expansion of a supernova (SN) remnant, penetrate behind the shock wave front, where they are heated and destroyed in the hot gas. This leads to a change in the emission properties of such particles. The paper considers the evolution of the infrared (IR) luminosity of an SN remnant expanding in an inhomogeneous interstellar medium with a lognormal distribution of density perturbations. The IR luminosity of the swept up interstellar dust increases rapidly during the first few thousand years after the SN explosion and reaches a maximum. It then decreases due to the destruction of particles in the hot gas and a drop in their emissivity in the cooling gas of the shell. The dependence of the evolution of the IR luminosity of the dust in the remnant on the gas density dispersion ahead of the shock wave front from the SN is shown. It was found that the band centered at 70 (mu)m can be considered as the most optimal for studying late remnants, since the maximum IR luminosity is located within its limits for a significant time (40–50 kyr). During the evolution, the dust temperature changes from 70 to 20 K and weakly depends on the level of inhomogeneity of the medium. During the radiative phase, strong lines of metal ions appear in the remnant spectra against the dust continuum. Their luminosity grows rapidly and exceeds the luminosity of dust in the continuum under the line by approximately 10–10({}^{3}) times. The moment of achieving high luminosity in the lines depends significantly on the inhomogeneity of the medium. The possibilities of observing IR emission both in the dust continuum and in the lines are discussed. It is expected that their ratios will allow us to estimate the magnitude of inhomogeneity of the medium in which the remnant is expanding.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 1","pages":"22 - 37"},"PeriodicalIF":1.3,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144140179","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