Astronomy Reports最新文献_第2页

Erratum to: On the Generalized Kepler Problem under the Effect of Outer Third-Body Perturbation 勘误：论外部第三体扰动作用下的广义开普勒问题

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924100019

M. R. S. Suzuki

引用次数: 0

Should We Expect Further Acceleration of the Earth’s Rotation in the Coming Years? 我们是否应该期待地球自转在未来几年进一步加速？

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924700884

Z. M. Malkin

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New Look at the Structure of the Nearest Circumstellar Environment of the Weak-Line T Tauri Star V718 Per 弱线金牛座恒星 V718 Per 的最近恒星环环境结构新观察

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924700860

V. P. Grinin, B. S. Safonov, N. V. Efimova, O. Yu. Barsunova, I. A. Strachov, G. A. Borman, S. Yu. Shugarov

{"title":"New Look at the Structure of the Nearest Circumstellar Environment of the Weak-Line T Tauri Star V718 Per","authors":"V. P. Grinin, B. S. Safonov, N. V. Efimova, O. Yu. Barsunova, I. A. Strachov, G. A. Borman, S. Yu. Shugarov","doi":"10.1134/S1063772924700860","DOIUrl":"10.1134/S1063772924700860","url":null,"abstract":"In this paper, we have analyzed the properties of the photometric and spectral variability of young star V718 Per, a member of the cluster IC 348, in terms of its possible binarity. The most realistic is the model where the main component of the V718 Per A system—with an effective temperature of 5200 K—is periodically shielded by two extended dust structures consisting of large particles and moving around the star in resonance with two planets. Their orbital periods are 4.7 years and 213 days. Their ratio with high accuracy is equal to 1 : 8, and the ratio of the large semi-axes is 1 : 4. The masses of the planets have not exceeded (6 ,{{M}_{{{text{Jup}}}}}). At the moments of total eclipses V718 Per A, the radiation of the system has been dominated by a colder component with an effective temperature of (4150 pm 100) K, which has explained the reddening of the star observed in the brightness minima, as well as its spectral changes during brightness weakening. Speckle interferometric observations performed using the 2.5-m telescope of the Sternberg Astronomical Institute have made it possible to estimate the upper limit of the angular distance between the components of the system: ≤0.1('' ), which is equivalent to a projection distance of ≤30 AU. The unique feature of this system has been that the planes of the planetary orbits practically coincide with the line of sight. Such an orientation of the system has been most favorable for measuring fluctuations in the radial velocity of a star caused by the orbital motion of planets, as well as for observing planetary transits along the disk of the main component of the system.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 10","pages":"995 - 1002"},"PeriodicalIF":1.1,"publicationDate":"2024-12-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142844779","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

New Formula for the Angular Velocity of Rotation of Liquid Equilibrium Figures 液体平衡图旋转角速度的新公式

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924700872

B. P. Kondratyev

引用次数: 0

Destruction of Open Star Clusters and the Radius–Mass Relationship 疏散星团的毁灭与半径-质量关系

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924700896

A. V. Tutukov, S. V. Vereshchagin, N. V. Chupina

引用次数: 0

Spot Activity of the Dwarf Star V772 Her 矮星 V772 Her 的光斑活动

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-18 DOI: 10.1134/S1063772924700847

I. Yu. Alekseev, A. V. Kozhevnikova, V. P. Kozhevnikov

引用次数: 0

Kinematics of Fainst Stars of the Sco-Cen Association According to Gaia Catalog 根据盖亚星表的scoc - centa协暗星运动学

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S106377292470077X

V. V. Bobylev, A. T. Bajkova

引用次数: 0

Study of Maser Emission in 18 cm Lines in the Star Formation Region G 109.871+2.114 (Cep A) 恒星形成区G 109.871+2.114 (Cep A) 18 cm谱线脉泽辐射的研究

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S106377292470080X

E. E. Lekht, N. T. Ashimbaeva, V. V. Krasnov, V. R. Shutenkov

{"title":"Study of Maser Emission in 18 cm Lines in the Star Formation Region G 109.871+2.114 (Cep A)","authors":"E. E. Lekht, N. T. Ashimbaeva, V. V. Krasnov, V. R. Shutenkov","doi":"10.1134/S106377292470080X","DOIUrl":"10.1134/S106377292470080X","url":null,"abstract":"The results of the study of the star formation region G 109.871+2.114 (Cep A) in OH lines at 18 cm are presented. Polarization observations (monitoring) were performed with a large Nançay radio telescope (France) in 2007–2024. OH maser emission is highly variable. The structure of the spectrum and the flux density of the individual spectral features are changing. However, the radial velocities of most features changed slightly. Short-term emission flares in individual features were observed. Many features have strong circular polarization, reaching 100%, but have weak linear polarization. A new features at –15.53 km/s and a short-term part at 1.58 km/s with high circular and low linear polarizations were detected in the 1667 MHz line. The spectral features of our monitoring were spatially identified with the maser spots on the Cohen, Argon, and Fish maps. The magnitude of the monotonic decrease in splitting, and, consequently, the longitudinal magnetic field of three Zeeman pairs (–16.2L/–14.25R and –6.94L/–0.82R km/s in the 1665 MHz line and –15.76L/–14.2R in the 1667 MHz line). For the –13.95L/–11.60R pair, no splitting change was detected in the 1665 MHz line. Broadband absorption and emission are observed in the satellite lines of 1612 and 1720 MHz, respectively. A Zeeman pair was also detected in the 1720 MHz line. The position angle (chi ) is calculated for linearly polarized emission of most spectral features in both main lines at 1665 and 1667 MHz. It is shown that the magnetic field in the H II regions is oriented either along the external magnetic field or along the radio jets.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"906 - 924"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790389","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

Effect of the Pseudo Mean Motion on the Dynamics of Perturbed Elliptic Restricted Three-Body Problem 伪平均运动对摄动椭圆型受限三体问题动力学的影响

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700768

Bhavneet Kaur, Sapna Kumari Meena, Ram Krishan Sharma, Rajiv Aggarwal

引用次数: 0

Impact of Star Flare Activity on the Structure of the Hydrogen–Helium Upper Atmosphere of Hot Jupiter 恒星耀斑活动对热木星氢氦高层大气结构的影响

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700793

A. G. Zhilkin, Y. G. Gladysheva, V. I. Shematovich, G. N. Tsurikov, D. V. Bisikalo

{"title":"Impact of Star Flare Activity on the Structure of the Hydrogen–Helium Upper Atmosphere of Hot Jupiter","authors":"A. G. Zhilkin, Y. G. Gladysheva, V. I. Shematovich, G. N. Tsurikov, D. V. Bisikalo","doi":"10.1134/S1063772924700793","DOIUrl":"10.1134/S1063772924700793","url":null,"abstract":"In the paper, the impact of a stellar flare on the upper atmosphere of hot Jupiter has been studied using 1D aeronomic model. The atmosphere has been assumed to have a hydrogen–helium chemical composition, and calculations have been carried out for hot Jupiter HD 209458b. We have examined single and repeated flares, in which the flux of hard UV radiation has increased by 10, 100, and 1000 times compared to the quiescent state of the star. The active phase of the dynamic response of the atmosphere has lasted 12–15 h after the flare, and the characteristic period of relaxation to the initial state has been about a day. From the obtained results, it follows that the flare activity of solar-type stars has not had a significant effect on the evolution of the planetary atmospheres of hot Jupiters. However, the interpretation of transit observations of the disturbed atmospheres of hot Jupiters will make it possible to separate from each other the observational effects associated with the interaction of stellar flares and coronal mass ejections with the upper atmospheres and envelopes of these planets. This will make it possible to determine more accurately the parameters of the stellar wind and coronal mass ejections of solar-type parent stars.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"865 - 877"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790390","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