Astrophysical Bulletin最新文献_第4页

B[e] star CI Cam: a High-Resolution Spectrum Atlas in the Range of 395–780 nm B[e] star CI Cam: 395 ~ 780nm高分辨率光谱图谱

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600619

V. G. Klochkova, A. S. Miroshnichenko, V. N. Komarova, N. S. Tavolzhanskaya

{"title":"B[e] star CI Cam: a High-Resolution Spectrum Atlas in the Range of 395–780 nm","authors":"V. G. Klochkova, A. S. Miroshnichenko, V. N. Komarova, N. S. Tavolzhanskaya","doi":"10.1134/S1990341325600619","DOIUrl":"10.1134/S1990341325600619","url":null,"abstract":"The atlas of the spectrum of the B[e] star CI Cam obtained with the 6-m BTA telescope of the SAO RAS applying the NES spectrograph in the wavelength range of 395–780 nm with a resolution of (lambda/Deltalambdageq 60,000) is presented. The atlas identifies about 400 spectral features and illustrates the diversity of spectral features of the unique star, forming in a complex circumstellar environment. The spectrum is dominated by forceful single-peaked H I, He I emissions and numerous double-peaked permitted and forbidden emission lines of ions of chemical elements starting from the CNO triad up to metals (Mg, Al, Ti, V, Cr, Fe) with ‘‘rectangular’’ profiles. The Fe II and [Fe II] emissions predominate in the spectrum. However, several double-peaked forbidden ion emissions were also detected: [V II], [Cr II], [Ni II]. The atlas is presented graphically, with a separate figure corresponding to each échelle order. A list of identified lines, including a number of known interstellar features is presented in table form. The supergiant status of CI Cam is confirmed by the richness of its spectrum with different features of nitrogen.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 4","pages":"551 - 573"},"PeriodicalIF":1.4,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147341536","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 Massive Binary System WR 20a: Light Curve Analysis in a Colliding Wind Model 大质量双星系统WR 20a：碰撞风模型中的光曲线分析

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600486

I. I. Antokhin, E. A. Antokhina, A. M. Cherepashchuk

{"title":"The Massive Binary System WR 20a: Light Curve Analysis in a Colliding Wind Model","authors":"I. I. Antokhin, E. A. Antokhina, A. M. Cherepashchuk","doi":"10.1134/S1990341325600486","DOIUrl":"10.1134/S1990341325600486","url":null,"abstract":"The article presents the results of the analysis of optical light curves of the massive binary system WR 20a (WN 6ha (+) WN 6ha). The analysis was performed with a binary system model, extending the standard Roche model for the case when both components of the system have powerful stellar winds. The model takes into account the collision of the winds and the influence of orbital motion on the collision zone. The observational light curves in (BVI) filters were taken from previously published papers, in which they were analyzed using the standard Roche model. The main difference between the results of our work and the previous results is that in our model the radii of the components are about 25(%) smaller. As a consequence, the luminosity of the system in our model decreased by approximately 40(%), and the distance to the system by 20(%). In addition, the model was able to successfully describe the observed asymmetry of the light curve with respect to the phases of the conjunctions, which is impossible in the standard Roche model. The model light curves were also compared with the observational curves obtained by the TESS satellite and the ASAS-SN project. It was shown that, taking into account recent studies of interstellar extinction in the direction of the young open cluster Westerlund 2, the distance to WR 20a obtained in our calculations is consistent with the hypothesis that WR 20a is a member of the cluster.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 4","pages":"605 - 619"},"PeriodicalIF":1.4,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147341510","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

Magnetic Field of Chemically Peculiar Stars from SDSS/APOGEE Infrared Survey. I. HD 13404, HD 225114, and BD (boldsymbol{{+}64^{circ}}) 325 SDSS/远地点红外巡天中化学特殊恒星的磁场。1 . HD 13404， HD 225114和BD (boldsymbol{{+}64^{circ}}) 325

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600656

I. I. Romanyuk, I. A. Yakunin, E. P. Korchagina, A. V. Moiseeva, V. N. Aitov

引用次数: 0

Catalog of Average Magnetic Phase Curves of Stars. II. Addendum to the Second Catalog 恒星平均磁相曲线表。2。第二目录增编

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600644

V. D. Bychkov, L. V. Bychkova

引用次数: 0

On the Influence of Component Orbital Motion on the Photometric Variability of DF Tau 分量轨道运动对DF - Tau光度变异性的影响

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600474

M. A. Burlak, K. N. Grankin, A. V. Dodin, N. V. Emelyanov, N. P. Ikonnikova, Ya. A. Lazovik, S. A. Lamzin, B. S. Safonov, I. A. Strakhov

引用次数: 0

Distances of Galaxy Groups and Clusters Measured Using Fundamental Planes 用基本平面测量星系团和星系团的距离

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600309

F. G. Kopylova, A. I. Kopylov

{"title":"Distances of Galaxy Groups and Clusters Measured Using Fundamental Planes","authors":"F. G. Kopylova, A. I. Kopylov","doi":"10.1134/S1990341325600309","DOIUrl":"10.1134/S1990341325600309","url":null,"abstract":"In this paper, we continue our research on constructing the optimal fundamental plane (FP) of galaxy groups and clusters for measuring their distances. This work was carried out using archival data from the SDSS and 2MASX catalogs. We present the fundamental planes (scaling relations of dynamical and photometric parameters) of 205 galaxy groups and clusters ((z<0.15)). We found that in the near infrared ((K)-filter), the distribution of galaxy clusters is well approximated by three-parameter planes of the form (R_{e}proptosigma^{1.01pm 0.05}langle I_{e}rangle{{}^{-0.32pm 0.03}}) and (R_{e}propto N^{0.43pm 0.01}langle I_{e}rangle^{-0.40pm 0.02}) and a four-parameter plane of the form (R_{e}proptosigma^{0.15pm 0.06}langle I_{e}rangle^{-0.39pm 0.02}N^{0.38pm 0.02}). The fundamental planes have logarithmic standard deviations of 0.060, 0.036, and 0.035. If we use the fundamental planes to measure distances of galaxy systems, these deviations correspond to 14(%) and 8(%) errors in the distance of a single cluster. Using the four-parameter fundamental plane, we obtained the scatter of the Hubble constant (H_{0}=70pm 5.6text{ km s}^{-1}) Mpc({}^{-1}). Using three fundamental planes of galaxy clusters, it was found that the velocity of the average drift motion in the three-degree cosmic microwave background (CMB) system of five superclusters of galaxies from the SDSS region is (langle V_{textrm{pec}}rangle={+}241pm 180text{ km s}^{-1}).","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 4","pages":"519 - 529"},"PeriodicalIF":1.4,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147341319","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

Long-Term Monitoring of the Variable Star J022237.31+422234.2 in NGC 891: a New LBV or a Yellow Hypergiant? NGC 891中J022237.31+422234.2变星的长期观测：新的LBV还是黄色超巨星？

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600188

Yu. N. Solovyeva, A. S. Vinokurov, E. O. Dedov, A. S. Medvedev, A. E. Kostenkov, A. N. Sarkisyan

{"title":"Long-Term Monitoring of the Variable Star J022237.31+422234.2 in NGC 891: a New LBV or a Yellow Hypergiant?","authors":"Yu. N. Solovyeva, A. S. Vinokurov, E. O. Dedov, A. S. Medvedev, A. E. Kostenkov, A. N. Sarkisyan","doi":"10.1134/S1990341325600188","DOIUrl":"10.1134/S1990341325600188","url":null,"abstract":"We continue to search for luminous blue variables (LBVs) in the Local Volume galaxies to further study their fundamental parameters in relation to the age of their stellar environments and the metallicity of the gas in their host galaxies. In this paper, we report the discovery of the luminous star J022237.31+422234.2 ((M_{V{textrm{max}}}<{-}10overset{textrm{m}}{.}2)) in the galaxy NGC 891 located at a distance of about 10 Mpc. The study involves data from ground-based and space telescopes (HST, JWST). Over the period from 1997 to 2024, the star exhibited the photometric variability (Delta V=1overset{textrm{m}}{.}12pm 0overset{textrm{m}}{.}06). A statistical analysis of the broadband photometric data revealed a direct correlation between the ((V-I_{c})) color index and the (V)-band brightness of the star, while no significant variability was observed in ((B-V)) and ((V-R_{c})). Based on a comparison of the optical spectrum obtained with the 6-m BTA telescope with a grid of extended atmosphere models, we estimated the photospheric temperature ((8000lesssim T_{textrm{eff}}lesssim 10100text{ K})) and the mass-loss rate ((8times 10^{-5}lesssimdot{M}lesssim 5times 10^{-4}M_{odot}text{ yr}^{-1})). Fitting the observed optical spectral energy distribution with models of extended atmospheres, accounting for interstellar extinction, yielded a bolometric luminosity estimate of (1.1times 10^{6}L_{odot}lesssim Llesssim 2.6times 10^{6}L_{odot}). In the infrared range, a significant excess emission was detected at 1.5–8 (mu)m, which may indicate the presence of a warm dust with a temperature of 1300 K. The observed properties of J022237.31+422234.2 suggest its classification as a yellow hypergiant or an LBV in a cold state.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 4","pages":"530 - 544"},"PeriodicalIF":1.4,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147341316","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

Doubly Discordant S(boldsymbol{H_{0}})ES NGC 4258 Cepheid Relations ((boldsymbol{HVI})) and Impactful Extinction Laws 双重不和谐S (boldsymbol{H_{0}}) ES NGC 4258造父变星关系（(boldsymbol{HVI})）和影响的灭绝规律

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600206

D. Majaess

{"title":"Doubly Discordant S(boldsymbol{H_{0}})ES NGC 4258 Cepheid Relations ((boldsymbol{HVI})) and Impactful Extinction Laws","authors":"D. Majaess","doi":"10.1134/S1990341325600206","DOIUrl":"10.1134/S1990341325600206","url":null,"abstract":"S(H_{0})ES (Supernovae and (H_{0}) for the Equation of State of dark energy) 2016–2022 (HVI) data for classical Cepheids in the keystone galaxy NGC 4258 yield doubly discordant Wesenheit Leavitt functions: (Delta W_{0,H-VI}=-0overset{textrm{m}}{.}13pm 0overset{textrm{m}}{.}02) ((-0overset{textrm{m}}{.}17) unweighted) and that is paired with the previously noted (Delta W_{0,I-VI}simeq-0overset{textrm{m}}{.}3), which in concert with complimentary evidence suggest the 2016 S(H_{0})ES NGC 4258-anchored (H_{0}pmsigma_{H_{0}}) warrants scrutiny (i.e., (sigma_{H_{0}}/{H_{0}}gtrsim 6%)). Cepheid distance uncertainties are further exacerbated by extinction law ambiguities endemic to such Leavitt relations (e.g., NGC 4258), particularly for comparatively obscured variables (e.g., (Delta dgtrsim 4%), reddened Cepheid subsamples in the Milky Way, M 31, NGC 2442, NGC 4424, NGC 5643, NGC 7250). Lastly, during the analysis it was identified that the 2022 S(H_{0})ES database relays incorrect SMC Cepheid photometry.","PeriodicalId":478,"journal":{"name":"Astrophysical Bulletin","volume":"80 4","pages":"545 - 550"},"PeriodicalIF":1.4,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147341320","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

Orbit of the Speckle Interferometric Binary System HIP 10944 散斑干涉双星系统HIP 10944的轨道

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600668

M. D. Butorina, V. V. Dyachenko, A. S. Beskakotov, A. A. Mitrofanova, A. F. Maksimov, Yu. Yu. Balega

引用次数: 0

Evidence for the Symbiotic Nature of 2MASS J21012803(boldsymbol{+})4555377 2MASS J21012803 (boldsymbol{+}) 4555377共生性质的证据

IF 1.4 4区物理与天体物理

Astrophysical Bulletin Pub Date : 2026-02-24 DOI: 10.1134/S1990341325600632

A. M. Tatarnikov, A. A. Tatarnikova, N. A. Maslennikova, A. V. Dodin, M. A. Burlak, A. A. Tatarnikov

引用次数: 0