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New M-type Periodic Variables of Catalina Sky Survey Database Catalina巡天数据库中新的m型周期变量
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2026-04-21 DOI: 10.1007/s10511-026-09901-9
G. R. Kostandyan
{"title":"New M-type Periodic Variables of Catalina Sky Survey Database","authors":"G. R. Kostandyan","doi":"10.1007/s10511-026-09901-9","DOIUrl":"10.1007/s10511-026-09901-9","url":null,"abstract":"<p>In this paper we continue spectral class determinations for optically faint periodic variables from Catalina Sky Survey (CSS) database for which P ≥ 10 days. Based on Gaia Data Release 3 (DR3) BP/RP spectroscopic data base 169 objects are confirmed as G and K-type stars, 78 objects are confirmed as M-type stars. We have constructed the color-absolute M(G) magnitude (CaMD) diagram and 2MASS data J-H versus H-Ks color-color diagram for new 78 M type stars. By analyzing the two diagrams and Transiting Exoplanet Survey Satellite (TESS) data, we can conclude that 74 objects are M giants and 4 objects are M dwarfs. The ASAS-SN phase dependence light curves analysis confirms 47 stars as Mira-type variables, 25 as Semi-Regulars (SR), two objects as Irregular (IR)-type variables and 4 as Rotating variables (ROT). Two M type dwarfs and 34 giants, show Spectral Energy Distribution (SED) with infrared excess, indicating the existence of circumstellar envelope around them.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 4","pages":"571 - 582"},"PeriodicalIF":0.7,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147828586","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
Interstellar Polarization Around the Bok Globule CB67 布克球状体CB67周围的星际偏振
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2026-04-21 DOI: 10.1007/s10511-026-09900-w
M. S. Prokopjeva, H. A. Krayani, V. B. Il’in, T. Kondratieva, A. K. Sen, R. Gupta
{"title":"Interstellar Polarization Around the Bok Globule CB67","authors":"M. S. Prokopjeva,&nbsp;H. A. Krayani,&nbsp;V. B. Il’in,&nbsp;T. Kondratieva,&nbsp;A. K. Sen,&nbsp;R. Gupta","doi":"10.1007/s10511-026-09900-w","DOIUrl":"10.1007/s10511-026-09900-w","url":null,"abstract":"<p>Original polarimetric data of stars in the vicinity of the Bok globule CB67, located at the periphery of the nearby star-forming region ρ Oph, are considered. Variations of the visual extinction <i>A</i><sub><i>V</i></sub> in the plane of the sky and with distance d are analyzed using various data sources. It is found that a jump in <i>A</i><sub><i>V</i></sub> of about 0<sup>m</sup>.8 at a distance of <i>d</i> ≈ 140 pc is associated with the neutral wind of the Upper Scorpius part of the Sco–Cen OB association. In the outer layers of CB67 (d = 140 pc), this jump increases by more than 0<sup>m</sup>.5–1. The derived parameters of interstellar polarization for 66 stars around CB67 are supplemented with modern data on their distances and interstellar extinction. It is found that the magnetic-field direction in the immediate vicinity (several arcminutes) of CB67 has a position angle θ<sub><i>B</i></sub> = 90 ± 20°, which differs significantly from the mean orientation in a wider (several-degree) region, where <span>(overline{uptheta })</span> ≈ 60° . It is noted that for CB67 the value of θ<sub><i>B</i></sub> agrees better than <span>(overline{uptheta })</span> with the usual correlations between the magnetic-field (polarization) direction and the directions of maximum elongation of clouds and their rotation axes. For CB67, the latter are characterized by θ<sub><i>L</i></sub> ≈ 107° and θ<sub><i>R</i></sub> = 112°, respectively. With the exception of a few stars, the observed degree of polarization P correlates fairly well with <i>A</i><sub><i>V</i></sub>, and the obtained ratios P/<i>A</i><sub><i>V</i></sub> = 0.5–2%/mag are typical of the diffuse interstellar medium.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 4","pages":"554 - 570"},"PeriodicalIF":0.7,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147828581","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 Local Volume Galaxy Census and HST Snap Surveys 本地星系普查和HST快速调查
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2026-04-21 DOI: 10.1007/s10511-026-09898-1
I. D. Karachentsev, M. I. Chazov, V. E. Karachentseva
{"title":"The Local Volume Galaxy Census and HST Snap Surveys","authors":"I. D. Karachentsev,&nbsp;M. I. Chazov,&nbsp;V. E. Karachentseva","doi":"10.1007/s10511-026-09898-1","DOIUrl":"10.1007/s10511-026-09898-1","url":null,"abstract":"<p>We examined F814W and F606W images of dwarf galaxies from the Hubble Space Telescope archive, which were obtained under the HST SNAP programs 17159 to 17797. Among 58 observed dwarfs located outside the Local Group, we found only a few objects that were confidently resolved into stars. We determined two new distances for the galaxies: dw1252+2215 (5.32 ± 0.20 Mpc) and dw1234+3952 (4.34 ± 0.16 Mpc) via the Tip of the Red Giant Branch. They turned out to be new probable dwarf satellites of the nearby luminous spiral galaxies NGC4826 and NGC4736, respectively. We also note that recent SNAP surveys vary in their productivity in measuring new galaxy distances by more than an order of magnitude.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 4","pages":"537 - 542"},"PeriodicalIF":0.7,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147828583","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
Mira Variables in the DFBS Catalogue of Late-Type Stars DFBS迟型星表中的Mira变星
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2026-04-21 DOI: 10.1007/s10511-026-09902-8
K. K. Gigoyan, K. S. Gigoyan, A. Sarkissian, M. Meftah, P. Keckhut, G. Paronyan, F. Rahmatullaeva
{"title":"Mira Variables in the DFBS Catalogue of Late-Type Stars","authors":"K. K. Gigoyan,&nbsp;K. S. Gigoyan,&nbsp;A. Sarkissian,&nbsp;M. Meftah,&nbsp;P. Keckhut,&nbsp;G. Paronyan,&nbsp;F. Rahmatullaeva","doi":"10.1007/s10511-026-09902-8","DOIUrl":"10.1007/s10511-026-09902-8","url":null,"abstract":"<p>We present phase-dependent ASAS-SN light curves, periods and spectral classes for seven Mira-type variables, based on Gaia DR3 BP/RP low-resolution spectra. We also present their spectral energy distributions (SEDs), mass ranges, mass-loss rates, Galactic plane positions, and other important astrophysical parameters. These stars are included in the \"Value-Added Catalogue of Late-Type Stars Found in the Digitized First Byurakan Survey Database\" (Third Edition).</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 4","pages":"583 - 593"},"PeriodicalIF":0.7,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147828584","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
Nonlinear Radiative Transfer in Resonance Lines with Noncoherent Scattering 非相干散射共振线中的非线性辐射传递
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2026-04-21 DOI: 10.1007/s10511-026-09907-3
A. Kh. Khachatryan
{"title":"Nonlinear Radiative Transfer in Resonance Lines with Noncoherent Scattering","authors":"A. Kh. Khachatryan","doi":"10.1007/s10511-026-09907-3","DOIUrl":"10.1007/s10511-026-09907-3","url":null,"abstract":"<p>This paper addresses to the solving of the nonlinear radiative transfer equation in resonance lines under partial frequency redistribution. The existence of a constructive solution to the two-dimensional integral equation is proven for the general case of nonlinearity with non-coherent scattering. Special attention is focused to different kinds of nonlinear dependencies of the source function on the mean intensity. Along with nonlinearity, we also separately consider the cases of coherent, complete, and general frequency redistribution. Based on the theoretical results, numerical simulations are implemented to demonstrate the qualitative and quantitative differences between the linear and nonlinear solutions. Numerical calculations are carried out for the different spectral lines arising in masers, as well as in solar and stellar chromospheres.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 4","pages":"632 - 647"},"PeriodicalIF":0.7,"publicationDate":"2026-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147828536","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 Smooth Bounce: How Anisotropy and f(R,T) Gravity Preserve Perturbations in a Bianchi-V Cosmology 平滑反弹：各向异性和f（R，T）引力如何在Bianchi-V宇宙学中保持微扰
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2025-11-07 DOI: 10.1007/s10511-025-09887-w
S. Sharma, K. Singh, R. K. Tiwari, S. K. Tiwari, A. Beesham
{"title":"The Smooth Bounce: How Anisotropy and f(R,T) Gravity Preserve Perturbations in a Bianchi-V Cosmology","authors":"S. Sharma,&nbsp;K. Singh,&nbsp;R. K. Tiwari,&nbsp;S. K. Tiwari,&nbsp;A. Beesham","doi":"10.1007/s10511-025-09887-w","DOIUrl":"10.1007/s10511-025-09887-w","url":null,"abstract":"<p>In this paper we have examined the Bianchi type-V model within the framework of linear model which is a special case of broader <i>f</i> (<i>R</i>, <i>T</i>) gravity framework proposed by Harko et al. Here we have considered the <i>f</i> (<i>R</i>, <i>T</i>) = <i>R</i>+ 2λ<i>T</i> where λ is an arbitrary constant, <i>R</i> is the Ricci scalar, <i>T</i> is the trace of stress energy momentum tensor. To find the solution of field equations, we have assumed the condition that cosmic jerk parameter <i>j</i> is directly proportional to negative of deceleration parameter <i>q</i>, namely <i>j</i> ∝ – <i>q</i>. Different cases of Hubble parameter <i>H</i>, spacial volume <i>V</i>, deceleration parameter <i>q</i>, energy density ρ, pressure of matter <i>p</i> and cosmological constant Λ are discussed. Also, we have discussed the physical and geometrical properties of the model. Our results match with the observations.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 3","pages":"426 - 443"},"PeriodicalIF":0.7,"publicationDate":"2025-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145555592","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
Atmospheric Mass Loss of Planet WASP-195b 行星WASP-195b的大气质量损失
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2025-10-31 DOI: 10.1007/s10511-025-09881-2
I. S. Savanov, E. S. Dmitrienko
{"title":"Atmospheric Mass Loss of Planet WASP-195b","authors":"I. S. Savanov,&nbsp;E. S. Dmitrienko","doi":"10.1007/s10511-025-09881-2","DOIUrl":"10.1007/s10511-025-09881-2","url":null,"abstract":"<p>The study presents estimates of the atmospheric mass-loss rate for the planet WASP-195 b. The F-type star WASP-195 hosts a planet whose mass is only 0.104 that of Jupiter, yet their radii are comparable. The planet thus has a low mean density (ρ = 0.16± 0.06 g/cm<sup>3</sup>). To evaluate the atmospheric mass outflow, two approaches were applied: (1) an approximate relation corresponding to the energy-limited escape model, and (2) a method based on interpolation of results obtained from a grid of hydrodynamic upper-atmosphere models. The stellar <i>XUV</i> photon fluxes were estimated using an analytical relation linking <i>F</i><sub><i>XUV</i></sub> and the chromospheric activity index <span>({{mathrm{log}R}^{mathrm{^{prime}}}}_{HK})</span>. The obtained estimates of the atmospheric mass-loss rate <i>Ṁ</i> were compared as a function of <span>({{mathrm{log}R}^{mathrm{^{prime}}}}_{HK})</span> variations for both the energy-limited and hydrodynamic escape models. The calculations show that the atmospheric mass loss of the exoplanet is significant even in the case of low chromospheric activity of the host star. The maximum value of <i>Ṁ</i> may reach 7.3·10<sup>11</sup> g/s (according to the hydrodynamic model under conditions of high stellar activity).</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 3","pages":"354 - 359"},"PeriodicalIF":0.7,"publicationDate":"2025-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145555591","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
On Quasiperiodic Variations of Period Derivative of Pulsars 脉冲星周期导数的准周期变化
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2025-10-31 DOI: 10.1007/s10511-025-09886-x
K. M. Shahabasyan
{"title":"On Quasiperiodic Variations of Period Derivative of Pulsars","authors":"K. M. Shahabasyan","doi":"10.1007/s10511-025-09886-x","DOIUrl":"10.1007/s10511-025-09886-x","url":null,"abstract":"<p>Observational data on quasiperiodic variations of the period derivative of pulsars are considered. Characteristic radii of the superfluid regions of pulsars are obtained under the assumption that these variations represent collective elastic oscillations of the superfluid vortex lattice (Tkachenko modes). The derived values of the radii were compared with those obtained from observations of the X-ray satellites NICER and XMM-Newton. These values were also compared with those inferred from the equation of state. The simple model of Tkachenko waves requires further refinement. This method can be used for approximate estimation of pulsar radii in certain cases.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 3","pages":"418 - 425"},"PeriodicalIF":0.7,"publicationDate":"2025-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145555595","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
Special Properties of Magnetic O-Type Star HD149438 磁性o型星HD149438的特殊性能
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2025-10-31 DOI: 10.1007/s10511-025-09882-1
Yu. V. Glagolevskij
{"title":"Special Properties of Magnetic O-Type Star HD149438","authors":"Yu. V. Glagolevskij","doi":"10.1007/s10511-025-09882-1","DOIUrl":"10.1007/s10511-025-09882-1","url":null,"abstract":"<p>We investigate the magnetic field and other physical properties of the star HD 149438 ( τ Sco). The analysis shows that this object exhibits all the key characteristics typical of other known magnetic O-type stars. Furthermore, all magnetic O-type stars display properties closely resembling those of SrCrEu + Si + He-w + He-r peculiar stars, suggesting a common origin and evolutionary pathway for these objects. The results also indicate that the hypotheses proposed in the literature (that magnetic stars originate from close binary systems) are not supported by observational evidence.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 3","pages":"360 - 376"},"PeriodicalIF":0.7,"publicationDate":"2025-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145555599","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
Low-Frequency Type II Radio Bursts and Associated Solar Flares, Coronal Holes, and CMEs During 2001 to 2015 2001年至2015年间的低频II型射电暴和相关的太阳耀斑、日冕洞和cme
IF 0.7 4区 物理与天体物理
Astrophysics Pub Date : 2025-10-31 DOI: 10.1007/s10511-025-09884-z
N. Mittal, V. Verma
{"title":"Low-Frequency Type II Radio Bursts and Associated Solar Flares, Coronal Holes, and CMEs During 2001 to 2015","authors":"N. Mittal,&nbsp;V. Verma","doi":"10.1007/s10511-025-09884-z","DOIUrl":"10.1007/s10511-025-09884-z","url":null,"abstract":"<p>We have analyzed 20 low-frequencies (LF) type-II radio bursts associated with solar coronal mass ejections (CMEs), coronal holes (CHs), and solar flares observed during the solar cycle 23 and solar cycle 24, which consist of the period of year 1997 to year 2015. A total number of 505 types-II radio bursts were observed during the above period out of which only 20 types II radio bursts have frequencies ≤ 1 MHz. The time duration of 20 LF type II bursts ranges from 5 min to 2020 min. On investigation of 17 type-II bursts associated CMEs, solar flares, and coronal holes we also found that 12 types-II burst related CMEs observed when there were CHs and solar flares within 10° and 5 type-II burst-associated CMEs found when there were CHs and solar flares within 30°, respectively. In this paper we have done statistical analysis of low frequency type II radio bursts and related solar phenomena. The LF type-II radio bursts start after the peak time of associated solar flares. In this paper each LF type-II radio burst and other related solar phenomena are seen and analyzed to understand the origin of LF type-II radio bursts from the Sun in the latest scenario of solar heliophysics.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"68 3","pages":"387 - 402"},"PeriodicalIF":0.7,"publicationDate":"2025-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145555598","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
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