Contributions of the Astronomical Observatory Skalnate Pleso最新文献_第5页

Asteroseismology of the heartbeat star KIC 5006817 心跳星KIC 5006817的星震学

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-11-17 DOI: 10.31577/CAOSP.2021.51.1.45

J. Merc, Cs. Kalup, R. Rathour, J. S. Sánchez Arias, P. Beck

{"title":"Asteroseismology of the heartbeat star KIC 5006817","authors":"J. Merc, Cs. Kalup, R. Rathour, J. S. Sánchez Arias, P. Beck","doi":"10.31577/CAOSP.2021.51.1.45","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.1.45","url":null,"abstract":"This paper summarizes the project work on asteroseismology at the ERASMUS+ GATE 2020 Summer school on space satellite data. The aim was to do a global asteroseismic analysis of KIC 5006817 and quantify its stellar properties using the high-quality, state of the art space missions data. We employed the aperture photometry to analyze the data from the Kepler space telescope and the Transiting Exoplanet Survey Satellite (TESS). Using the lightkurve Python package, we have derived the asteroseismic parameters and calculated the stellar parameters using the scaling relations. Our analysis of KIC 5006817 confirmed its classification as a heartbeat binary. The rich oscillation spectrum facilitate estimating power excess ($nu_{rm max}$) at 145.50$pm$0.50 $mu$Hz and large frequency separation ($Deltanu$) to be 11.63$pm$0.10 $mu$Hz. Our results showed that the primary component is a low-luminosity, red-giant branch star with a mass, radius, surface gravity, and luminosity of 1.53$pm$0.07 M$_odot$, 5.91$pm$0.12 R$_odot$, 3.08$pm$0.01 dex, and 19.66$pm$0.73 L$_odot$, respectively. The orbital period of the system is 94.83$pm$0.05 d.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-11-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78271599","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: 4

What we can learn from eclipsing binaries in large surveys: The case of EA Catalina systems 我们可以从大型调查中的食双星中学到什么:以EA Catalina系统为例

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-11-01 DOI: 10.31577/caosp.2020.50.4.774

A. Papageorgiou, P. Christopoulou, M. Catelán, A. Drake, S. Djorgovski

引用次数: 0

Substellar and stellar companions in eclipsing binaries 食双星中的亚恒星和伴星

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-11-01 DOI: 10.31577/caosp.2020.50.4.772

K. Zervas, E. Christopoulou, A. Papageorgiou

引用次数: 0

Exact solution for the rotating polytropes with index unity, its approximations and some applications 具有指数单位的旋转多面体的精确解及其近似和一些应用

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-11-01 DOI: 10.31577/caosp.2020.50.4.748

M. Vavrukh, D. Dzikovskyi

{"title":"Exact solution for the rotating polytropes with index unity, its approximations and some applications","authors":"M. Vavrukh, D. Dzikovskyi","doi":"10.31577/caosp.2020.50.4.748","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.4.748","url":null,"abstract":". The fundamental stages of development of the polytropic theory of stars with axial rotation are considered as a generalization of the Lane-Emden theory. The solution of the diﬀerential equilibrium equation for the polytropic star model with index n = 1 and axial rotation with the angular velocity ω is presented in the form of inﬁnite series of the Legendre polynomials and the spherical Bessel functions. Two variants of the approximate solution in the form of the ﬁnite number of terms are proposed. Integration constants were found in a self-consistent way using the integral form of the equilibrium equation and the iteration numerical method. Dependence of the geometrical and physical characteristics of the model on the dimensionless angular velocity Ω = ω (2 πGρ c ) − 1 / 2 (where ρ c is the density in the centre) is analyzed. A comparison with the results of other authors is performed. The obtained critical value of the angular velocity Ω max , when an instability occurs is smaller than in other works (Chandrasekhar, 1933; James, 1964, and et al.). The inverse problem is also considered – a determination of the polytropic model parameters for individual stars based on the solution of the equilibrium equation according to the values of their masses and radii, which are known from observations. In particular, the model parameters for the star α Eri, as well as a similar “class” of the star models of types O5 ÷ G0, were determined. The solution of the equilibrium equation for the polytrope n = 1+ δ (where δ is a small value) is obtained using the method of perturbation theory.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44347310","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: 6

Formation of magnetized spatial structures in the Beta Lyrae system. II. Reflection of magnetically controlled structures in the visible spectrum 天琴座β星系中磁化空间结构的形成。2磁控制结构在可见光谱中的反射

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-08-20 DOI: 10.31577/caosp.2020.50.4.717

M. Skulskyy

{"title":"Formation of magnetized spatial structures in the Beta Lyrae system. II. Reflection of magnetically controlled structures in the visible spectrum","authors":"M. Skulskyy","doi":"10.31577/caosp.2020.50.4.717","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.4.717","url":null,"abstract":"This article proposes a picture of magnetized accretion structures formed during the mass transfer in the Beta Lyrae system. It is shown that the structure of the gaseous flows between the donor and the gainer is due to the spatial configuration of the donor magnetic field. Its dipole axis is deviated substantially from the line joining the centers of the components and is inclined to the orbital plane of the binary system; the center of the magnetic dipole is displaced from the donor center toward the gainer. The surface around the donor magnetic pole, which is close to the gainer, is a region of an additional matter loss from the donor surface. The effective collision of the magnetized plasma with the accretion disk is enhanced by the fast counter-rotation of this disk, especially in the secondary quadrature phases, in which the high-temperature medium and the system of formed accretion flows are observed. This concept is demonstrated, primarily, in the obvious correlations between the phase variability of the donor magnetic field and the corresponding variability of the dynamic and energy characteristics of the various complex lines. This refers to the behavior of the radial velocity curves of the emission-absorption lines formed in the gaseous structures of type H$alpha$, HeI $lambda$ 7065, or the variability of their equivalent width and intensity, and the variability of conventional absorption lines of the donor atmosphere. This is true for the phase variability of the absolute flux in the H$alpha$ emission line and the fast varying of the continuum in the H$alpha$ region as certain parameters, which reflect the phase variability of the donor magnetic field. This approach made it possible to determine the phase boundaries of the location of the magnetic polar region on the donor surface above which the matter outflows are formed.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-08-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41951487","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

Editorial 社论

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-07-01 DOI: 10.31577/caosp.2020.50.3.647

A. Skopal, R. Komžík

引用次数: 0

Note on magnitude estimation on digitized astronomical photographic plates 数字天文照相底片的星等估计注记

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-07-01 DOI: 10.31577/caosp.2020.50.3.704

R. Hudec, E. Splittgerber

引用次数: 1

Formation of magnetized spatial structures in the Beta Lyrae system. I. Observation as a research background of this phenomenon 贝塔天琴座系统中磁化空间结构的形成。一、作为这一现象研究背景的观察

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-05-21 DOI: 10.31577/caosp.2020.50.3.681

M. Skulskyy

{"title":"Formation of magnetized spatial structures in the Beta Lyrae system. I. Observation as a research background of this phenomenon","authors":"M. Skulskyy","doi":"10.31577/caosp.2020.50.3.681","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.3.681","url":null,"abstract":"The discovery of the donor magnetic field has repeatedly posed the task of a thorough study of the phenomenon, which is based on the concept of the influence of the magnetic field on the processes of the formation of gaseous structures and mass transfer in the Beta Lyrae system. This article provides an overview, analysis, and synthesis of the results of a variety of long-term observations as a necessary basis for further clarification of issues aimed primarily at the study of magnetized gaseous structures. As a part of such a study, it was found that the structure of the gaseous flows between the donor and the gainer varies in some way depending on the phases of the orbital period; and, accordingly, that the donor magnetic field influences the formation of these moving magnetized structures. The analysis of the masses of both components for use in further scientific works suggests that the following values are optimal: 2.9 M_sun for the donor and 13 M_sun for the gainer. The study of satellite lines as a certain phenomenon leads to the fact that the accretion disk surrounding the gainer consists of two parts: the external satellite disk and the internal massive opaque disk. From the analysis of all observations and studies of the magnetic field, observations on the 6-m telescope can be considered the most reliable. They have formed the spatial configuration of the donor magnetic field, which is important for studying and understanding the features of the mass transfer in this interacting system. Further evidence regarding the picture of the magnetized accretion structures as the special phenomenon will be presented in the following articles.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43089791","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: 2

Close eclipsing binary BD And: a triple system 近食双星BD和:一个三重系统

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-05-15 DOI: 10.31577/CAOSP.2020.50.3.649

T. Pribulla, L. Hambalek, E. Guenther, R. Komžík, E. Kundra, J. Nedoroščík, V. Perdelwitz, M. Vaňko

{"title":"Close eclipsing binary BD And: a triple system","authors":"T. Pribulla, L. Hambalek, E. Guenther, R. Komžík, E. Kundra, J. Nedoroščík, V. Perdelwitz, M. Vaňko","doi":"10.31577/CAOSP.2020.50.3.649","DOIUrl":"https://doi.org/10.31577/CAOSP.2020.50.3.649","url":null,"abstract":"BD And is a fairly bright (V = 10.8), active and close (P = 0.9258 days) eclipsing binary. The cyclic variability of the apparent orbital period as well as third light in the light curves indicate the presence of an additional late-type component. The principal aim is the spectroscopic testing of the third-body hypothesis and determination of absolute stellar parameters for both components of the eclipsing binary. First medium and high-resolution spectroscopy of the system was obtained. The broadening-function technique appropriate for heavily-broadened spectra of close binaries was used. The radial velocities were determined fitting the Gaussian functions and rotational profiles to the broadening functions. A limited amount of photometric data has also been obtained. Although the photometric observations were focused on the obtaining the timing information, a cursory light-curve analysis was also performed. Extracted broadening functions clearly show the presence of a third, slowly-rotating component. Its radial velocity is within error of the systemic velocity of the eclipsing pair, strongly supporting the physical bond. The observed systemic radial-velocity and third-component changes do not support the 9 year orbit found from the timing variability. Masses of the components of the eclipsing pair are determined with about 0.5% precision. Further characterization of the system would require long-term photometric and spectroscopic monitoring.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47987388","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

LAMOST J202629.80+423652.0 is not a symbiotic star LAMOST J202629.80+423652.0不是一颗共生恒星

IF 0.5 4区物理与天体物理

Contributions of the Astronomical Observatory Skalnate Pleso Pub Date : 2020-04-22 DOI: 10.31577/CAOSP.2020.50.3.672

V. Andreoli, U. Munari

引用次数: 2