Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.632
M. Vaňko, T. Pribulla, L. Hambálek, E. Kundra, R. Komžík, Z. Garai, J. Budaj, E. Paunzen, P. Zieliński, J. Zverko
We present a long-term spectroscopic monitoring of seven CP stars in which binarity has either been established or signs of possible companions have been indicated. The primary goal of the survey was to examine the radial velocities (RVs) variations of the stars published earlier and to study multiplicity of the objects.
{"title":"Long-term spectroscopic survey of seven interesting CP stars","authors":"M. Vaňko, T. Pribulla, L. Hambálek, E. Kundra, R. Komžík, Z. Garai, J. Budaj, E. Paunzen, P. Zieliński, J. Zverko","doi":"10.31577/caosp.2020.50.2.632","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.632","url":null,"abstract":"We present a long-term spectroscopic monitoring of seven CP stars in which binarity has either been established or signs of possible companions have been indicated. The primary goal of the survey was to examine the radial velocities (RVs) variations of the stars published earlier and to study multiplicity of the objects.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74332102","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.621
E. Paunzen, E. Niemczura, P. Kołaczek-Szymański, S. Hubrig
HD 66051 (V414 Pup) is an eclipsing and spectroscopic double-lined binary, hosting two chemically peculiar stars: a highly peculiar B star as primary and an Am star as secondary. It also shows out-of-eclipse variability that is due to chemical spots. Using a set of high-resolution spectropolarimetric observations, a weak magnetic field on the primary was found. The investigation of the new high-resolution UVES spectrum of HD 66051 allowed us to decide on the chemical peculiarity type of both components with more reliability.
HD 66051 (V414 Pup)是一颗食相和光谱双星，拥有两颗化学性质奇特的恒星:一颗非常奇特的B星是主恒星，一颗Am星是副恒星。它还显示了由化学斑点引起的月食外的变化。通过一组高分辨率的偏振光谱观测，在原星上发现了一个弱磁场。对HD 66051新的高分辨率紫外光谱的研究使我们能够更可靠地确定两种成分的化学特性类型。
{"title":"The enigmatic highly peculiar binary system HD 66051","authors":"E. Paunzen, E. Niemczura, P. Kołaczek-Szymański, S. Hubrig","doi":"10.31577/caosp.2020.50.2.621","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.621","url":null,"abstract":"HD 66051 (V414 Pup) is an eclipsing and spectroscopic double-lined binary, hosting two chemically peculiar stars: a highly peculiar B star as primary and an Am star as secondary. It also shows out-of-eclipse variability that is due to chemical spots. Using a set of high-resolution spectropolarimetric observations, a weak magnetic field on the primary was found. The investigation of the new high-resolution UVES spectrum of HD 66051 allowed us to decide on the chemical peculiarity type of both components with more reliability.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44974296","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.580
P. Mayer, P. Harmanec, P. Zasche, R. Catalan-Hurtado, B. Barlow, Y. Frémat, M. Wolf, H. Drechsel, R. Chini, A. Nasseri, G. Christie, W. Walker, A. Henden, T. Bohlsen, H. Božić
Using a collection of 79 spectra of the quadruple system QZ Car, we were able – for the first time in the optical region – to measure radial velocities of both components of the eclipsing subsystem Ac, and in combination with the photometric solution to obtain masses and radii of both bodies. We confirm that the Ac binary is a semi-detached system with a brighter primary Ac1 and a more massive secondary Ac2. Variations due to the light-time effect and secular * Based on spectra from observations made with ESO telescopes at La Silla and Paranal Observatories under programmes 076.C-0431(A), 081.C-2003(A), 083.D-0589(A), 089.D0975(A), 095.A-9032(A); the program TYCHO P2; on the BESO spectra and spectra from CTIO, and on Hipparcos, ASAS3 and our V photometry. † Pavel Mayer passed away on the day of his 86th birthday, Nov. 7, 2018 The quadruple system QZ Car 581 changes in the systemic velocities of both binaries, Aa and Ac, allowed us to estimate the period of mutual orbit of binaries Aa and Ac to be about 11700 d. Preliminary improved basic properties of the system and its components are provided.
{"title":"Improved physical properties of the quadruple sub-system with the eclipsing binary QZ Carinae","authors":"P. Mayer, P. Harmanec, P. Zasche, R. Catalan-Hurtado, B. Barlow, Y. Frémat, M. Wolf, H. Drechsel, R. Chini, A. Nasseri, G. Christie, W. Walker, A. Henden, T. Bohlsen, H. Božić","doi":"10.31577/caosp.2020.50.2.580","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.580","url":null,"abstract":"Using a collection of 79 spectra of the quadruple system QZ Car, we were able – for the first time in the optical region – to measure radial velocities of both components of the eclipsing subsystem Ac, and in combination with the photometric solution to obtain masses and radii of both bodies. We confirm that the Ac binary is a semi-detached system with a brighter primary Ac1 and a more massive secondary Ac2. Variations due to the light-time effect and secular * Based on spectra from observations made with ESO telescopes at La Silla and Paranal Observatories under programmes 076.C-0431(A), 081.C-2003(A), 083.D-0589(A), 089.D0975(A), 095.A-9032(A); the program TYCHO P2; on the BESO spectra and spectra from CTIO, and on Hipparcos, ASAS3 and our V photometry. † Pavel Mayer passed away on the day of his 86th birthday, Nov. 7, 2018 The quadruple system QZ Car 581 changes in the systemic velocities of both binaries, Aa and Ac, allowed us to estimate the period of mutual orbit of binaries Aa and Ac to be about 11700 d. Preliminary improved basic properties of the system and its components are provided.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74490030","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.557
K. Andrych, D. Tvardovskyi, L. Chinarova, I. Andronov
We developed the software package MAVKA for the determination of characteristics of extrema (moment of extremum, magnitude) and their errors. The program realizes the application of 11 basic functions for approximation of extrema. We tested all these methods in two parts. In the first part we used generated data sets (various smooth curves with noise). We investigated deviations between generated and computed values of moments of extremum and magnitude, as well as execution time for different extrema parameters. In the second part we used real observations of different variable stars using photometric and visual observations from different databases.
{"title":"MAVKA: Investigation of stellar brightness extrema approximation stability for various methods","authors":"K. Andrych, D. Tvardovskyi, L. Chinarova, I. Andronov","doi":"10.31577/caosp.2020.50.2.557","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.557","url":null,"abstract":"We developed the software package MAVKA for the determination of characteristics of extrema (moment of extremum, magnitude) and their errors. The program realizes the application of 11 basic functions for approximation of extrema. We tested all these methods in two parts. In the first part we used generated data sets (various smooth curves with noise). We investigated deviations between generated and computed values of moments of extremum and magnitude, as well as execution time for different extrema parameters. In the second part we used real observations of different variable stars using photometric and visual observations from different databases.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89526355","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.585
A. Oplištilová, P. Harmanec, P. Mayer, P. Zasche, M. Šlechta, H. Pablo, A. Pigulski
We present an improved model of triple star Delta Orionis A. For the first time we were able to disentangle the very weak spectral lines of the secondary in the blue parts of the optical spectrum and derive a reliable mass ratio q = 0.415. Along with light-curve solutions, based on photometry from the SMEI, MOST and BRITE satellites, we obtained realistic masses and radii of both components of the close binary.
{"title":"Improved model of Delta Orionis","authors":"A. Oplištilová, P. Harmanec, P. Mayer, P. Zasche, M. Šlechta, H. Pablo, A. Pigulski","doi":"10.31577/caosp.2020.50.2.585","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.585","url":null,"abstract":"We present an improved model of triple star Delta Orionis A. For the first time we were able to disentangle the very weak spectral lines of the secondary in the blue parts of the optical spectrum and derive a reliable mass ratio q = 0.415. Along with light-curve solutions, based on photometry from the SMEI, MOST and BRITE satellites, we obtained realistic masses and radii of both components of the close binary.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73054246","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.530
K. Conroy
Eclipsing binary stars allow for the direct measurement of stellar parameters and distances and are therefore an important tool in the calibration of stellar relationships. In benchmark cases, we can achieve a precision of 2-3% in fundamental stellar parameters. Due to tighter constraints caused by mutual eclipse events, systems with additional companions allow achieving precision as low as 0.5%. Triple systems have also been proposed as a mechanism for explaining an overabundance of short-period tight binaries. Despite all of this, we do not yet have a complete model for these multiple star systems that include tight binaries. In order to precisely and accurately model these complex systems, we must take into account several considerations, including: light time effects, perturbations to orbital elements, and the distortion of the stellar surfaces. Including all of these into a comprehensive treatment of triple and higher order systems within PHOEBE is currently under development and planned for an upcoming release.
{"title":"Upcoming support for triple stellar systems in PHOEBE","authors":"K. Conroy","doi":"10.31577/caosp.2020.50.2.530","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.530","url":null,"abstract":"Eclipsing binary stars allow for the direct measurement of stellar parameters and distances and are therefore an important tool in the calibration of stellar relationships. In benchmark cases, we can achieve a precision of 2-3% in fundamental stellar parameters. Due to tighter constraints caused by mutual eclipse events, systems with additional companions allow achieving precision as low as 0.5%. Triple systems have also been proposed as a mechanism for explaining an overabundance of short-period tight binaries. Despite all of this, we do not yet have a complete model for these multiple star systems that include tight binaries. In order to precisely and accurately model these complex systems, we must take into account several considerations, including: light time effects, perturbations to orbital elements, and the distortion of the stellar surfaces. Including all of these into a comprehensive treatment of triple and higher order systems within PHOEBE is currently under development and planned for an upcoming release.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76152665","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.630
M. Skarka, P. Kabáth, E. Paunzen, M. Mašek, J. Žák, J. Janík
HD99458 was recently discovered to be a first object of its kind: a short-period eclipsing binary hosts a spotted, chemically peculiar A-type primary star that is a delta Scuti pulsator, and an M-dwarf secondary. These phenomena should not co-exist at the same time. Based on new photometric data we find that the previously published period of the main pulsation mode is a Nyquist alias of the true period (0.036 d, and not 0.052 d) given by the Kepler sampling.
{"title":"On the first δ Scuti-like pulsating Ap star in an eclipsing binary","authors":"M. Skarka, P. Kabáth, E. Paunzen, M. Mašek, J. Žák, J. Janík","doi":"10.31577/caosp.2020.50.2.630","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.630","url":null,"abstract":"HD99458 was recently discovered to be a first object of its kind: a short-period eclipsing binary hosts a spotted, chemically peculiar A-type primary star that is a delta Scuti pulsator, and an M-dwarf secondary. These phenomena should not co-exist at the same time. Based on new photometric data we find that the previously published period of the main pulsation mode is a Nyquist alias of the true period (0.036 d, and not 0.052 d) given by the Kepler sampling.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73202732","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.535
Özge Güzel, O. Özdarcan
A new, modern graphical user interface (GUI) for the 2015 version of the Wilson-Devinney (WD) code is developed. PyWD2015 is written in Python 2.7 and uses the Qt4 interface framework. At its core, the GUI generates lcin and dcin files from user inputs and sends them to WD, then reads and visualises the output in a user friendly way. It also includes some useful tools for the user, which makes technical aspects of the modelling process significantly easier. While multiple sky surveys and space missions generate, reduce and categorize large amounts of observational data, it’s up to dedicated studies to analyse peculiar or anomalous systems and make further progress in the field of physics of eclipsing binaries. We believe PyWD2015 will be a great “dedicated study” suite for such systems.
{"title":"PyWD2015 -- A new GUI for the Wilson-Devinney code","authors":"Özge Güzel, O. Özdarcan","doi":"10.31577/caosp.2020.50.2.535","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.535","url":null,"abstract":"A new, modern graphical user interface (GUI) for the 2015 version of the Wilson-Devinney (WD) code is developed. PyWD2015 is written in Python 2.7 and uses the Qt4 interface framework. At its core, the GUI generates lcin and dcin files from user inputs and sends them to WD, then reads and visualises the output in a user friendly way. It also includes some useful tools for the user, which makes technical aspects of the modelling process significantly easier. While multiple sky surveys and space missions generate, reduce and categorize large amounts of observational data, it’s up to dedicated studies to analyse peculiar or anomalous systems and make further progress in the field of physics of eclipsing binaries. We believe PyWD2015 will be a great “dedicated study” suite for such systems.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73338134","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.601
I. Volkov
We discuss small anomalies in the multicolour photometric light curves (LCs) of eclipsing binary stars which may indicate the presence of additional satellites in the systems.
我们讨论了食双星的多色光度曲线(lc)中的小异常，这可能表明系统中存在额外的卫星。
{"title":"Search for invisible satellites in eclipsing binary systems using photometric methods","authors":"I. Volkov","doi":"10.31577/caosp.2020.50.2.601","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.601","url":null,"abstract":"We discuss small anomalies in the multicolour photometric light curves (LCs) of eclipsing binary stars which may indicate the presence of additional satellites in the systems.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75279296","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}
Pub Date : 2020-03-01DOI: 10.31577/caosp.2020.50.2.615
A. Kravtsova, I. Volkov, T. Pribulla
Absolute physical and geometrical parameters of the system are derived. BD -20 4369 is a strongly evolved stellar system after the first mass exchange.
{"title":"A new spectroscopic and eclipsing binary BD -20 4369","authors":"A. Kravtsova, I. Volkov, T. Pribulla","doi":"10.31577/caosp.2020.50.2.615","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.615","url":null,"abstract":"Absolute physical and geometrical parameters of the system are derived. BD -20 4369 is a strongly evolved stellar system after the first mass exchange.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73588530","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}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：