Pub Date : 2024-04-01DOI: 10.31577/caosp.2024.54.1.57
L. Neslušan, R. Rudawska, M. Hajduková, S. Ďurišová, T. Jopek
. At times, it becomes necessary to verify the internal consistency of meteor shower characteristics, regardless they are one’s own observations or information taken from the literature. A check of internal consistency also appears desirable when the shower characteristics are reported to the Meteor Data Center (MDC) of the International Astronomical Union (IAU). In this article, we describe and provide software that we have developed, which is capable of performing checks of internal consistency between the mean geocentric parameters (solar longitude, geocentric radiant, and geocentric velocity) and mean orbital elements (perihelion distance, eccentricity, argument of perihelion, longitude of ascending node, and inclination) of a shower or several showers. The program is freely accessible (Fortran77 source code as well as executable static binary code) along with this article or from the IAU MDC web pages.
{"title":"The computer programs to check the internal consistency of the meteor-shower data","authors":"L. Neslušan, R. Rudawska, M. Hajduková, S. Ďurišová, T. Jopek","doi":"10.31577/caosp.2024.54.1.57","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.1.57","url":null,"abstract":". At times, it becomes necessary to verify the internal consistency of meteor shower characteristics, regardless they are one’s own observations or information taken from the literature. A check of internal consistency also appears desirable when the shower characteristics are reported to the Meteor Data Center (MDC) of the International Astronomical Union (IAU). In this article, we describe and provide software that we have developed, which is capable of performing checks of internal consistency between the mean geocentric parameters (solar longitude, geocentric radiant, and geocentric velocity) and mean orbital elements (perihelion distance, eccentricity, argument of perihelion, longitude of ascending node, and inclination) of a shower or several showers. The program is freely accessible (Fortran77 source code as well as executable static binary code) along with this article or from the IAU MDC web pages.","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"1063 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140761030","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.205
V. G. Godunova, A.O. Simon, Y.S. Markus, S. Shugarov, V. Troianskyi, V. Reshetnyk, I.O. Izviekova, B. Zhilyaev, A. Shchurova, M. Husárik, S. Geier, D. Oszkiewicz, D. Tomko
. We report on follow-up studies of transient events and objects, which have been conducted in recent years using ground-based optical observations. BVRI photometry has been performed with small and medium-sized telescopes located in Europe and North America. The purpose of these studies, which are mainly focused on objects of unknown nature, is to reveal features of
{"title":"Photometric and colorimetric studies of target objects using small and medium-size telescopes","authors":"V. G. Godunova, A.O. Simon, Y.S. Markus, S. Shugarov, V. Troianskyi, V. Reshetnyk, I.O. Izviekova, B. Zhilyaev, A. Shchurova, M. Husárik, S. Geier, D. Oszkiewicz, D. Tomko","doi":"10.31577/caosp.2024.54.2.205","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.205","url":null,"abstract":". We report on follow-up studies of transient events and objects, which have been conducted in recent years using ground-based optical observations. BVRI photometry has been performed with small and medium-sized telescopes located in Europe and North America. The purpose of these studies, which are mainly focused on objects of unknown nature, is to reveal features of","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"111 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140463809","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.198
A. Maliuk, V. Krushevska, S. Shugarov, Z. Garai, Ya. Romanyuk, Y. Kuznyetsova, M. Andreev
. We keep investigating the new variable of Delta Scuti type 2MASS J13122513+5443409 discovered by our group previously. We have analyzed the data obtained not only from the relatively small telescopes of Slovakia and Ukraine, but also from the TESS mission. We calculated the pulsation period and amplitude using the Lomb-Scargle periodogram. We found that the dominant period is about 0 . 079 days. However, the oscillations displayed beating, indicating the presence of several pulsation frequencies.
{"title":"Photometric study of the Delta Scuti variable 2MASS J13122513+5443409 in UMa","authors":"A. Maliuk, V. Krushevska, S. Shugarov, Z. Garai, Ya. Romanyuk, Y. Kuznyetsova, M. Andreev","doi":"10.31577/caosp.2024.54.2.198","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.198","url":null,"abstract":". We keep investigating the new variable of Delta Scuti type 2MASS J13122513+5443409 discovered by our group previously. We have analyzed the data obtained not only from the relatively small telescopes of Slovakia and Ukraine, but also from the TESS mission. We calculated the pulsation period and amplitude using the Lomb-Scargle periodogram. We found that the dominant period is about 0 . 079 days. However, the oscillations displayed beating, indicating the presence of several pulsation frequencies.","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"73 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140466526","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.43
T. Pribulla, M. Vaňko, R. Komžík, P. Sivanič
{"title":"High-resolution échelle spectrograph at Skalnaté Pleso Observatory","authors":"T. Pribulla, M. Vaňko, R. Komžík, P. Sivanič","doi":"10.31577/caosp.2024.54.2.43","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.43","url":null,"abstract":"","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"46 13","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140464451","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.47
A. Miroshnichenko, S. Danford, S. Zharikov, A. Aarnio, P. Prendergast, S. Khokhlov, I. A. Gabitova, A. Amantayeva, N. L. Vaidman, S. S. Baktybayev, I. Andronov, L. L. Chinarova, I. Usenko
. Results are reviewed of a long-term program of binary systems observing since 2013 at the 0.81 m telescope of the Three College Observatory in North Carolina, USA, with an ´echelle spectrograph at a medium spectral resolution. The target list includes recognized and suspected binary systems with normal stars (no spectral lines in emission), classical Be stars, and objects with the B[e] phenomenon. The results include refinement of the orbital elements of bright binaries previously observed with photographic plates, further evidence for phased-locked peak intensity variations of double-peaked line profiles in Be binaries, and recent discoveries of binaries among objects with the B[e] phenomenon.
{"title":"A variety of binary targets for small telescopes","authors":"A. Miroshnichenko, S. Danford, S. Zharikov, A. Aarnio, P. Prendergast, S. Khokhlov, I. A. Gabitova, A. Amantayeva, N. L. Vaidman, S. S. Baktybayev, I. Andronov, L. L. Chinarova, I. Usenko","doi":"10.31577/caosp.2024.54.2.47","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.47","url":null,"abstract":". Results are reviewed of a long-term program of binary systems observing since 2013 at the 0.81 m telescope of the Three College Observatory in North Carolina, USA, with an ´echelle spectrograph at a medium spectral resolution. The target list includes recognized and suspected binary systems with normal stars (no spectral lines in emission), classical Be stars, and objects with the B[e] phenomenon. The results include refinement of the orbital elements of bright binaries previously observed with photographic plates, further evidence for phased-locked peak intensity variations of double-peaked line profiles in Be binaries, and recent discoveries of binaries among objects with the B[e] phenomenon.","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"276 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140468917","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.213
V. Marsakova, S. Shugarov, I. Andronov
,
,
{"title":"Multiwavelength research of the cyclic variability of symbiotic nova RT Ser","authors":"V. Marsakova, S. Shugarov, I. Andronov","doi":"10.31577/caosp.2024.54.2.213","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.213","url":null,"abstract":",","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"877 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140467643","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.171
M. Vaňko, T. Pribulla, N. Shagatova, R. Komžík, P. Dubovský
,
,
{"title":"FM CMa: hot and massive eclipsing binary with a pulsating component","authors":"M. Vaňko, T. Pribulla, N. Shagatova, R. Komžík, P. Dubovský","doi":"10.31577/caosp.2024.54.2.171","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.171","url":null,"abstract":",","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"363 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140468468","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.186
M. Tomova, K. Stoyanov, Y. Nikolov, P. Kaygorodov
. RS Oph is a recurrent symbiotic novae which underwent its last optical eruption in August 2021. The early H α spectroscopy of the system (at days 11–15 of the outburst) reveals satellite line components at the velocity position of about ± 2400 km s − 1 which are an indication of bipolar collimated outflow. We derived some parameters of the outflows and system’s components and their evolution during our observation.
.RS Oph 是一个周期性共生新星，它的最后一次光学爆发发生在 2021 年 8 月。该系统的早期 H α 光谱（爆发的第 11-15 天）显示了速度位置约为± 2400 km s - 1 的卫星线成分，这是双极准直外流的迹象。我们推导出了外流和系统成分的一些参数，以及它们在观测过程中的演变情况。
{"title":"Optical observations of RS Oph after its 2021 outburst","authors":"M. Tomova, K. Stoyanov, Y. Nikolov, P. Kaygorodov","doi":"10.31577/caosp.2024.54.2.186","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.186","url":null,"abstract":". RS Oph is a recurrent symbiotic novae which underwent its last optical eruption in August 2021. The early H α spectroscopy of the system (at days 11–15 of the outburst) reveals satellite line components at the velocity position of about ± 2400 km s − 1 which are an indication of bipolar collimated outflow. We derived some parameters of the outflows and system’s components and their evolution during our observation.","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"205 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140468739","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.175
L’. Hamb´alek, T. Pribulla
. We have used a Roche-geometry code to pre-generate light curves of contact binary stars using only mass ratio q , fill out f of the Roche lobes, and the inclination i of the orbital plane. We have parametrized TESS light curves of several binaries with a trigonometric polynomial. We used our code UNiQUE to find the best fit of the overall shape of the observed light curve and its associated parameters ( q , f , i ). We compared these parameters to those from a rigorous modelling of our selected objects with known mass ratio q sp inferred from spectra. The method is useful to find a close solution before the full modelling. We also got an indication of possible third light present in a system.
.我们利用罗氏几何代码，仅使用质量比 q、罗氏裂片的满度 f 和轨道平面的倾角 i 就预先生成了接触双星的光变曲线。我们用三角多项式对几颗双星的 TESS 光曲线进行了参数化。我们使用 UNiQUE 代码找出了观测到的光曲线整体形状及其相关参数 ( q , f , i ) 的最佳值。我们将这些参数与从光谱中推断出的已知质量比 q sp 的选定天体的严格建模参数进行了比较。这种方法有助于在全面建模之前找到一个接近的解决方案。我们还得到了一个系统中可能存在的第三光的指示。
{"title":"The uniqueness of determination of the photometric mass ratio of contact binary stars with applications to selected binaries","authors":"L’. Hamb´alek, T. Pribulla","doi":"10.31577/caosp.2024.54.2.175","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.175","url":null,"abstract":". We have used a Roche-geometry code to pre-generate light curves of contact binary stars using only mass ratio q , fill out f of the Roche lobes, and the inclination i of the orbital plane. We have parametrized TESS light curves of several binaries with a trigonometric polynomial. We used our code UNiQUE to find the best fit of the overall shape of the observed light curve and its associated parameters ( q , f , i ). We compared these parameters to those from a rigorous modelling of our selected objects with known mass ratio q sp inferred from spectra. The method is useful to find a close solution before the full modelling. We also got an indication of possible third light present in a system.","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"85 10","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140469626","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-02-01DOI: 10.31577/caosp.2024.54.2.150
Z. Garai, H. Osborn, A. Tuson, S. Ulmer-Moll, The Cheops Consortium
{"title":"Confirming long-period transiting exoplanets with TESS and CHEOPS. The case of HD 22946 d","authors":"Z. Garai, H. Osborn, A. Tuson, S. Ulmer-Moll, The Cheops Consortium","doi":"10.31577/caosp.2024.54.2.150","DOIUrl":"https://doi.org/10.31577/caosp.2024.54.2.150","url":null,"abstract":"","PeriodicalId":515045,"journal":{"name":"Contributions of the Astronomical Observatory Skalnaté Pleso","volume":"80 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140466339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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