Pub Date : 2021-12-01DOI: 10.31577/caosp.2021.51.3.186
V. Efremov, O. Popova, D. Glazachev, A. Margonis, J. Oberst, A. Kartashova
V. Efremov, O. Popova, D. Glazachev, A. Margonis, J. Oberst and A. Kartashova 1 Sadovsky Institute of Geosphere Dynamics RAS, Moscow, Russia, (E-mail: efremov.vv@phystech.edu) 2 Moscow Institute of Physics and Technology Moscow, Russia 3 Technische Universität Berlin, Institute of Geodesy and Geoinformation Science Berlin, Germany 4 German Aerospace Center (DLR), Institute of Planetary Research Berlin, Germany 5 Institute of Astronomy RAS Moscow, Russia
{"title":"Small meteor ablation model: Applying to Perseid observations","authors":"V. Efremov, O. Popova, D. Glazachev, A. Margonis, J. Oberst, A. Kartashova","doi":"10.31577/caosp.2021.51.3.186","DOIUrl":"https://doi.org/10.31577/caosp.2021.51.3.186","url":null,"abstract":"V. Efremov, O. Popova, D. Glazachev, A. Margonis, J. Oberst and A. Kartashova 1 Sadovsky Institute of Geosphere Dynamics RAS, Moscow, Russia, (E-mail: efremov.vv@phystech.edu) 2 Moscow Institute of Physics and Technology Moscow, Russia 3 Technische Universität Berlin, Institute of Geodesy and Geoinformation Science Berlin, Germany 4 German Aerospace Center (DLR), Institute of Planetary Research Berlin, Germany 5 Institute of Astronomy RAS Moscow, Russia","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48346291","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 : 2021-12-01DOI: 10.31577/caosp.2021.51.3.266
S. Sichevsky, E. Kanev, V. Shmagin, M. Sachkov
The World Space Observatory for Ultraviolet (WSO–UV) is a space observatory equipped with instrumentation for spectroscopy and for imaging in the UV spectral range. After the Hubble Space Telescope, WSO–UV will be the largest mirror telescope for UV astronomy. Thus, the WSO-UV space observatory will guarantee continuity of UV observation of comets and exoplanets.
{"title":"WSO-UV field camera unit for comet and exoplanet observations","authors":"S. Sichevsky, E. Kanev, V. Shmagin, M. Sachkov","doi":"10.31577/caosp.2021.51.3.266","DOIUrl":"https://doi.org/10.31577/caosp.2021.51.3.266","url":null,"abstract":"The World Space Observatory for Ultraviolet (WSO–UV) is a space observatory equipped with instrumentation for spectroscopy and for imaging in the UV spectral range. After the Hubble Space Telescope, WSO–UV will be the largest mirror telescope for UV astronomy. Thus, the WSO-UV space observatory will guarantee continuity of UV observation of comets and exoplanets.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"43024448","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 : 2021-10-23DOI: 10.31577/caosp.2022.52.1.5
D. Z. cCamurdan, Burcu Ozkardecs Ege University, S. Faculty, D. Astronomy, S. Sciences, Department of Biosphere-Geosphere System Science, Technologies, Faculty of Arts, Sciences, cCanakkale Onsekiz Mart University
This study aims at timing the eclipses of the binary star TU UMi. The times of minima are taken from the literature, from our observations in April 2004 and from TESS observations between 2019 and 2022. The orbital period analysis of the system indicates that there is a cyclic oscillation with an amplitude of 0.0081d and a period of 9.03 yr, accompanied by a continuous decrease at a rate of $dP/dt =-1.12 times 10^{-7},mathrm{d}, mathrm{yr}^{-1}$. We study the secular evolution of the orbital period of the system and the possibility of the existence of a third companion or the magnetic activity cycle of the primary component in the system.
{"title":"Photospheric silicon abundances of upper main-sequence stars derived from Si II 6347/6371 doublet lines","authors":"D. Z. cCamurdan, Burcu Ozkardecs Ege University, S. Faculty, D. Astronomy, S. Sciences, Department of Biosphere-Geosphere System Science, Technologies, Faculty of Arts, Sciences, cCanakkale Onsekiz Mart University","doi":"10.31577/caosp.2022.52.1.5","DOIUrl":"https://doi.org/10.31577/caosp.2022.52.1.5","url":null,"abstract":"This study aims at timing the eclipses of the binary star TU UMi. The times of minima are taken from the literature, from our observations in April 2004 and from TESS observations between 2019 and 2022. The orbital period analysis of the system indicates that there is a cyclic oscillation with an amplitude of 0.0081d and a period of 9.03 yr, accompanied by a continuous decrease at a rate of $dP/dt =-1.12 times 10^{-7},mathrm{d}, mathrm{yr}^{-1}$. We study the secular evolution of the orbital period of the system and the possibility of the existence of a third companion or the magnetic activity cycle of the primary component in the system.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45202943","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 : 2021-06-01DOI: 10.31577/CAOSP.2021.51.2.163
I. Bulut, A. Bulut
. In this study we performed the first detailed photometric and period analysis of the recently discovered eclipsing binary star V2783 Ori. The analysis of the light curve has shown that the system is in a detached configuration, with the orbital eccentricity e = 0.274 ± 0.008. The photometric mass ratio of V2783 Ori determined from the light curve analysis is q = 0.734 ± 0.015. The absolute parameters of the system were obtained as a result of the light curve solution. Absolute parameters were found as follows: masses M 1 = 1.80 ± 0.01 M (cid:12) , M 2 = 1.32 ± 0.01 M (cid:12) , radii R 1 = 2.19 ± 0.10 R (cid:12) , R 2 = 1.91 ± 0.10 R (cid:12) , temperatures T 1 = 8325 ± 100 K and T 2 = 8300 ± 100 K. A comparison of these parameters with theoretical stellar models show that the secondary component is located inside the main-sequence band and still close to ZAMS, while the primary component is located in the middle of ZAMS-TAMS limits. The distance of the system determined from the absolute parameters, d = 1064 ± 150 pc, takes into account the interstellar reddening. The (O–C) diagram was discussed considering all reliable minima times found in the literature and new values for the parameters of the apsidal motion and light-time effect were found. The apsidal motion rate of V2783 Ori is ˙ ω = 0.0063 ± 0.0017 deg cycle − 1 , and it corresponds to an apsidal motion period of U = 656 ± 103 yr. The third body orbital period is 10 ± 2 yr, its minimal mass is 0.82 ± 0.11 M (cid:12) .
． 在这项研究中，我们对最近发现的双星猎户座V2783进行了首次详细的光度和周期分析。光曲线分析表明，该系统处于分离构型，轨道偏心率e = 0.274±0.008。通过光曲线分析得到V2783 Ori的光度质量比为q = 0.734±0.015。通过光曲线求解得到了系统的绝对参数。得到的绝对参数如下:质量m1 = 1.80±0.01 M (cid:12)， m2 = 1.32±0.01 M (cid:12)，半径r1 = 2.19±0.10 R (cid:12)， r2 = 1.91±0.10 R (cid:12)，温度t1 = 8325±100 K, t2 = 8300±100 K。这些参数与理论恒星模型的比较表明，次级分量位于主层序带内，仍然接近ZAMS，而主分量位于ZAMS- tams极限的中间。系统的距离由绝对参数d = 1064±150pc确定，考虑了星际变红。对(O-C)图进行了讨论，考虑了文献中发现的所有可靠的最小时间，并找到了附加运动和光时效应参数的新值。V2783 Ori的附加运动速率为˙ω = 0.0063±0.0017 deg cycle−1，对应的附加运动周期为U = 656±103 yr，第三个天体的轨道周期为10±2 yr，最小质量为0.82±0.11 M (cid:12)。
{"title":"Photometric and period analysis of the eclipsing binary system V2783 Ori","authors":"I. Bulut, A. Bulut","doi":"10.31577/CAOSP.2021.51.2.163","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.2.163","url":null,"abstract":". In this study we performed the first detailed photometric and period analysis of the recently discovered eclipsing binary star V2783 Ori. The analysis of the light curve has shown that the system is in a detached configuration, with the orbital eccentricity e = 0.274 ± 0.008. The photometric mass ratio of V2783 Ori determined from the light curve analysis is q = 0.734 ± 0.015. The absolute parameters of the system were obtained as a result of the light curve solution. Absolute parameters were found as follows: masses M 1 = 1.80 ± 0.01 M (cid:12) , M 2 = 1.32 ± 0.01 M (cid:12) , radii R 1 = 2.19 ± 0.10 R (cid:12) , R 2 = 1.91 ± 0.10 R (cid:12) , temperatures T 1 = 8325 ± 100 K and T 2 = 8300 ± 100 K. A comparison of these parameters with theoretical stellar models show that the secondary component is located inside the main-sequence band and still close to ZAMS, while the primary component is located in the middle of ZAMS-TAMS limits. The distance of the system determined from the absolute parameters, d = 1064 ± 150 pc, takes into account the interstellar reddening. The (O–C) diagram was discussed considering all reliable minima times found in the literature and new values for the parameters of the apsidal motion and light-time effect were found. The apsidal motion rate of V2783 Ori is ˙ ω = 0.0063 ± 0.0017 deg cycle − 1 , and it corresponds to an apsidal motion period of U = 656 ± 103 yr. The third body orbital period is 10 ± 2 yr, its minimal mass is 0.82 ± 0.11 M (cid:12) .","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46716912","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 : 2021-06-01DOI: 10.31577/CAOSP.2021.51.2.118
B. Özkardeş
The analysis of light curves (from TESS, ASAS–SN and KWS databases) of the eclipsing binary V355 And is presented for the first time. The O-C diagram was constructed using all available times of minimum light together with the ones determined in this study, and the revised ephemeris was obtained. The final photometric model describes V355 And as an Algollike type binary star with a detached configuration. Absolute parameters of the components of the system were found to be: masses, M1=1.56 ± 0.01 M and M2=1.38 ± 0.01 M , radii, R1=1.70 ± 0.03 R and R2=1.38 ± 0.03 R , and effective temperatures, T1=6650 ± 200 K and T2=6235 ± 201 K. Considering interstellar extinction the distance to V355 And was computed as 117 ± 7 pc. The evolutionary state of V355 And is also discussed using the Geneva stellar models.
首次利用TESS、ASAS-SN和KWS数据库对V355和食双星的光曲线进行了分析。利用所有可获得的最小光照时间和本研究确定的最小光照时间，构建了星历图，得到了修正后的星历表。最后的光度模型将V355描述为一颗具有分离结构的Algollike型双星。系统各组成部分的绝对参数为:质量M1=1.56±0.01 M, M2=1.38±0.01 M;半径R1=1.70±0.03 R, R2=1.38±0.03 R;有效温度T1=6650±200 K, T2=6235±201 K。考虑星际消光，计算到V355和的距离为117±7pc。用日内瓦恒星模型讨论了V355和的演化状态。
{"title":"V355 And: a neglected detached binary in a multiple star system","authors":"B. Özkardeş","doi":"10.31577/CAOSP.2021.51.2.118","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.2.118","url":null,"abstract":"The analysis of light curves (from TESS, ASAS–SN and KWS databases) of the eclipsing binary V355 And is presented for the first time. The O-C diagram was constructed using all available times of minimum light together with the ones determined in this study, and the revised ephemeris was obtained. The final photometric model describes V355 And as an Algollike type binary star with a detached configuration. Absolute parameters of the components of the system were found to be: masses, M1=1.56 ± 0.01 M and M2=1.38 ± 0.01 M , radii, R1=1.70 ± 0.03 R and R2=1.38 ± 0.03 R , and effective temperatures, T1=6650 ± 200 K and T2=6235 ± 201 K. Considering interstellar extinction the distance to V355 And was computed as 117 ± 7 pc. The evolutionary state of V355 And is also discussed using the Geneva stellar models.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46823248","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 : 2021-01-01DOI: 10.31577/caosp.2021.51.1.7
M. Skulskyy
Spatial gaseous structures in the Beta Lyrae system have been studied with the fact of change in the longitudinal component of the donor's magnetic field during the orbital period in mind. The investigation was based primarily on the study of the dynamics of the circumstellar structures surrounding the binary system as a whole. The special emphasis was placed on the study of complex helium lines, in particular those arising from metastable levels. A number of different observable facts from the ultraviolet to the red spectral region were analyzed. The configuration of the donor magnetic field is a factor that not only enhances mass transfer and influences the formation of spatial gas structures between stellar components but, to some extent, also affects the outflow of matter and the formation of external gas structures around this interacting binary system. Together with previous articles citep{Skulskyy2020a, Skulskyy2020b}, the pieces of evidence of this work, confirming the reflection of magnetically controlled matter in circumbinary structures, define the basis for a coherent picture of the mass exchange between components and outflows of matter outwards
{"title":"Formation of magnetized spatial structures in the Beta Lyrae system. III. Reflection of magnetically controlled matter in circumbinary structures in helium lines, in particular arising from metastable levels","authors":"M. Skulskyy","doi":"10.31577/caosp.2021.51.1.7","DOIUrl":"https://doi.org/10.31577/caosp.2021.51.1.7","url":null,"abstract":"Spatial gaseous structures in the Beta Lyrae system have been studied with the fact of change in the longitudinal component of the donor's magnetic field during the orbital period in mind. The investigation was based primarily on the study of the dynamics of the circumstellar structures surrounding the binary system as a whole. The special emphasis was placed on the study of complex helium lines, in particular those arising from metastable levels. A number of different observable facts from the ultraviolet to the red spectral region were analyzed. The configuration of the donor magnetic field is a factor that not only enhances mass transfer and influences the formation of spatial gas structures between stellar components but, to some extent, also affects the outflow of matter and the formation of external gas structures around this interacting binary system. Together with previous articles citep{Skulskyy2020a, Skulskyy2020b}, the pieces of evidence of this work, confirming the reflection of magnetically controlled matter in circumbinary structures, define the basis for a coherent picture of the mass exchange between components and outflows of matter outwards","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45203025","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 : 2021-01-01DOI: 10.31577/CAOSP.2021.51.1.41
M. Skarka, Janusz Janik, E. Paunzen, V. Glos
The education activities in the form of short and condensed courses such as summer schools are essential parts of the educational process of every scientist. Here we briefly describe the program and the organization of the GATE summer school that was held in a form of virtual meeting between August 8 and 15 in Brno, Czech Republic.
{"title":"The GATE summer school","authors":"M. Skarka, Janusz Janik, E. Paunzen, V. Glos","doi":"10.31577/CAOSP.2021.51.1.41","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.1.41","url":null,"abstract":"The education activities in the form of short and condensed courses such as summer schools are essential parts of the educational process of every scientist. Here we briefly describe the program and the organization of the GATE summer school that was held in a form of virtual meeting between August 8 and 15 in Brno, Czech Republic.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"28 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79348885","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 : 2021-01-01DOI: 10.31577/caosp.2021.51.1.5
A. Skopal, R. Komžík
{"title":"Editorial","authors":"A. Skopal, R. Komžík","doi":"10.31577/caosp.2021.51.1.5","DOIUrl":"https://doi.org/10.31577/caosp.2021.51.1.5","url":null,"abstract":"","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"42606433","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 : 2021-01-01DOI: 10.31577/CAOSP.2021.51.1.68
Pavol Gajdoš, A. Maliuk, M. Vítková, H. Parviainen
We revise parameters of four transiting hot Jupiter planets discovered by ground-based surveys. We use follow-up observations carried by TESS mission together with PyTransit software. Space telescopes like TESS provide better coverage and photometry precision than ground-based telescopes. PyTransit is fast and user-friendly exoplanet transit light curve modelling package, implementing optimised versions of the Gimenéz and the Mandel & Agol transit models. After applying PyTransit to TESS data, our results show an improvement in the exoplanets parameters estimation.
{"title":"Improving light curve parameters of exoplanets based on TESS data","authors":"Pavol Gajdoš, A. Maliuk, M. Vítková, H. Parviainen","doi":"10.31577/CAOSP.2021.51.1.68","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.1.68","url":null,"abstract":"We revise parameters of four transiting hot Jupiter planets discovered by ground-based surveys. We use follow-up observations carried by TESS mission together with PyTransit software. Space telescopes like TESS provide better coverage and photometry precision than ground-based telescopes. PyTransit is fast and user-friendly exoplanet transit light curve modelling package, implementing optimised versions of the Gimenéz and the Mandel & Agol transit models. After applying PyTransit to TESS data, our results show an improvement in the exoplanets parameters estimation.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"100 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75861114","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 : 2020-12-17DOI: 10.31577/CAOSP.2021.51.1.78
O. Maryeva, K. Bicz, C. Xia, M. Baratella, P. Čechvala, K. Vida
The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from {it TESS} mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type objects. Of all flares, 63% were detected in a sample of cool stars ($T_{rm eff}<5000$~K), and 29% -- in stars of spectral type G, while 23% in K-type stars and approximately 34% of all detected flares are in M-type stars. Using the FLATW'RM (FLAre deTection With Ransac Method) flare finding algorithm, we estimated parameters of flares and rotation period of detected flare stars. The flare with the largest amplitude appears on the M3 type EQ,Cha star. Statistical analysis did not reveal any direct correlation between ages, rotation periods and flaring activity.
这项研究致力于利用TESS任务的高节奏光度法在已确认的银河系疏散星团成员中寻找耀斑星。我们分析了136个疏散星团中957个成员的高节奏光曲线。结果发现了56颗耀斑星，其中8颗是炽热的B-A型天体。在所有的耀斑中，63%是在低温恒星($T_{rm eff}<5000$~K)的样本中检测到的，29%是在光谱型G的恒星中检测到的，而23%是在K型恒星中检测到的，大约34%是在m型恒星中检测到的。利用FLATW'RM (FLAre deTection With Ransac Method)耀斑查找算法，估计了被探测到的耀斑恒星的耀斑参数和旋转周期。最大振幅的耀斑出现在M3型EQ，Cha星上。统计分析没有发现年龄、自转周期和耀斑活动之间有任何直接的联系。
{"title":"Flare stars in nearby Galactic open clusters based on TESS data","authors":"O. Maryeva, K. Bicz, C. Xia, M. Baratella, P. Čechvala, K. Vida","doi":"10.31577/CAOSP.2021.51.1.78","DOIUrl":"https://doi.org/10.31577/CAOSP.2021.51.1.78","url":null,"abstract":"The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from {it TESS} mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type objects. Of all flares, 63% were detected in a sample of cool stars ($T_{rm eff}<5000$~K), and 29% -- in stars of spectral type G, while 23% in K-type stars and approximately 34% of all detected flares are in M-type stars. Using the FLATW'RM (FLAre deTection With Ransac Method) flare finding algorithm, we estimated parameters of flares and rotation period of detected flare stars. The flare with the largest amplitude appears on the M3 type EQ,Cha star. Statistical analysis did not reveal any direct correlation between ages, rotation periods and flaring activity.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83017970","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}
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