Pub Date : 2020-04-01DOI: 10.31577/caosp.2020.50.2.400
T. Borkovits, S. Rappaport
During the era of Kepler, TESS, and other related star-monitoring space-based missions, quasi-continuous observations of thousands of known and previously unknown eclipsing binaries for several months (or even years) has led to the discovery of hundreds of compact hierarchical triple (and multiple) star systems. Many of them produce spectacular observational effects that were never (or at least, rarely) seen before, for example: extra outer eclipses; thirdbody perturbation-dominated, large amplitude, non-sinusoidal eclipse timing variations; rapid eclipse depth variations, etc. Successful modeling of these phenomena is a great challenge; however, it does offer substantial astrophysical benefits. In this paper we review our two different approaches to these challenges: one of them is based on the analytical theory of third-body perturbations and is applied exclusively to the eclipse timing variations, while the other is a complex, numerical, spectro-photodynamical modeling of all the available observations of such systems. We discuss some recent results obtained for TESS systems.
{"title":"(Not so) hierarchical stellar multiples seen through the eyes of Kepler, TESS, and other missions.","authors":"T. Borkovits, S. Rappaport","doi":"10.31577/caosp.2020.50.2.400","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.400","url":null,"abstract":"During the era of Kepler, TESS, and other related star-monitoring space-based missions, quasi-continuous observations of thousands of known and previously unknown eclipsing binaries for several months (or even years) has led to the discovery of hundreds of compact hierarchical triple (and multiple) star systems. Many of them produce spectacular observational effects that were never (or at least, rarely) seen before, for example: extra outer eclipses; thirdbody perturbation-dominated, large amplitude, non-sinusoidal eclipse timing variations; rapid eclipse depth variations, etc. Successful modeling of these phenomena is a great challenge; however, it does offer substantial astrophysical benefits. In this paper we review our two different approaches to these challenges: one of them is based on the analytical theory of third-body perturbations and is applied exclusively to the eclipse timing variations, while the other is a complex, numerical, spectro-photodynamical modeling of all the available observations of such systems. We discuss some recent results obtained for TESS systems.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"34 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89901726","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.414
C. Siopis, G. Sadowski, N. Mowlavi, B. Holl, I. Lecoeur-Taibi, L. Eyer
The ESA mission Gaia is expected to detect a few million eclipsing binaries, most of them hitherto unknown. We present an outline of the processing of these objects in the Gaia Data Processing and Analysis Consortium pipeline, with an emphasis on the scientific validation of the software components.
{"title":"Eclipsing binaries in the era of Gaia.","authors":"C. Siopis, G. Sadowski, N. Mowlavi, B. Holl, I. Lecoeur-Taibi, L. Eyer","doi":"10.31577/caosp.2020.50.2.414","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.414","url":null,"abstract":"The ESA mission Gaia is expected to detect a few million eclipsing binaries, most of them hitherto unknown. We present an outline of the processing of these objects in the Gaia Data Processing and Analysis Consortium pipeline, with an emphasis on the scientific validation of the software components.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"38 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79039595","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.405
A. Forró, R. Szabó
The aim of the Kepler Pixel Project is to discover new pulsating and other types of variable stars in the individual pixels of the original Kepler mission. In the framework of the project, 1272 eclipsing binary candidates were identified in the background pixels. After eliminating false positives and those stars that are already present in the Kepler Eclipsing Binary Catalog, we were left with 776 new eclipsing binaries. This is a substantial and significant addition to the 2922 eclipsing binaries present in the catalog. We present the methods we applied, examine the 4-year (Q1-Q17) light curves of selected newly found variable stars. The applied methods are automatic, therefore they can be used in the future to explore the vast amounts of data produced by other space missions (e.g. TESS, later PLATO).
{"title":"Eclipsing binaries hiding in the background: the Kepler Pixel Project.","authors":"A. Forró, R. Szabó","doi":"10.31577/caosp.2020.50.2.405","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.405","url":null,"abstract":"The aim of the Kepler Pixel Project is to discover new pulsating and other types of variable stars in the individual pixels of the original Kepler mission. In the framework of the project, 1272 eclipsing binary candidates were identified in the background pixels. After eliminating false positives and those stars that are already present in the Kepler Eclipsing Binary Catalog, we were left with 776 new eclipsing binaries. This is a substantial and significant addition to the 2922 eclipsing binaries present in the catalog. We present the methods we applied, examine the 4-year (Q1-Q17) light curves of selected newly found variable stars. The applied methods are automatic, therefore they can be used in the future to explore the vast amounts of data produced by other space missions (e.g. TESS, later PLATO).","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"1 1","pages":"481-482"},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88324848","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.419
J. Nuspl, T. Hajdu, T. Hegedüs
The Kepler Eclipsing Binary Catalog Third Revision contains data for about 3000 systems (Prša et al, 2011). Enumerate all the papers connected to the database we could get around 1300 papers in the literature published during the last decade, so its impact is definitely huge. One could suppose that this uniquely large database with unprecedented accuracy would provide a good foundation for detailed studies as it was advocated, e.g. in Wilson (2003), to look for an efficient, effective, and automatic processing of massive database secured by large-scale surveys but ‘Eclipsing binary (EB) modeling naturally partitions into several areas, headed by the overall issue of how to find astrophysically useful numbers.’ (Wilson, 2006) However, the number of studies discussing astrophysical details is much more limited. Pursuing this main goal, we have browsed through the catalog of corrected and detrended light curves in the database, and have found a few typical features created during data processing. These detections demonstrate that one must be careful around the details before using the data directly to deduce any physical conclusion. The artificial side effects contaminate the real data and can mimic otherwise pretty intriguing real effects.
开普勒食双星表第三次修订包含了大约3000个星系的数据(Prša et al, 2011)。列举所有连接到数据库的论文，我们可以找到近十年来发表的1300篇论文，所以它的影响绝对是巨大的。人们可能会认为，这个独特的大型数据库具有前所未有的准确性，将为详细的研究提供良好的基础，因为它被提倡，例如在Wilson(2003)中，寻找一种高效，有效和自动处理大规模调查保护的大型数据库，但“食双星(EB)建模自然分为几个领域，以如何找到天体物理学上有用的数字为首要问题。(Wilson, 2006)然而，讨论天体物理细节的研究数量要有限得多。为了实现这一主要目标，我们浏览了数据库中校正和去趋势光曲线的目录，并发现了一些在数据处理过程中产生的典型特征。这些发现表明，在直接使用数据推断任何物理结论之前，必须仔细考虑细节。人为的副作用污染了真实的数据，并且可以模仿其他非常有趣的真实效果。
{"title":"On some strange features in Kepler EB light curves.","authors":"J. Nuspl, T. Hajdu, T. Hegedüs","doi":"10.31577/caosp.2020.50.2.419","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.419","url":null,"abstract":"The Kepler Eclipsing Binary Catalog Third Revision contains data for about 3000 systems (Prša et al, 2011). Enumerate all the papers connected to the database we could get around 1300 papers in the literature published during the last decade, so its impact is definitely huge. One could suppose that this uniquely large database with unprecedented accuracy would provide a good foundation for detailed studies as it was advocated, e.g. in Wilson (2003), to look for an efficient, effective, and automatic processing of massive database secured by large-scale surveys but ‘Eclipsing binary (EB) modeling naturally partitions into several areas, headed by the overall issue of how to find astrophysically useful numbers.’ (Wilson, 2006) However, the number of studies discussing astrophysical details is much more limited. Pursuing this main goal, we have browsed through the catalog of corrected and detrended light curves in the database, and have found a few typical features created during data processing. These detections demonstrate that one must be careful around the details before using the data directly to deduce any physical conclusion. The artificial side effects contaminate the real data and can mimic otherwise pretty intriguing real effects.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"110 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79317202","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.390
K. Oláh, S. Rappaport, A. Derekas, A. Vanderburg, T. Jacobs, D. LaCourse, M. Kristiansen, H. Schwengeler, I. Terentev
Red giant stars with deep convection zones and rapid rotation maintain a strong surface magnetic field which may alter their observable astrophysical parameters. The resulting lower surface temperature due to spots makes the inferred masses and ages from evolutionary tracks uncertain. Eclipsing binaries having an active giant component can help in finding the stellar mass independently. However, until the recent space missions it was nearly impossible to find such systems from the ground. Since the evolution on the giant branch is rapid, the number of binaries containing giant stars is low. The eclipses, if the inclination allows, are very shallow, on the order of the photometric accuracy from the ground, due to the large brightness difference between a red giant primary and its solar size or smaller secondary. And, the typically acquired data from the ground are not uniform or continuous. In this paper, a few new eclipsing binaries are presented with active giant components observed by TESS and discovered by citizen scientists, which are worthy of further studies.
{"title":"The importance of studying active giant stars in eclipsing binaries -- and the role of citizen scientists in finding them","authors":"K. Oláh, S. Rappaport, A. Derekas, A. Vanderburg, T. Jacobs, D. LaCourse, M. Kristiansen, H. Schwengeler, I. Terentev","doi":"10.31577/caosp.2020.50.2.390","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.390","url":null,"abstract":"Red giant stars with deep convection zones and rapid rotation maintain a strong surface magnetic field which may alter their observable astrophysical parameters. The resulting lower surface temperature due to spots makes the inferred masses and ages from evolutionary tracks uncertain. Eclipsing binaries having an active giant component can help in finding the stellar mass independently. However, until the recent space missions it was nearly impossible to find such systems from the ground. Since the evolution on the giant branch is rapid, the number of binaries containing giant stars is low. The eclipses, if the inclination allows, are very shallow, on the order of the photometric accuracy from the ground, due to the large brightness difference between a red giant primary and its solar size or smaller secondary. And, the typically acquired data from the ground are not uniform or continuous. In this paper, a few new eclipsing binaries are presented with active giant components observed by TESS and discovered by citizen scientists, which are worthy of further studies.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"38 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74342640","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.421
T. Hajdu, T. Borkovits, E. Forgács-dajka, J. Sztakovics, G. Marschalkó, G. Kutrovátz
We report the result of eclipse timing variation (ETV) analyses of OGLE-IV eclipsing binaries (EBs). We have identified around 1000 potential triple (or multiple) system candidates and, in addition, we determined the orbital parameters and we carried out statistical analyses of the properties of the candidates. We found that (i) the distribution of the outer eccentricity has a maximum around e2 = 0.3; (ii) in most cases the estimated outer mass ratio is lower than q2 ∼ 0.5. Besides, we also present some systems that deserve special attention.
{"title":"Hierarchical triple star systems towards the Galactic Bulge through OGLE's eye.","authors":"T. Hajdu, T. Borkovits, E. Forgács-dajka, J. Sztakovics, G. Marschalkó, G. Kutrovátz","doi":"10.31577/caosp.2020.50.2.421","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.421","url":null,"abstract":"We report the result of eclipse timing variation (ETV) analyses of OGLE-IV eclipsing binaries (EBs). We have identified around 1000 potential triple (or multiple) system candidates and, in addition, we determined the orbital parameters and we carried out statistical analyses of the properties of the candidates. We found that (i) the distribution of the outer eccentricity has a maximum around e2 = 0.3; (ii) in most cases the estimated outer mass ratio is lower than q2 ∼ 0.5. Besides, we also present some systems that deserve special attention.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"1 1","pages":"421-425"},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88734748","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.384
Y. Kim, J. Yoon
Efforts at the Chungbuk National University, Korea, to encourage amateur astronomers to participate in astronomical observation are presented. The Chungbuk National University Observatory opened the Jincheon station with 1.0-m and 0.6-m optical telescopes for research and education. The observatory is equipped with a fully automated observation and control system. Since its opening in 2008, the observatory has developed amateur astronomer programs and provided training in astronomical observation. The observatory also aims at stimulating other observatories in Korea to engage in reserach and education. We summarize our programs and future plans regarding professional-amateur collaborations in Korea.
{"title":"Professional-amateur programs at Chungbuk National University","authors":"Y. Kim, J. Yoon","doi":"10.31577/caosp.2020.50.2.384","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.384","url":null,"abstract":"Efforts at the Chungbuk National University, Korea, to encourage amateur astronomers to participate in astronomical observation are presented. The Chungbuk National University Observatory opened the Jincheon station with 1.0-m and 0.6-m optical telescopes for research and education. The observatory is equipped with a fully automated observation and control system. Since its opening in 2008, the observatory has developed amateur astronomer programs and provided training in astronomical observation. The observatory also aims at stimulating other observatories in Korea to engage in reserach and education. We summarize our programs and future plans regarding professional-amateur collaborations in Korea.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"21 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87320169","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.398
H. Kučáková
Introduction of the observatory of Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava.
奥帕瓦西里西亚大学哲学与科学学院物理研究所天文台简介。
{"title":"WHOO! -- White Hole Observatory Opava.","authors":"H. Kučáková","doi":"10.31577/caosp.2020.50.2.398","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.398","url":null,"abstract":"Introduction of the observatory of Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"14 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89491975","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.426
J. Merc, R. Gális, M. Wolf
Symbiotic variables belong to an interesting class of interacting binary stars. At the beginning of this century, a systematic search for these objects was begun and such surveys in the Milky Way and the Local Group have resulted in discoveries of many new symbiotics and dozens of candidates. Because the latest catalogue of symbiotic binaries has been outdated for almost two decades, we decided to prepare a new database of the Galactic and extra-Galactic symbiotic systems. We present it in this work. Our database is available online, allowing it to be up-to-date and available to the astronomical community at any time. The database also includes a web portal that allows easy data access without the necessity for any additional software or formatting of the data.
{"title":"Galactic members in the New Online Database of Symbiotic Variables.","authors":"J. Merc, R. Gális, M. Wolf","doi":"10.31577/caosp.2020.50.2.426","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.426","url":null,"abstract":"Symbiotic variables belong to an interesting class of interacting binary stars. At the beginning of this century, a systematic search for these objects was begun and such surveys in the Milky Way and the Local Group have resulted in discoveries of many new symbiotics and dozens of candidates. Because the latest catalogue of symbiotic binaries has been outdated for almost two decades, we decided to prepare a new database of the Galactic and extra-Galactic symbiotic systems. We present it in this work. Our database is available online, allowing it to be up-to-date and available to the astronomical community at any time. The database also includes a web portal that allows easy data access without the necessity for any additional software or formatting of the data.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"28 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78544082","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 : 2020-04-01DOI: 10.31577/caosp.2020.50.2.409
E. Lalounta, A. Papageorgiou, P. Christopoulou, M. Catelán
We have conducted a survey of overcontact binary systems (EW) with mass ratio = 0.25 from the Catalina Sky Survey (CSS) that are considered strong merger candidates and are probable progenitors of FK Com-type stars and blue stragglers. The discovery of such extreme mass ratio overcontact binaries is vital to resolve the critical mass ratio ambiguity to merge, the mass loss process, and to refine the current theoretical models. So far only a few tens of such systems have been identified. To increase this sample, we selected and derived the physical parameters (mass, temperature and radius ratios, inclination and fill-out factor, along with their respective uncertainties) of 92 newly discovered totally eclipsing low-mass-ratio (LMR) EW systems based on their VCSS light curves, using PHOEBE-0.31a scripter and Monte Carlo methods.
{"title":"An investigation of low-mass-ratio EW systems from the Catalina Sky Survey.","authors":"E. Lalounta, A. Papageorgiou, P. Christopoulou, M. Catelán","doi":"10.31577/caosp.2020.50.2.409","DOIUrl":"https://doi.org/10.31577/caosp.2020.50.2.409","url":null,"abstract":"We have conducted a survey of overcontact binary systems (EW) with mass ratio = 0.25 from the Catalina Sky Survey (CSS) that are considered strong merger candidates and are probable progenitors of FK Com-type stars and blue stragglers. The discovery of such extreme mass ratio overcontact binaries is vital to resolve the critical mass ratio ambiguity to merge, the mass loss process, and to refine the current theoretical models. So far only a few tens of such systems have been identified. To increase this sample, we selected and derived the physical parameters (mass, temperature and radius ratios, inclination and fill-out factor, along with their respective uncertainties) of 92 newly discovered totally eclipsing low-mass-ratio (LMR) EW systems based on their VCSS light curves, using PHOEBE-0.31a scripter and Monte Carlo methods.","PeriodicalId":50617,"journal":{"name":"Contributions of the Astronomical Observatory Skalnate Pleso","volume":"35 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87134834","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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