Pub Date : 2021-10-01DOI: 10.1017/S1743921322000047
I. Vavilova, S. Shatokhina, L. Pakuliak, O. Yizhakevych, I. Eglitis, V. Andruk, Y. Protsyuk
Abstract We present the developed methods of digitization, image processing, reduction, and scientific data mining with the latest reference catalogs, which allowed us to obtain a good positional and photometric accuracy in B-band of 6,500 asteroids down to 17.5 m from the Ukrainian Virtual Observatory database of astroplates. The archive includes FON-Kyiv, FON-Kitab, FON-Dushanbe sky surveys (1981–1996) and astroplates of the Baldone and Tautenburg observatories. For some of asteroids, observations are either completely absent or not enough over the certain time interval to the moments of their official discoveries (about 300 such objects were found). Positional observations during these time scales are highly useful for a more detailed study of the dynamics and orbital parameters of asteroids as well as the obtained photometric parameters are very complementary with present-day data for studying changes in brightness and light curves.
{"title":"Astrometry and photometry of asteroids from the UkrVO database of astroplates","authors":"I. Vavilova, S. Shatokhina, L. Pakuliak, O. Yizhakevych, I. Eglitis, V. Andruk, Y. Protsyuk","doi":"10.1017/S1743921322000047","DOIUrl":"https://doi.org/10.1017/S1743921322000047","url":null,"abstract":"Abstract We present the developed methods of digitization, image processing, reduction, and scientific data mining with the latest reference catalogs, which allowed us to obtain a good positional and photometric accuracy in B-band of 6,500 asteroids down to 17.5 m from the Ukrainian Virtual Observatory database of astroplates. The archive includes FON-Kyiv, FON-Kitab, FON-Dushanbe sky surveys (1981–1996) and astroplates of the Baldone and Tautenburg observatories. For some of asteroids, observations are either completely absent or not enough over the certain time interval to the moments of their official discoveries (about 300 such objects were found). Positional observations during these time scales are highly useful for a more detailed study of the dynamics and orbital parameters of asteroids as well as the obtained photometric parameters are very complementary with present-day data for studying changes in brightness and light curves.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"101 1","pages":"239 - 245"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85880643","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 : 2021-10-01DOI: 10.1017/S174392132200179X
Alessandra Celletti, C. Galeş, Cristian Beaugé, Anne Lemaître
{"title":"IAU volume 15 issue 364 Cover and Front matter","authors":"Alessandra Celletti, C. Galeş, Cristian Beaugé, Anne Lemaître","doi":"10.1017/S174392132200179X","DOIUrl":"https://doi.org/10.1017/S174392132200179X","url":null,"abstract":"","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"1 1","pages":"f1 - f16"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77085333","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 : 2021-10-01DOI: 10.1017/S1743921322000588
A. Celletti, G. Pucacco, T. Vartolomei
Abstract Normal form methods allow one to compute quasi-invariants of a Hamiltonian system, which are referred to as proper elements. The computation of the proper elements turns out to be useful to associate dynamical properties that lead to identify families of space debris, as it was done in the past for families of asteroids. In particular, through proper elements we are able to group fragments generated by the same break-up event and we possibly associate them to a parent body. A qualitative analysis of the results is given by the computation of the Pearson correlation coefficient and the probability of the Kolmogorov-Smirnov statistical test.
{"title":"Back-tracing space debris using proper elements","authors":"A. Celletti, G. Pucacco, T. Vartolomei","doi":"10.1017/S1743921322000588","DOIUrl":"https://doi.org/10.1017/S1743921322000588","url":null,"abstract":"Abstract Normal form methods allow one to compute quasi-invariants of a Hamiltonian system, which are referred to as proper elements. The computation of the proper elements turns out to be useful to associate dynamical properties that lead to identify families of space debris, as it was done in the past for families of asteroids. In particular, through proper elements we are able to group fragments generated by the same break-up event and we possibly associate them to a parent body. A qualitative analysis of the results is given by the computation of the Pearson correlation coefficient and the probability of the Kolmogorov-Smirnov statistical test.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"22 1","pages":"134 - 139"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80938590","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 : 2021-10-01DOI: 10.1017/S1743921321001307
V. Carruba, S. Aljbaae, R. C. Domingos, M. Huaman, W. Barletta
Abstract Close encounters or resonances overlaps can create chaotic motion in small bodies in the Solar System. Approaches that measure the separation rate of trajectories that start infinitesimally near, or changes in the frequency power spectrum of time series, among others, can discover chaotic motion. In this paper, we introduce the ACF index (ACFI), which is based on the auto-correlation function of time series. Auto-correlation coefficients measure the correlation of a time-series with a lagged duplicate of itself. By counting the number of auto-correlation coefficients that are larger than 5% after a certain amount of time has passed, we can assess how the time series auto-correlates with each other. This allows for the detection of chaotic time-series characterized by low ACFI values.
{"title":"Chaos identification through the auto-correlation function indicator (ACFI)","authors":"V. Carruba, S. Aljbaae, R. C. Domingos, M. Huaman, W. Barletta","doi":"10.1017/S1743921321001307","DOIUrl":"https://doi.org/10.1017/S1743921321001307","url":null,"abstract":"Abstract Close encounters or resonances overlaps can create chaotic motion in small bodies in the Solar System. Approaches that measure the separation rate of trajectories that start infinitesimally near, or changes in the frequency power spectrum of time series, among others, can discover chaotic motion. In this paper, we introduce the ACF index (ACFI), which is based on the auto-correlation function of time series. Auto-correlation coefficients measure the correlation of a time-series with a lagged duplicate of itself. By counting the number of auto-correlation coefficients that are larger than 5% after a certain amount of time has passed, we can assess how the time series auto-correlates with each other. This allows for the detection of chaotic time-series characterized by low ACFI values.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"66 1","pages":"108 - 112"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76310937","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 : 2021-10-01DOI: 10.1017/S1743921321001320
A. Rosaev, E. Plávalová
Abstract We have randomly selected 20 close asteroid pairs (younger than 800 kyr) from known pairs, and by the application of backward numerical integration we have calculated their orbits. For the reason of speeding up the process of making the resonances visible, we have used a high value of Yarkowsky drift. The results of the calculation show that only two pairs appear to have a simple resonance with Earth and Jupiter while half of the tested pairs are visibly in the vicinity of three-body resonances. We have found a 2-1J-1M resonance for the pair (56232) 1999 JM31 and (115978) 2003 WQ56. Following our study of the pair (10123) Fideoja and (117306) 2004 VF21, we discovered a different resonance than the 7-2J mean motion resonance previously published: we have proved that this pair is perturbed by 9-6J-4M three body resonance.
{"title":"Some of the most interesting cases of close asteroid pairs perturbed by resonance","authors":"A. Rosaev, E. Plávalová","doi":"10.1017/S1743921321001320","DOIUrl":"https://doi.org/10.1017/S1743921321001320","url":null,"abstract":"Abstract We have randomly selected 20 close asteroid pairs (younger than 800 kyr) from known pairs, and by the application of backward numerical integration we have calculated their orbits. For the reason of speeding up the process of making the resonances visible, we have used a high value of Yarkowsky drift. The results of the calculation show that only two pairs appear to have a simple resonance with Earth and Jupiter while half of the tested pairs are visibly in the vicinity of three-body resonances. We have found a 2-1J-1M resonance for the pair (56232) 1999 JM31 and (115978) 2003 WQ56. Following our study of the pair (10123) Fideoja and (117306) 2004 VF21, we discovered a different resonance than the 7-2J mean motion resonance previously published: we have proved that this pair is perturbed by 9-6J-4M three body resonance.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"542 1","pages":"226 - 231"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76709150","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 : 2021-10-01DOI: 10.1017/S1743921322000758
Stefanie Reiter, C. Lhotka
Abstract The interplanetary magnetic field may cause large amplitude changes in the orbital inclinations of charged dust particles. In order to study this effect in the case of dust grains moving in 1:1 mean motion resonance with planet Jupiter, a simplified semi-analytical model is developed to reduce the full dynamics of the system to the terms containing the information of the secular evolution dominated by the Lorentz force. It was found that while the planet causes variations in all orbital elements, the influence of the magnetic field most heavily impacts the long-term evolution of the inclination and the longitude of the ascending node. The simplified secular-resonant model recreates the oscillations in these parameters very well in comparison to the full solution, despite neglecting the influence of the magnetic field on the other orbital parameters.
{"title":"Latitudinal variations of charged dust in co-orbital resonance with Jupiter","authors":"Stefanie Reiter, C. Lhotka","doi":"10.1017/S1743921322000758","DOIUrl":"https://doi.org/10.1017/S1743921322000758","url":null,"abstract":"Abstract The interplanetary magnetic field may cause large amplitude changes in the orbital inclinations of charged dust particles. In order to study this effect in the case of dust grains moving in 1:1 mean motion resonance with planet Jupiter, a simplified semi-analytical model is developed to reduce the full dynamics of the system to the terms containing the information of the secular evolution dominated by the Lorentz force. It was found that while the planet causes variations in all orbital elements, the influence of the magnetic field most heavily impacts the long-term evolution of the inclination and the longitude of the ascending node. The simplified secular-resonant model recreates the oscillations in these parameters very well in comparison to the full solution, despite neglecting the influence of the magnetic field on the other orbital parameters.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"29 1","pages":"102 - 107"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73685129","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 : 2021-10-01DOI: 10.1017/S1743921322000059
S. Ferraz-Mello
Abstract This paper reviews the basic equations used in the study of the tidal variations of the rotational and orbital elements of a system formed by one star and one close-in planet as given by the creep tide theory and Darwin’s constant time lag (CTL) theory. At the end, it reviews and discusses the determinations of the relaxation factors (and time lags) in the case of host stars and hot Jupiters based on actual observations of orbital decay, stellar rotation and age, etc. It also includes a recollection of the basic facts concerning the variations of the rotation of host stars due to the leakage of angular momentum associated with stellar winds.
{"title":"On Tides and Exoplanets","authors":"S. Ferraz-Mello","doi":"10.1017/S1743921322000059","DOIUrl":"https://doi.org/10.1017/S1743921322000059","url":null,"abstract":"Abstract This paper reviews the basic equations used in the study of the tidal variations of the rotational and orbital elements of a system formed by one star and one close-in planet as given by the creep tide theory and Darwin’s constant time lag (CTL) theory. At the end, it reviews and discusses the determinations of the relaxation factors (and time lags) in the case of host stars and hot Jupiters based on actual observations of orbital decay, stellar rotation and age, etc. It also includes a recollection of the basic facts concerning the variations of the rotation of host stars due to the leakage of angular momentum associated with stellar winds.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"25 1","pages":"20 - 30"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81044936","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 : 2021-10-01DOI: 10.1017/S1743921322000023
M. Vasylenko, Y. Pavlenko, D. Dobrycheva, I. Kulyk, O. Shubina, P. Korsun
Abstract Currently, the Transiting Exoplanet Survey Satellite (TESS) searches for Earth-size planets around nearby dwarf stars. To identify specific weak variations in the light curves of stars, sophisticated data processing methods and analysis of the light curve shapes should be developed and applied. We report some preliminary results of our project to find and identify minima in the light curves of stars collected by TESS and stored in the MAST (Mikulski Archive for Space Telescopes) database. We developed Python code to process the short-cadence (2-min) TESS PDCSAP (Pre-search Data Conditioning Simple Aperture Photometry) light curves. Our code allows us to create test samples to apply machine learning methods to classify minima in the light curves taking into account their morphological signatures. Our approach will be used to find and analyze some sporadic events in the observed light curves originating from transits of comet-like bodies.
目前，凌日系外行星巡天卫星(TESS)在附近的矮星周围寻找地球大小的行星。为了识别恒星光曲线的特定微弱变化，需要开发和应用复杂的数据处理方法和光曲线形状分析。我们报告了我们的项目的一些初步结果，该项目旨在寻找和识别由TESS收集并存储在MAST(米库尔斯基空间望远镜档案)数据库中的恒星的光曲线中的极小值。我们开发了Python代码来处理短节奏(2分钟)TESS PDCSAP (Pre-search Data Conditioning Simple Aperture Photometry)光曲线。我们的代码允许我们创建测试样本，以应用机器学习方法对光照曲线中的最小值进行分类，同时考虑到它们的形态特征。我们的方法将用于发现和分析观测到的源自类彗星天体凌日的光曲线中的一些零星事件。
{"title":"An algorithm for automatic identification of asymmetric transits in the TESS database","authors":"M. Vasylenko, Y. Pavlenko, D. Dobrycheva, I. Kulyk, O. Shubina, P. Korsun","doi":"10.1017/S1743921322000023","DOIUrl":"https://doi.org/10.1017/S1743921322000023","url":null,"abstract":"Abstract Currently, the Transiting Exoplanet Survey Satellite (TESS) searches for Earth-size planets around nearby dwarf stars. To identify specific weak variations in the light curves of stars, sophisticated data processing methods and analysis of the light curve shapes should be developed and applied. We report some preliminary results of our project to find and identify minima in the light curves of stars collected by TESS and stored in the MAST (Mikulski Archive for Space Telescopes) database. We developed Python code to process the short-cadence (2-min) TESS PDCSAP (Pre-search Data Conditioning Simple Aperture Photometry) light curves. Our code allows us to create test samples to apply machine learning methods to classify minima in the light curves taking into account their morphological signatures. Our approach will be used to find and analyze some sporadic events in the observed light curves originating from transits of comet-like bodies.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"21 1","pages":"264 - 266"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86512655","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 : 2021-10-01DOI: 10.1017/S1743921322000011
Z. Makó, J. Salamon
Abstract This paper provides a study on the weak stability transition region in the framework of the planar elliptic restricted three-body problem. We define the lower boundary curve of the weak stability transition region and as a particular case, we determine this curve in the Sun-Earth system. The orbit of the Moon is near the lower boundary of the weak stability transition region.
{"title":"Weak stability transition region near the orbit of the Moon","authors":"Z. Makó, J. Salamon","doi":"10.1017/S1743921322000011","DOIUrl":"https://doi.org/10.1017/S1743921322000011","url":null,"abstract":"Abstract This paper provides a study on the weak stability transition region in the framework of the planar elliptic restricted three-body problem. We define the lower boundary curve of the weak stability transition region and as a particular case, we determine this curve in the Sun-Earth system. The orbit of the Moon is near the lower boundary of the weak stability transition region.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"4 1","pages":"184 - 190"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81310527","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 : 2021-10-01DOI: 10.1017/S1743921321001289
F. Zoppetti, H. Folonier, A. Leiva, C. Beaugé
Abstract Tidal evolution of low-eccentric circumbinary planets is expected to drive the rotational evolution toward a pseudo-synchronous solution. In this work, we present a study of the oscillation amplitudes around this state by considering that the two central stars exert creep tides on the planet. These amplitudes are computed by direct numerical integrations of the creep equations and also by means of the calculation of the coefficients of the periodic terms in this stationary solution. As in the two-body-problem, the planetary spin and lag-angle are observed to have maximum oscillation amplitudes for stiff bodies and almost null oscillation for the gaseous regime, while the opposite behaviour is observed in the equatorial and polar flattenings. Our analytical approximation shows to be very accurate and specially necessary for very-low eccentric planets. However, the magnitudes of the oscillation amplitudes around the pseudo-synchronous solution in the circumbinary problem appears to be very small respect to the mean value. Thus, considering these oscillation in the computation of the tidal energy dissipation may not have a substantial contribution in the results, at least compared to the case in which only the mean values are taken into account.
{"title":"Oscillations around tidal pseudo-synchronous solutions for circumbinary planets","authors":"F. Zoppetti, H. Folonier, A. Leiva, C. Beaugé","doi":"10.1017/S1743921321001289","DOIUrl":"https://doi.org/10.1017/S1743921321001289","url":null,"abstract":"Abstract Tidal evolution of low-eccentric circumbinary planets is expected to drive the rotational evolution toward a pseudo-synchronous solution. In this work, we present a study of the oscillation amplitudes around this state by considering that the two central stars exert creep tides on the planet. These amplitudes are computed by direct numerical integrations of the creep equations and also by means of the calculation of the coefficients of the periodic terms in this stationary solution. As in the two-body-problem, the planetary spin and lag-angle are observed to have maximum oscillation amplitudes for stiff bodies and almost null oscillation for the gaseous regime, while the opposite behaviour is observed in the equatorial and polar flattenings. Our analytical approximation shows to be very accurate and specially necessary for very-low eccentric planets. However, the magnitudes of the oscillation amplitudes around the pseudo-synchronous solution in the circumbinary problem appears to be very small respect to the mean value. Thus, considering these oscillation in the computation of the tidal energy dissipation may not have a substantial contribution in the results, at least compared to the case in which only the mean values are taken into account.","PeriodicalId":20590,"journal":{"name":"Proceedings of the International Astronomical Union","volume":"89 1","pages":"252 - 258"},"PeriodicalIF":0.0,"publicationDate":"2021-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86742538","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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