Pub Date : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.12
Marios Chatzikos, Stefano Bianchi, Francesco Camilloni, Priyanka Chakraborty, Chamani M. Gunasekera, Francisco Guzmán, Jonathan S. Milby, Arnab Sarkar, Gargi Shaw, Peter A. M. van Hoof, Gary J. Ferland
We describe the 2023 release of the spectral synthesis code Cloudy. Since the previous major release, migrations of our online services motivated us to adopt git as our version control system. This change alone led us to adopt an annual release scheme, accompanied by a short release paper, the present being the inaugural. Significant changes to our atomic and molecular data have improved the accuracy of Cloudy predictions: we have upgraded our instance of the Chianti database from version 7 to 10; our H- and He-like collisional rates to improved theoretical values; our molecular data to the most recent LAMDA database, and several chemical reaction rates to their most recent UDfA and KiDA values. Finally, we describe our progress on upgrading Cloudy's capabilities to meet the requirements of the X-ray microcalorimeters aboard the upcoming XRISM and Athena missions, and outline future developments that will make Cloudy of use to the X-ray community.
{"title":"THE 2023 RELEASE OF Cloudy","authors":"Marios Chatzikos, Stefano Bianchi, Francesco Camilloni, Priyanka Chakraborty, Chamani M. Gunasekera, Francisco Guzmán, Jonathan S. Milby, Arnab Sarkar, Gargi Shaw, Peter A. M. van Hoof, Gary J. Ferland","doi":"10.22201/ia.01851101p.2023.59.02.12","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.12","url":null,"abstract":"We describe the 2023 release of the spectral synthesis code Cloudy. Since the previous major release, migrations of our online services motivated us to adopt git as our version control system. This change alone led us to adopt an annual release scheme, accompanied by a short release paper, the present being the inaugural. Significant changes to our atomic and molecular data have improved the accuracy of Cloudy predictions: we have upgraded our instance of the Chianti database from version 7 to 10; our H- and He-like collisional rates to improved theoretical values; our molecular data to the most recent LAMDA database, and several chemical reaction rates to their most recent UDfA and KiDA values. Finally, we describe our progress on upgrading Cloudy's capabilities to meet the requirements of the X-ray microcalorimeters aboard the upcoming XRISM and Athena missions, and outline future developments that will make Cloudy of use to the X-ray community.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"66 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054390","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.03
Ritika Sethi, D. Bisht, Geeta Rangwal, A. Raj
This paper investigates a poorly studied open cluster, NGC 5288, using 2MASS JHKS and the recently released Gaia DR3 astrometric and photometric data. The mean proper motions in right ascension and declination are estimated as (-3.840 ± 0.230) and (-1.934 ± 0.162) mas yr-1 respectively. We also derive the age and distance of the cluster as 510 ± 190 Myr and 2.64 ± 0.11 kpc, using color-magnitude diagrams (CMDs). We also obtain the distance as 2.77 ± 0.42 kpc using the parallax method. Interstellar reddening E(B ‒ V) in the direction of the cluster is determined as 0.45 mag using the ((J ‒ H), (J ‒ K)) color-color diagram. We find the mass function slope for main-sequence stars as 1.39 ± 0.29 within the mass range 1.0-2.7 M☉, which agrees with Salpeter's value within the uncertainty. Galactic orbits are derived using the Galactic potential model, indicating that NGC 5288 follows a circular path around the Galactic center.
{"title":"A DEEP STUDY OF THE OPEN CLUSTER NGC 5288 USING PHOTOMETRIC AND ASTROMETRIC DATA FROM GAIA DR3 AND 2MASS","authors":"Ritika Sethi, D. Bisht, Geeta Rangwal, A. Raj","doi":"10.22201/ia.01851101p.2023.59.02.03","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.03","url":null,"abstract":"This paper investigates a poorly studied open cluster, NGC 5288, using 2MASS JHKS and the recently released Gaia DR3 astrometric and photometric data. The mean proper motions in right ascension and declination are estimated as (-3.840 ± 0.230) and (-1.934 ± 0.162) mas yr-1 respectively. We also derive the age and distance of the cluster as 510 ± 190 Myr and 2.64 ± 0.11 kpc, using color-magnitude diagrams (CMDs). We also obtain the distance as 2.77 ± 0.42 kpc using the parallax method. Interstellar reddening E(B ‒ V) in the direction of the cluster is determined as 0.45 mag using the ((J ‒ H), (J ‒ K)) color-color diagram. We find the mass function slope for main-sequence stars as 1.39 ± 0.29 within the mass range 1.0-2.7 M☉, which agrees with Salpeter's value within the uncertainty. Galactic orbits are derived using the Galactic potential model, indicating that NGC 5288 follows a circular path around the Galactic center.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"13 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054392","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.10
G. Cordero-Tercero, D. Maravilla, M. Covarrubias-Saavedra
In this document we briefly review the evolution of the term meteoroid and we make several proposals for a definition, emphasizing the importance of the criteria used for it. Finally, we propose a definition based on observations rather than on the instrument of observation.
{"title":"A NEW PROPOSAL OF THE TERM METEOROID","authors":"G. Cordero-Tercero, D. Maravilla, M. Covarrubias-Saavedra","doi":"10.22201/ia.01851101p.2023.59.02.10","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.10","url":null,"abstract":"In this document we briefly review the evolution of the term meteoroid and we make several proposals for a definition, emphasizing the importance of the criteria used for it. Finally, we propose a definition based on observations rather than on the instrument of observation.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"67 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054399","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.11
E. Quiroga
Messier 104, NGC 4594, also known as the Sombrero Galaxy, has been extensively studied, especially its structure and stellar halo. Its abundance of globular clusters has given rise to many theories and much speculation. However, other objects in the vicinity of such a spectacular galaxy are sometimes ignored. While studying HST images available on the HST Legacy website of the halo of M104 (HST proposal 9714, PI: Keith Noll), the author observed at 12:40:07.829 -11:36:47.38 (in j2000) an object about 4 arc seconds in diameter. A study with VO tools suggests that the object is a SBc galaxy with an AGN (Seyfert).
梅西耶104,NGC 4594，也被称为草帽星系，已经被广泛研究，特别是它的结构和恒星晕。它丰富的球状星团已经产生了许多理论和猜测。然而，在这样一个壮观的星系附近的其他物体有时会被忽略。在研究HST遗产网站上提供的M104光环(HST提案9714,PI: Keith Noll)的HST图像时，作者在2000年的12:40:07.829 -11:36:47.38观测到一个直径约为4角秒的物体。用VO工具进行的一项研究表明，该物体是一个具有AGN (Seyfert)的SBc星系。
{"title":"A PECULIAR GALAXY NEAR M104","authors":"E. Quiroga","doi":"10.22201/ia.01851101p.2023.59.02.11","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.11","url":null,"abstract":"Messier 104, NGC 4594, also known as the Sombrero Galaxy, has been extensively studied, especially its structure and stellar halo. Its abundance of globular clusters has given rise to many theories and much speculation. However, other objects in the vicinity of such a spectacular galaxy are sometimes ignored. While studying HST images available on the HST Legacy website of the halo of M104 (HST proposal 9714, PI: Keith Noll), the author observed at 12:40:07.829 -11:36:47.38 (in j2000) an object about 4 arc seconds in diameter. A study with VO tools suggests that the object is a SBc galaxy with an AGN (Seyfert).","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"136 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054398","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.13
C. A. Caretta, H. Andernach, M. Chow-Martínez, R. Coziol, J. De Anda-Suárez, C. Hernández-Aguayo, J. M. Islas-Islas, M. M. Mireles-Vidales, M. A. Muñiz-Torres, H. Santoyo-Ruiz, J. J. Trejo-Alonso, Y. Venkatapathy, J. M. Zúñiga
We have compiled a sample of 67 nearby (z < 0.15) clusters of galaxies, for which on average more than 150 spectroscopic members are available and, by applying different methods to detect substructures in their galaxy distribution, we have studied their assembly history. Our analysis confirms that substructures are present in 70% of our sample, having a significant dynamical impact in 57% of them. A classification of the assembly state of the clusters based on the dynamical significance of their substructures is proposed. In 19% of our clusters, the originally identified brightest cluster galaxy is not the central gravitationally dominant galaxy (CDG), but turns out to be either the second-rank, or the dominant galaxy of a substructure (a SDG, in our classification), or even a possible “fossil” galaxy in the periphery of the cluster. Moreover, no correlation was found in general between the projected offset of the CDG from the X-ray peak and its peculiar velocity.
{"title":"TRACING THE ASSEMBLY HISTORIES OF GALAXY CLUSTERS IN THE NEARBY UNIVERSE","authors":"C. A. Caretta, H. Andernach, M. Chow-Martínez, R. Coziol, J. De Anda-Suárez, C. Hernández-Aguayo, J. M. Islas-Islas, M. M. Mireles-Vidales, M. A. Muñiz-Torres, H. Santoyo-Ruiz, J. J. Trejo-Alonso, Y. Venkatapathy, J. M. Zúñiga","doi":"10.22201/ia.01851101p.2023.59.02.13","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.13","url":null,"abstract":"We have compiled a sample of 67 nearby (z < 0.15) clusters of galaxies, for which on average more than 150 spectroscopic members are available and, by applying different methods to detect substructures in their galaxy distribution, we have studied their assembly history. Our analysis confirms that substructures are present in 70% of our sample, having a significant dynamical impact in 57% of them. A classification of the assembly state of the clusters based on the dynamical significance of their substructures is proposed. In 19% of our clusters, the originally identified brightest cluster galaxy is not the central gravitationally dominant galaxy (CDG), but turns out to be either the second-rank, or the dominant galaxy of a substructure (a SDG, in our classification), or even a possible “fossil” galaxy in the periphery of the cluster. Moreover, no correlation was found in general between the projected offset of the CDG from the X-ray peak and its peculiar velocity.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136055236","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.04
J. Echevarría, S. H. Ramírez, M. Fuentes, L. J. Sánchez, V. Patiño, V. Chavushyan
We present new optical spectroscopic observations of U Geminorum obtained during a quiescent stage. We perform a radial velocity analysis of three Balmer emission lines yielding inconsistent results. Assuming that the radial velocity semi amplitude accurately reflects the motion of the white dwarf, we arrive at masses for the primary which are in the range of Mwd = 1.21−1.37M☉. Based on the internal radial velocity inconsistencies and results produced from the Doppler tomography - wherein we do not detect emission from the hot spot, but rather an intense asymmetric emission overlaying the disc, reminiscent of spiral arms - we discuss the possibility that the overestimation of the masses may be due to variations of gas opacities and a partial truncation of the disc.
{"title":"NEW SPECTROSCOPY OF U GEM","authors":"J. Echevarría, S. H. Ramírez, M. Fuentes, L. J. Sánchez, V. Patiño, V. Chavushyan","doi":"10.22201/ia.01851101p.2023.59.02.04","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.04","url":null,"abstract":"We present new optical spectroscopic observations of U Geminorum obtained during a quiescent stage. We perform a radial velocity analysis of three Balmer emission lines yielding inconsistent results. Assuming that the radial velocity semi amplitude accurately reflects the motion of the white dwarf, we arrive at masses for the primary which are in the range of Mwd = 1.21−1.37M☉. Based on the internal radial velocity inconsistencies and results produced from the Doppler tomography - wherein we do not detect emission from the hot spot, but rather an intense asymmetric emission overlaying the disc, reminiscent of spiral arms - we discuss the possibility that the overestimation of the masses may be due to variations of gas opacities and a partial truncation of the disc.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"50 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054385","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.07
Rodolfo de J. Zermeño, Ana M. Hidalgo-Gámez
The rotation curve of a galaxy contains a wealth of information about its dynamical properties, being the mass distribution one of the most important. The rotation curve fitting procedures used to estimate the mass profiles of disc galaxies have become more sophisticated over the years, providing ever more reliable results. However, the time-cost and data requirements (e.g. high-resolution NIR photometry) necessary to put to use some of them have restricted these kind of studies to small samples of galaxies. We propose a simple procedure that could be used as a good first approximation for the study of large galaxy samples. It is based on a parameter-fitting method along with a recent optimization algorithm, called the Asexual Genetic Algorithm (AGA). With this procedure, we were able to replicate previously published results, within uncertainties, suggesting that it will provide a reliable first estimation, suitable for its application to large galaxy samples.
{"title":"MASS PROFILES OF LATE GALAXIES USING A GENETIC ALGORITHM. I - TESTING THE ALGORITHM","authors":"Rodolfo de J. Zermeño, Ana M. Hidalgo-Gámez","doi":"10.22201/ia.01851101p.2023.59.02.07","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.07","url":null,"abstract":"The rotation curve of a galaxy contains a wealth of information about its dynamical properties, being the mass distribution one of the most important. The rotation curve fitting procedures used to estimate the mass profiles of disc galaxies have become more sophisticated over the years, providing ever more reliable results. However, the time-cost and data requirements (e.g. high-resolution NIR photometry) necessary to put to use some of them have restricted these kind of studies to small samples of galaxies. We propose a simple procedure that could be used as a good first approximation for the study of large galaxy samples. It is based on a parameter-fitting method along with a recent optimization algorithm, called the Asexual Genetic Algorithm (AGA). With this procedure, we were able to replicate previously published results, within uncertainties, suggesting that it will provide a reliable first estimation, suitable for its application to large galaxy samples.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"41 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054526","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.01
W. A. Badawy, A. L. Tadross, Y. H. M. Hendy, M. N. Ismail, A. Mouner
Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kronberger 13, Kronberger 18, Majaess 99, NGC 7795, Ruprecht 139, Teutsch 55, S1, and FSR 0596, which are close to the Galactic plane of the Milky Way. The number of probable cluster members is found to be 81, 77, 120, 155, 108, 110, 160, and 116 respectively. Radii are determined as 5.40, 5.25, 4.80, 4.20, 4.28, 3.70, 4.30, 4.30, and 3.53 arcmin, respectively. With solar metallicity isochrones log ages of 7.70, 9.00, 8.35, 7.50, 9.00, 8.00, 7.50, 8.50, and 9.5 yr are determined for these clusters. The best fitting of the isochrone produced distances of 2.6, 1.27, 1.16, 1.16, 3.10, 1.64, 2.50, 2.44, and 0.98 kpc that are similar to the distances calculated from inverting median parallaxes. The mass function slopes are in agreement with the Salpeter value. The results of the total masses are found to be 116.07, 79.33, 141.24, 147.34, 145.76, 491.01, 155, 212.46, and 82.79 M☉.
{"title":"ASTROPHYSICAL STUDIES OF 9 UNSTUDIED OPEN STAR CLUSTERS USING GAIA DR3","authors":"W. A. Badawy, A. L. Tadross, Y. H. M. Hendy, M. N. Ismail, A. Mouner","doi":"10.22201/ia.01851101p.2023.59.02.01","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.01","url":null,"abstract":"Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kronberger 13, Kronberger 18, Majaess 99, NGC 7795, Ruprecht 139, Teutsch 55, S1, and FSR 0596, which are close to the Galactic plane of the Milky Way. The number of probable cluster members is found to be 81, 77, 120, 155, 108, 110, 160, and 116 respectively. Radii are determined as 5.40, 5.25, 4.80, 4.20, 4.28, 3.70, 4.30, 4.30, and 3.53 arcmin, respectively. With solar metallicity isochrones log ages of 7.70, 9.00, 8.35, 7.50, 9.00, 8.00, 7.50, 8.50, and 9.5 yr are determined for these clusters. The best fitting of the isochrone produced distances of 2.6, 1.27, 1.16, 1.16, 3.10, 1.64, 2.50, 2.44, and 0.98 kpc that are similar to the distances calculated from inverting median parallaxes. The mass function slopes are in agreement with the Salpeter value. The results of the total masses are found to be 116.07, 79.33, 141.24, 147.34, 145.76, 491.01, 155, 212.46, and 82.79 M☉.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"13 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136055244","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.05
R. H. Nelson, K. B. Alton, M. Kendurkar
New radial velocity (RV) data obtained at the Dominion Astrophysical Observatory (DAO) in Victoria, British Columbia along with light curve (LC) data for the Algol-type binary V1241 Tau have been simultaneously analysed with the 2003 version of the Wilson-Devinney code (WD2003). There were two distinct LC datasets: one was from the Transiting Exoplanet Survey Satellite (TESS) and the others (BVIc) from the (land-based) Desert Blooms Observatory (DBO). The TESS data were considered to have the least photometric uncertainty; consequently, we derived estimates for M1 (1.91(8) M☉), M2 (1.04(4) M☉), R1 (1.86(1) R☉), R2 (1.73(1) R☉), qWD (0.54(3)), L1 (10.7(8) L☉), and L2 (1.7(2) L☉) following simultaneous analysis (RV+LC) with the WD2003 code. Evolutionary modeling revealed that the primary star is somewhat evolved past the zero age main sequence (ZAMS) while the secondary is much evolved past the terminal age main sequence (TAMS).
{"title":"SPECTROSCOPIC & PHOTOMETRIC STUDY OF THE ALGOL-TYPE BINARY V1241 TAURI","authors":"R. H. Nelson, K. B. Alton, M. Kendurkar","doi":"10.22201/ia.01851101p.2023.59.02.05","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.05","url":null,"abstract":"New radial velocity (RV) data obtained at the Dominion Astrophysical Observatory (DAO) in Victoria, British Columbia along with light curve (LC) data for the Algol-type binary V1241 Tau have been simultaneously analysed with the 2003 version of the Wilson-Devinney code (WD2003). There were two distinct LC datasets: one was from the Transiting Exoplanet Survey Satellite (TESS) and the others (BVIc) from the (land-based) Desert Blooms Observatory (DBO). The TESS data were considered to have the least photometric uncertainty; consequently, we derived estimates for M1 (1.91(8) M☉), M2 (1.04(4) M☉), R1 (1.86(1) R☉), R2 (1.73(1) R☉), qWD (0.54(3)), L1 (10.7(8) L☉), and L2 (1.7(2) L☉) following simultaneous analysis (RV&plus;LC) with the WD2003 code. Evolutionary modeling revealed that the primary star is somewhat evolved past the zero age main sequence (ZAMS) while the secondary is much evolved past the terminal age main sequence (TAMS).","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054393","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 : 2023-10-01DOI: 10.22201/ia.01851101p.2023.59.02.02
D. D. Carpintero, J. C. Muzzio
The Lyapunov characteristic exponents are a useful indicator of chaos in astronomical dynamical systems. They are usually computed through a standard, very effcient and neat algorithm published in 1980. However, for Hamiltonian systems the expected result of pairs of opposite exponents is not always obtained with enough precision. We find here why in these cases the initial order of the deviation vectors matters, and how to sort them in order to obtain a correct result.
{"title":"ON THE CORRECT COMPUTATION OF ALL LYAPUNOV EXPONENTS IN HAMILTONIAN DYNAMICAL SYSTEMS","authors":"D. D. Carpintero, J. C. Muzzio","doi":"10.22201/ia.01851101p.2023.59.02.02","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.02.02","url":null,"abstract":"The Lyapunov characteristic exponents are a useful indicator of chaos in astronomical dynamical systems. They are usually computed through a standard, very effcient and neat algorithm published in 1980. However, for Hamiltonian systems the expected result of pairs of opposite exponents is not always obtained with enough precision. We find here why in these cases the initial order of the deviation vectors matters, and how to sort them in order to obtain a correct result.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"68 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136054528","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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