Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.10
A. Raga, J. Cantó
Relativistic, corkscrew jets are produced by some Galactic compact objects (notably, the SS433 outflow) and by some of the central monsters of quasars or AGN. As the result of arrival time-delay effects, the projections of the outflow locus onto the observed plane of the sky are remarkably different for the (blueshifted) jet and the (redshifted) counterjet. In terms of a ballistic, precessing jet model, we show that for a range of outflow parameters these relativistic effects correspond to apparent changes in: the orientation angle of the precession axis, the opening angle of the precession cone and the flow velocity. This description is appropriate for outflows with v/c ≤ 0 . 5. azul). En t´erminos de un modelo de jet precesante bal´ıstico, mostramos que para un intervalo de par´ametros del flujo estos efectos relativistas corresponden a cambios aparentes en: la orientacion del eje de precesi´on, el ´angulo de apertura del cono de precesi´on y la velocidad del flujo. Esta descripci´on es apropiada para flujos con v/c ≤ 0 . 5.
相对论的螺旋状喷流是由一些银河系致密天体（尤其是SS433外流）和一些类星体或AGN的中心怪物产生的。由于到达时间延迟的影响，（蓝移）喷流和（红移）反喷流在观测到的天空平面上的流出轨迹投影明显不同。就弹道进动射流模型而言，我们表明，对于一系列流动参数，这些相对论效应对应于进动轴的方位角、进动锥的开口角和流动速度的明显变化。此描述适用于v/c≤0的流量。5.天青）。在喷气推进模型的范围内，大多数情况下，飞行参数的相互影响与飞行速度的变化相对应。Esta descripti´on es appropiada para fluujos con v/c≤0。5.
{"title":"MILDLY RELATIVISTIC, BALLISTIC CORKSCREW JETS AS ROTATED SPIRALS","authors":"A. Raga, J. Cantó","doi":"10.22201/ia.01851101p.2022.58.02.10","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.10","url":null,"abstract":"Relativistic, corkscrew jets are produced by some Galactic compact objects (notably, the SS433 outflow) and by some of the central monsters of quasars or AGN. As the result of arrival time-delay effects, the projections of the outflow locus onto the observed plane of the sky are remarkably different for the (blueshifted) jet and the (redshifted) counterjet. In terms of a ballistic, precessing jet model, we show that for a range of outflow parameters these relativistic effects correspond to apparent changes in: the orientation angle of the precession axis, the opening angle of the precession cone and the flow velocity. This description is appropriate for outflows with v/c ≤ 0 . 5. azul). En t´erminos de un modelo de jet precesante bal´ıstico, mostramos que para un intervalo de par´ametros del flujo estos efectos relativistas corresponden a cambios aparentes en: la orientacion del eje de precesi´on, el ´angulo de apertura del cono de precesi´on y la velocidad del flujo. Esta descripci´on es apropiada para flujos con v/c ≤ 0 . 5.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47760878","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 : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.13
M. Nouh, Y. A. Azzam, E. Abdel-salam, F. Elnagahy, T. M. Kamel
Relativistic isothermal gas spheres are a powerful tool to model many astronomical objects, like compact stars and clusters of galaxies. In the present paper, we introduce an artificial neural network (ANN) algorithm and Taylor series to model the relativistic gas spheres using Tolman-Oppenheimer-Volkoff differential equations (TOV). Comparing the analytical solutions with the numerical ones revealed good agreement with maximum relative errors of 10−3. The ANN algorithm implements a three-layer feed-forward neural network built using a back-propagation learning technique that is based on the gradient descent rule. We analyzed the massradius relations and the density profiles of the relativistic isothermal gas spheres against different relativistic parameters and compared the ANN solutions with the analytical ones. The comparison between the two solutions reflects the efficiency of using the ANN to solve TOV equations.
{"title":"ANN AND ANALYTICAL SOLUTIONS TO RELATIVISTIC ISOTHERMAL GAS SPHERES","authors":"M. Nouh, Y. A. Azzam, E. Abdel-salam, F. Elnagahy, T. M. Kamel","doi":"10.22201/ia.01851101p.2022.58.02.13","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.13","url":null,"abstract":"Relativistic isothermal gas spheres are a powerful tool to model many astronomical objects, like compact stars and clusters of galaxies. In the present paper, we introduce an artificial neural network (ANN) algorithm and Taylor series to model the relativistic gas spheres using Tolman-Oppenheimer-Volkoff differential equations (TOV). Comparing the analytical solutions with the numerical ones revealed good agreement with maximum relative errors of 10−3. The ANN algorithm implements a three-layer feed-forward neural network built using a back-propagation learning technique that is based on the gradient descent rule. We analyzed the massradius relations and the density profiles of the relativistic isothermal gas spheres against different relativistic parameters and compared the ANN solutions with the analytical ones. The comparison between the two solutions reflects the efficiency of using the ANN to solve TOV equations.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49596065","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 : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.08
A. Arellano
We report the mean metallicity and absolute magnitude of RR Lyrae stars in a sample of 37 globular clusters, calculated via the Fourier decomposition of their light curves and ad hoc semi-empirical calibrations, in an unprecedented homogeneous approach. This enabled a new discussion of the metallicity dependence of the horizontal branch (HB) luminosity, as a fundamental distance indicator. The calibration for the RRab and RRc stars should be treated separately. For the RRab the dispersion is larger and non-linear. For the RRc stars the correlation is less steep, very tight and linear. The relevance of the HB structural parameter L, is highlighted and we offer a non-linear calibration of the form MV ([Fe/H], L). Excellent agreement is found between values of [Fe/H] and MV from the light curve decomposition with spectroscopic values and distances obtained via Gaia-DR3 and HST. The variables census in 35 clusters includes 326 stars found by our program.
{"title":"A VINDICATION OF THE RR LYRAE FOURIER LIGHT CURVE DECOMPOSITION FOR THE CALCULATION OF METALLICITY AND DISTANCE IN GLOBULAR CLUSTERS","authors":"A. Arellano","doi":"10.22201/ia.01851101p.2022.58.02.08","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.08","url":null,"abstract":"We report the mean metallicity and absolute magnitude of RR Lyrae stars in a sample of 37 globular clusters, calculated via the Fourier decomposition of their light curves and ad hoc semi-empirical calibrations, in an unprecedented homogeneous approach. This enabled a new discussion of the metallicity dependence of the horizontal branch (HB) luminosity, as a fundamental distance indicator. The calibration for the RRab and RRc stars should be treated separately. For the RRab the dispersion is larger and non-linear. For the RRc stars the correlation is less steep, very tight and linear. The relevance of the HB structural parameter L, is highlighted and we offer a non-linear calibration of the form MV ([Fe/H], L). Excellent agreement is found between values of [Fe/H] and MV from the light curve decomposition with spectroscopic values and distances obtained via Gaia-DR3 and HST. The variables census in 35 clusters includes 326 stars found by our program.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"1 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68129180","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 : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.19
G. Koenigsberger, N. Morrell, D. Hillier, W. Schmutz, R. Gamen, J. Arias, R. Barbá, G. Ferrero
Analysis of spectral line profile variations observed over 6 decades in the Wolf-Rayet system HD 5980 lead to the conclusion that Star A, the variable member of the system, has always dominated the wind collision zone (WCZ), contrary to suggestions that before 1994 the stronger wind belonged to its close companion, Star B. The observed variations are caused by a combination of physical occultations, wind eclipses and emission and absorption originating in the WCZ. The effects caused by the leading WCZ branch, which folds around Star B, are clearly seen as it crosses our line of sight to Star A during the secondary eclipse. These effects can inform on the WCZ velocity and density structures. We speculate that differences in line profiles at the same orbital phase but at different epochs may be linked to changes in the WCZ radiative properties. The 2017-2020 spectra indicate that HD 5980 was in a higher activity state than during 2010-2015.
{"title":"OBSERVATIONAL CONSTRAINTS ON THE HD 5980 WIND-WIND COLLISION","authors":"G. Koenigsberger, N. Morrell, D. Hillier, W. Schmutz, R. Gamen, J. Arias, R. Barbá, G. Ferrero","doi":"10.22201/ia.01851101p.2022.58.02.19","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.19","url":null,"abstract":"Analysis of spectral line profile variations observed over 6 decades in the Wolf-Rayet system HD 5980 lead to the conclusion that Star A, the variable member of the system, has always dominated the wind collision zone (WCZ), contrary to suggestions that before 1994 the stronger wind belonged to its close companion, Star B. The observed variations are caused by a combination of physical occultations, wind eclipses and emission and absorption originating in the WCZ. The effects caused by the leading WCZ branch, which folds around Star B, are clearly seen as it crosses our line of sight to Star A during the secondary eclipse. These effects can inform on the WCZ velocity and density structures. We speculate that differences in line profiles at the same orbital phase but at different epochs may be linked to changes in the WCZ radiative properties. The 2017-2020 spectra indicate that HD 5980 was in a higher activity state than during 2010-2015.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47628020","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 : 2022-08-16DOI: 10.22201/ia.01851101p.2023.59.01.01
A. Ferro, I. B. Fierro, S. Muneer, S. Giridhar
A CCD VI imaging time-series over 11-year is employed to explore the light curves of stars in the field of Palomar 2. We discovered 20 RRab and 1 RRc variables. A revision of Gaia-DR3 data enabled us to identify 10 more variables and confirm the RRab nature of 6 of them and one RGB. The cluster membership is discussed, and 18 variables are most likely cluster members. The Fourier light curve decomposition for the 11 best quality light curves of cluster member stars leads to independent estimates of the cluster distance 27.2 ± 1.8 kpc and [Fe/H]ZW = -1.39 ± 0.55. We confirm the cluster as of the Oo I type.
{"title":"RR LYRAE STARS IN THE GLOBULAR CLUSTER PALOMAR 2","authors":"A. Ferro, I. B. Fierro, S. Muneer, S. Giridhar","doi":"10.22201/ia.01851101p.2023.59.01.01","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.01.01","url":null,"abstract":"A CCD VI imaging time-series over 11-year is employed to explore the light curves of stars in the field of Palomar 2. We discovered 20 RRab and 1 RRc variables. A revision of Gaia-DR3 data enabled us to identify 10 more variables and confirm the RRab nature of 6 of them and one RGB. The cluster membership is discussed, and 18 variables are most likely cluster members. The Fourier light curve decomposition for the 11 best quality light curves of cluster member stars leads to independent estimates of the cluster distance 27.2 ± 1.8 kpc and [Fe/H]ZW = -1.39 ± 0.55. We confirm the cluster as of the Oo I type.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46631493","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 : 2022-08-06DOI: 10.22201/ia.01851101p.2022.58.02.16
F. S'anchez, E. Battaner
The existence of life is one of the most fundamental problems of astrophysics. The intriguing existence of progressively complex and apparently improbable living beings should be a general tendency of life in the Universe. We are looking for general physical laws governing the growth of complexity in any astrophysical environment. We posit the existence of a vital scalar field. This scalar is sensitive to the gradient of the inverse of specific entropy, such that its distribution tends to very high values in the interior of living beings. Besides the classical mutations, vital field driven mutations only produce decrements of entropy. The field equations give rise to the existence of vital waves. This theory is able to deal with both the origin of life and the evolution of life. We show that the growth of complexity is accelerated by the vital field.
{"title":"AN ASTROPHYSICAL PERSPECTIVE OF LIFE. THE GROWTH OF COMPLEXITY","authors":"F. S'anchez, E. Battaner","doi":"10.22201/ia.01851101p.2022.58.02.16","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.16","url":null,"abstract":"The existence of life is one of the most fundamental problems of astrophysics. The intriguing existence of progressively complex and apparently improbable living beings should be a general tendency of life in the Universe. We are looking for general physical laws governing the growth of complexity in any astrophysical environment. We posit the existence of a vital scalar field. This scalar is sensitive to the gradient of the inverse of specific entropy, such that its distribution tends to very high values in the interior of living beings. Besides the classical mutations, vital field driven mutations only produce decrements of entropy. The field equations give rise to the existence of vital waves. This theory is able to deal with both the origin of life and the evolution of life. We show that the growth of complexity is accelerated by the vital field.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48644228","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 : 2022-08-05DOI: 10.22201/ia.01851101p.2022.58.02.17
A. Tadross, Eslam G. Elhosseiny
A photometric and astrometric study of the two open star clusters Gulliver18 and Gulliver58 was carried out for the first time using the early third data release of the Gaia space observatory (Gaia-EDR3). By studying the proper motions, parallaxes, and color-magnitude diagrams of the two clusters, we determined their actual cluster membership. Therefore, ages, color excesses, and heliocentric distances of the clusters could be determined. The luminosity function, mass function, total mass, mass segregation, and relaxation time of Gulliver18 and Gulliver58 were estimated as well.
{"title":"THE PRINCIPAL ASTROPHYSICAL PARAMETERS OF THE OPEN CLUSTERS GULLIVER 18 AND GULLIVER 58 DETERMINED USING GAIA EDR3 DATA","authors":"A. Tadross, Eslam G. Elhosseiny","doi":"10.22201/ia.01851101p.2022.58.02.17","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.17","url":null,"abstract":"A photometric and astrometric study of the two open star clusters Gulliver18 and Gulliver58 was carried out for the first time using the early third data release of the Gaia space observatory (Gaia-EDR3). By studying the proper motions, parallaxes, and color-magnitude diagrams of the two clusters, we determined their actual cluster membership. Therefore, ages, color excesses, and heliocentric distances of the clusters could be determined. The luminosity function, mass function, total mass, mass segregation, and relaxation time of Gulliver18 and Gulliver58 were estimated as well.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46574411","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 : 2022-08-01DOI: 10.22201/ia.14052059p.2022.54.04
M. Shamshad, M. Chaniotakis, V. Boschi
As the world witnessed a swift change in every walk of life during the SARS-Cov2 pandemic, flexibility and adaption remained the key components for staying relevant in the field of science education. However, beyond the need for quick adaptation and acquisition of digital skills by both teachers and students, the digital transformation in education has opened up a window of opportunity making global and remote engagement possible for everyone. This paper presents the good practice of Virtual Visits to Virgo Gravitational Wave Detector coorganized by EGO-Virgo, the FRONTIERS and REINFORCE EU funded projects and the “School of Astronomy and Physics by Mirwat” with the participation of high school girls from Islamabad and remote regions of Pakistan. This paper presents the prospect of international collaboration for STEM education, early exposure to research environment to build the deeper understanding of the functioning and working of large research infrastructure, building science identity by informal science experiences and to empower the high school students by engagement in content creation activity. The experience indicates a positive outcome and improvement in understanding of students as well as a step towards building a science identity among them.
在SARS-Cov2大流行期间，世界各行各业都发生了迅速变化，灵活性和适应性仍然是在科学教育领域保持相关性的关键因素。然而，除了教师和学生需要快速适应和掌握数字技能之外，教育领域的数字化转型还打开了一扇机会之窗，使每个人都可以进行全球和远程参与。本文介绍了由EGO-Virgo、欧盟资助的FRONTIERS and REINFORCE项目和“Mirwat天文与物理学院”共同组织的处女座引力波探测器虚拟参观项目的良好实践，该项目有来自伊斯兰堡和巴基斯坦偏远地区的高中女生参与。本文介绍了STEM教育的国际合作前景，早期接触研究环境，以建立对大型研究基础设施的功能和工作的更深入理解，通过非正式的科学经验建立科学身份，并通过参与内容创造活动赋予高中生权力。这一经验表明了一个积极的结果和对学生的理解的改善，以及朝着在学生中建立科学身份迈出的一步。
{"title":"INTERNATIONAL COLLABORATION FOR SCIENCE EDUCATION IN UNDERPRIVILEGED AREAS: THE CASE STUDY OF THE ALL-GIRLS “SCHOOL OF ASTRONOMY AND PHYSICS BY MIRWAT” IN PAKISTAN AND VIRTUAL VISITS TO THE VIRGO INTERFEROMETER","authors":"M. Shamshad, M. Chaniotakis, V. Boschi","doi":"10.22201/ia.14052059p.2022.54.04","DOIUrl":"https://doi.org/10.22201/ia.14052059p.2022.54.04","url":null,"abstract":"As the world witnessed a swift change in every walk of life during the SARS-Cov2 pandemic, flexibility and adaption remained the key components for staying relevant in the field of science education. However, beyond the need for quick adaptation and acquisition of digital skills by both teachers and students, the digital transformation in education has opened up a window of opportunity making global and remote engagement possible for everyone. This paper presents the good practice of Virtual Visits to Virgo Gravitational Wave Detector coorganized by EGO-Virgo, the FRONTIERS and REINFORCE EU funded projects and the “School of Astronomy and Physics by Mirwat” with the participation of high school girls from Islamabad and remote regions of Pakistan. This paper presents the prospect of international collaboration for STEM education, early exposure to research environment to build the deeper understanding of the functioning and working of large research infrastructure, building science identity by informal science experiences and to empower the high school students by engagement in content creation activity. The experience indicates a positive outcome and improvement in understanding of students as well as a step towards building a science identity among them.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"52 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84500542","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 : 2022-08-01DOI: 10.22201/ia.14052059p.2022.54.28
J. Casado, G. de la Vega, L. M. E. Dominguez, B. García
Nowadays visualization is the main method to display and analyze scientific information in astronomy, only one sense analyzing a big amount of datasets, even after 20 years of formal meeting to discuss the use and capabilities of sonification. Beyond the reluctance to use sonification, there is a growing need for new forms of data display either for research or for outreach. In this sense, and centred mainly on research, SonoUno start been developed. In this opportunity, the sonoUno web interface is presented, the aim of this contribution is to produce a tool for users who don't need large datasets, or are simply interested in testing the concepts of the SonoUno project, without going through all the trouble of installing a full featured SonoUno system. The results are promising, real data sets were opened, sonified and some mathematical functions applied.
{"title":"SONOUNO WEB INTERFACE FOR SONIFICATION AND ANALYSIS OF ASTROPHYSICAL DATA","authors":"J. Casado, G. de la Vega, L. M. E. Dominguez, B. García","doi":"10.22201/ia.14052059p.2022.54.28","DOIUrl":"https://doi.org/10.22201/ia.14052059p.2022.54.28","url":null,"abstract":"Nowadays visualization is the main method to display and analyze scientific information in astronomy, only one sense analyzing a big amount of datasets, even after 20 years of formal meeting to discuss the use and capabilities of sonification. Beyond the reluctance to use sonification, there is a growing need for new forms of data display either for research or for outreach. In this sense, and centred mainly on research, SonoUno start been developed. In this opportunity, the sonoUno web interface is presented, the aim of this contribution is to produce a tool for users who don't need large datasets, or are simply interested in testing the concepts of the SonoUno project, without going through all the trouble of installing a full featured SonoUno system. The results are promising, real data sets were opened, sonified and some mathematical functions applied.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"32 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82400778","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 : 2022-08-01DOI: 10.22201/ia.14052059p.2022.54.12
K. Usuda-Sato, Y. Suzuki, S. Kawashima, Y. Goko, T. Inoue
We created a whole set of the "Touch the Universe" tactile exhibition, including 3D models of celestial bodies and telescopes that both blind and visually impaired (BVI) people and sighted people can understand and enjoy. Through the JAPAN Science Museum Association network, science museums in Japan can easily borrow it and hold their own tacile exhibition without using a 3D printer. The exhibition set consists of existing 3D models, additional tactile images, scale models of the Solar System. Each model has a concise description panel with both printed and braille letters. This easy-to-use set can be a breakthrough for science museum staff members to hold their own tactile exhibition and communicate with BVI people.
{"title":"DISSEMINATION OF THE “TOUCH THE UNIVERSE” TACTILE EXHIBITION","authors":"K. Usuda-Sato, Y. Suzuki, S. Kawashima, Y. Goko, T. Inoue","doi":"10.22201/ia.14052059p.2022.54.12","DOIUrl":"https://doi.org/10.22201/ia.14052059p.2022.54.12","url":null,"abstract":"We created a whole set of the \"Touch the Universe\" tactile exhibition, including 3D models of celestial bodies and telescopes that both blind and visually impaired (BVI) people and sighted people can understand and enjoy. Through the JAPAN Science Museum Association network, science museums in Japan can easily borrow it and hold their own tacile exhibition without using a 3D printer. The exhibition set consists of existing 3D models, additional tactile images, scale models of the Solar System. Each model has a concise description panel with both printed and braille letters. This easy-to-use set can be a breakthrough for science museum staff members to hold their own tactile exhibition and communicate with BVI people.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"72 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91253845","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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