https://hemerotecadigital.uanl.mx/files/original/408/19941/Celerinet_2018_Ano_6_No_2_Julio-Diciembre.ocr.pdf 686b41575398a14e95c0e849d1722c35 PDF Text Text O) ~ ' IO O) CX) C') C\J z (/) (/) 'l. / 1 ~ ~ .. .. ~ . r~ ~~ -- ~......, .,, ~~=~- ~~ >-~ ~ ~e -----= - ~ -5 ._ • ~~ ,~ ~ / l . ~· ~ ~ 'r' • ~ MATHEMATICS, PHYSICS, COMPUTER SCIENCE, ASTROPHYSICS 9 uANL l 1'\ IVl".ltSlllAI> i\lJ íÓNOMA nt·: Nttt-:\101 i-t1N FCFM f,-\f'l lLTAD DF C1f.NC7AS FiSICO MATfMAOCAS 5 ~ �lng. Rogelio Guillermo Garza Rivera Rector Dr. Santos Guzmán López Secretario General M.A. Emilia Edith Vásquez Farías Academic Secretary Dr. Celso José Garza Acuña Secretary of Cultural Affairs Lic. Antonio Ramos Revillas Publications Director Dr. Rogelio Juvenal Sepúlveda Guerrero Director of the Facultad de Ciencias Físico Matemáticas Dr. Romeo de Jesús Selvas Aguilar Editor in Chief M.A. Alma Patricia Calderón Martínez Lic. Nicelia María Buttén Salazar Editors Ángel Salvador Pérez Blanco Juan Pablo Salinas Estevane Angel Sanchez Colin Pedro Valdés-Sada Enrique J. Pérez Carlos E. Chávez Eduardo Pérez-Tijerina Collaborators M.A. Patricia Martínez Moreno M.T. José Apolinar Loyola Rodríguez Dr. Romeo de Jesús Selvas Aguilar M.C. Azucena Yoloxóchitl Ríos Mercado M.A. Alma Patricia Calderón Martínez Dr. Álvaro Reyes Martínez Dra. María de Jesús Antonia Ochoa Oliva Editorial Committee Dahlia Nayelli Espinoza Segovia Víctor Manuel Barrera Herrera Editorial Design Celerinet, Year 6, No. 1, July-December. Published on : December 19th, 2018 Gelerinet is a semestral publication edited by the Universidad Autónoma de Nuevo León, through the Facultad de Ciencias Físico Matemáticas. Address: Ave. Universidad S/N. Gd. Universitaria. San Nicolás de los Garza, Nuevo León, México, G.P. 66451. Telephone + 52 81 83294030. Fax: + 52 81 83522954. celerinet.uanl.mx Editor in Ghief: Dr. Romeo de Jesús Selvas Aguilar. Exclusive Rights Number 04-2014-102111595700-203 licenced by the Instituto Nacional de Derechos de Autor. ISSN 2395-8359. Responsible for last update: Unidad Informática, M.A. Reyna Guadalupe Castro Medellín, Ave. Universidad S/N. Gd. Universitaria. San Nicolás de los Garza, Nuevo León, México, G.P. 66451. Last update: December 19th, 2018. The views expressed in th is publication do not necessarily reflect the Editors' views. The partial or total reproduction of the contents and images in th is number is forbidden. AII rights reserved © Copyright 2018 celerinet @uanl.mx �1 SIZE VARIATION OF FE10 3 EMBEDDED IN A KAOLINITIC CLAY OF RECENT GEOLOGICALAGE 6 EMERGING PLANETARY ASTROPHYSICS AND RELATED TECHNOLOGIES RESEARCH IN NORTHEASTERN MEXICO �RESEARCH PAPERS , ARTICULOS DE, INVESTIGACION �RESEARCH/ PHYSICS Angel Salvador Pérez Blanco & Juan Pablo Salinas Estevane; UANLFCFM ABSTRACT Kaolinite is an alumina-silicate with a triclinic or monoclinic structure that originates from the evolution of minerals such as as feldspar or granite in accordance to its geologic origin. On this research, 10 kg of kaolinitic clay were extracted from three different places ata mineral pit in S. L. P., Mexico. X-Ray diffraction analysis (XRD) was performed on the different kaolin samples, afterwards they were anal yzed by optical m icroscopy on the image analyzer mode in order to observe the Fe::O3 size variation on the three different kaolinitc samples. lt could be verified that there is a considerable variation in the Fe::O3 size for samples coming form the same substrate, in addition to that, when the size of Fe2Q3 was compared o neto another, a significant difference in hematite size was observed. The large variation in the hematite size on each sample suggests a recent geological age. Keywords: Kaolinite; Microscopy; X-ray diffraction. RESUMEN La caolinita es un silicato de alúmina con una estructura triclínica o monoclínica que se origina a partir de la evolución de minerales como el feldespato o el granito según su origen geológico. En esta ínvestigación, se extrajeron 10 kg de arcilla caolinítica de tres lugares diferentes en un pozo mineral en S. L. P., México. El análisis de difracción de rayos X (XRD) se realizó en las diferentes muestras de caolín, luego se analizaron mediante microscopía óptica en el modo de analizador de imágenes para observar la variación del tamafio de Fe2O3 en las tres muestras de caolinitica diferentes. Se pudo verificar que existe una variación considerable en el tamaño de Fe2O3 para las muestras que provienen del mismo sustrato, además de que, cuando el tamaño de Fe2O3 se comparó entre sí, se observó una diferencia significativa en el tamafio de la hematita. La gran variación en el tamafio de la hematita en cada muestra sugiere una edad geológica reciente. Palabras clave: Caolinita; Microscopia; Mifracción de rayos Xt Pérez, A.S. & J.P. Salinas. (2018). Size variation ofFe2Q3 embedded in a kaolinitic clay of recent geological age. Celerinet. 6 (2), 1-5. 1 �CELERINET JULY - DECEMBER 2018 INTRODUCTION Clay is a petrographic term that is usually asigned to a material made up of certain minerals in variable proportions, it also refers to a fine grain and dusty material [ 1]. Different analysis by X-ray techniques have shown that kaolins are mainly composed of certain crystalline substances called clay minerals that are in escence hydro-alumina silicates [1]. Kaolinite (AhSi2Os(OH)4) is a hydro-alumina silicate with a triclinic or monoclinic structure that comes from mineral modification in its structure such as feldspar granite. During the tertiary and cretaceous ages it could be found in very thin rombic or hexagonal shape layers. The stoichiometric kaolin composition is: Al::O3:39.5%, SiOz:46.5%, H2O: 14%. Kaolinite is the main constituent material of kaolins. In certain places, kaolinite forms huge deposits where feldespatic rock erotion has been complete, it is usually transported by water in lakes mixed with quartz and other minerals making up clay beds. The highest purity clay, known as kaolin, has got many applications such as a paper constituent. lt is also used in the rubber and refractory industries, as added materials [ l] and even in diverse fields such as horticulture [4]. Sorne of the most common chromophorous materials found in kaolinitic clays are: MgO2, Fe2O3 and TiO2, ferrous oxides being the one with greatest impact in the kaolin color properties. During this research, it was found that Fe2O3 is not chemically combined on the studied kaolin clays, thus suggesting a young geological age for the mineral pit where these minerals were extracted. U.A.N . L. MATERIALS ANO EQUIPMENT Ten kilograms of kaolinitic clay were extracted from a mineral pit at Villa de Reyes, S. L. P., México. The studied kaolin for this investigation is called L28NM. The instruments used on this scientific research were: a) BaU ,nill, b) Powder X-ray diffracto1neter (Siemens D 5000), and c) Optical microscope (Olympus Bx60F ). L28NM was milled in the ball mili for one hour, afterwards, and X-ray diffraction analysis was carried out using the following conditions. OPTICAL MICROSCOPY In order to carry out an optical microscopy analysis of L28NM kaolinitic clay, very thin samples were prepared using a hydraulic press at 4,400 Lb for three minutes. The prepared samples were mounted on resine bases and polished a:fterwards. Each sample was analyzed at a 100X magnification and 5 micrographs were taken for its later analysis by an image analyzer software with a color discrimination function. Given the fact that ferrous oxide is red or dark in color it was possible to verify its presence by optical microscopy. STATISTICAL ANALYSIS An statistical analysis was carried out in order to observe the variation, homogeneity and tendency of the sizes of the ferrous iron oxide particles studied on the image analyzer. RESULTS EXPERIMENTAL Different tests and analysis were carried out in Centro de Laboratorios Especializados (Celaes) of the Facultad de Ciencias Químicas, 2 X-ray Diffraction (XRD) On Figure 1 we show the XRD analysis of L28NM, (JCPDS 14-164): �RESEARCH/ PHYSICS lttl() l:!ltM Clclt'aC l <(X) ..o w ,m l(IX) ~ 8X> o- e e .• e·1 e 8X> e ¿, w <IX> m o 1 e ll e Cu , C) 20 Ceu Cu 11) Cl0 a, Fig. 1: L28NM X-Ray diffraction pattern. Fig. 3: Optkal Microscopy of L28NM showing Fe2 0 3 embedded 1n kaolin clay. OPTICAL MICROSCOPY On Figures 2 and 3 Fe203 particles can be very easily identified on the micrographs taken ofL28NM. On Figure 4, the variation in size of Fe203 particles can be observed for the three samples of L28NM. • 1 • ••• • • o.s o Fig. 4: Fe203 Size evolution of Fe 20 3 on L28NM. Fig. 2: Optical microscopy of L28NM showing Fe 20 3 embedded in kaolin clay. 3 �CELERINET JULY - DECEMBER 2018 By the X-ray diffraction analysis it can Portland Cement. be concluded that L28NM is made up of the following major mineral compounds: saponite, [2] lmage Pro-Plus, Media Cybemetics Version stellerite, wollastonite, quartz and cristoballite 7.0 for Windows in accordance to JCPDS 14-164. Ferrous XP lron Oxide is not shown in the XRD pattern because its amount is too small for the XRD [3] Yanguatin H. et al., Pozolanic Reactivity of diffractometer resolution. Kaolin Clays, a review, Revista Ingeniería de On the statistical analysis based on the Construcción, ISSN 0718-5073, August 2017. obtained 1nicrographs using the image analizer software, a significative variation in size [4] Maier et al. , Evaluation of Kaolin Clays as for Fe2O3 particles could be observed. For an Altemative Management Tactic for Japanese samples 1 and 2 the sizes varied from 1,600 Beetle Feeding Damage in grape vineyards, to almost 3,000µm, whereas for sample 3 a Journal of Horticulture, ISSN 2376-0354, semi-uniformity for the size was found but are September 2016. larger in size compared to the ones for samples l and 2 and varied around 5,500 to 6,000µm. [5] Organismo Nacional de Normalización y From the Fe2O3 particle size variability, it Certificación de la Construcción y Edificación, can be concluded that L28'NM kaolin clay is S.C. , Norma Mexicana NMX-C-414-ONNCCE geologically young because of the fact that (1999). Fe2O3 particles did not have enough time to homogenize their size, and also because its [6] Balan, E., Calas, G., Bish, D.L. (2014) particles are not chemically combined with the Kaolin-group minerals: From hydrogen-bonded kaolinitic structure but are rather mixed in it. layers to environmental recorders. Elements: 10: 183-1 88. CONCLUSIONS [7] Behl, et al., Colored Titanoferous Coating The XRD analysis carried out on L28NM Pigment Obtained as a Flocculated By-Product show six mineralogic phases which are: in a kaolin purification process, U.S. Patent: saponite, kaolinite, wollastonite, stellerite, 5,688,315, November, (1997). crystoballite and quartz. The optical microscopy analysis and the statistical ana lysis on L28NM show an Fe2O3 size variation for the three studied samples, being sample 3 larger in size than the other two. From the Fe2O3 particle size variation it can be infered that L28NM is a geologically young kaolin clay which has a very pron1ising potential application in very diverse industries. [8] Williams, et al. , Method for Separating Mixture of Finely Divided Minerals U.S. Patent: 5,603,411. February, ( 1997). REFERENCES [10] J. lanicelli et al., Magnetic Separation of kaolin clay us,ng a high temperature superconducting magnet system, IEEE [l] ASTM Cl50, Standard Specification for 4 [9] Behl, et al., Colored Titanoferous Coating Pigment Obtained as a Flocculated By-Product in a Kaolin Purification Process, U.S. Patent: 5,584,394. December, (1996). �RESEARCH/ PHYSICS Transactions on Applied Superconductivity, June ( I997). [ 11] Williams et al. , Method for Separating Mixture of Finely Divided Minerals, ü.S. Patent: 5,603, 411 (1997). [ 12] Walter Borchardt, Springer, (1995). Crystallography, [ 13] Taylor, W; La Química de los Cementos, Urmo, (1967). ABOUT THE AUTHORS Á ngel Salvador Pérez Blanco Studied Mathematics at FCFM. He owns a Master degree in Computer Science and a Doctoral degree in Mathematics. He is currently doing research in Statistical Processes. angel. perezbl@uanl.edu.mx Juan Pablo Salinas Estevane Studied Physics at FCFM. He has a Master degree in Ceramics Engineering and a Doctoral degree in Materials Chemistry. He is currently doing research on Nano-Semiconductors. juan.salinassv@uanJ.edu.mx 5 �1 Angel Colin, 2 Pedro Valdés-Sada, ' Enrique J. Pérez, 3 Carlos E. Chávez, ' Eduardo Pérez-Tijerina; UANL - FCFMº - FIMEº - UMº in San Nicolás de los Garza, Nuevo León, México. ABSTRACT: We present sorne of the scientific and technological contributions that an emerging group of researchers from two universities in northeasthem Mexico have been performing in the past fi ve years, particularly in the area of planetary astrophysics. This includes: the development of a miniature space telescope, called RT-SAT (Refractor Telescope Satellite), that is being in1plemented into a 2U-Cubesat; the prelitninary results obtained during an observation campaign for the transiting planetary system HD189733; the first results of space debris detected with a 25-cm ORI-25 telescope at our ISON (International Scientific Optical Network) observatory; the results of planet dynamics obtained by means of theoretical and computational simulations; and the results obtained in our efforts to contibute to the Mexican Campaign of Asteroid Photometry (CMFA). Key Words: Planetary astrophysics; Exoplanets; Asteroids; Photometry; Cubesat; Satellite; Telescope. RESUMEN: Presentamos las contribuciones científicas y tecnológicas que un grupo emergente de investigadores en dos universidades del noreste de México han estado realizando en los últimos cinco afios, particularmente en el área de astrofísica planetaria. Esto incluye: el desarrollo de un telescopio espacial miniaturizado llamado RT-SAT (Refractor Telescope Satellite), el cual está siendo implementado en un cubo-satélite de 2-Unidades; los resultados preliminares obtenidos durante una campaña de observación para el sistema planetario que transita HD 189733; los primeros resultados de la basura espacial detectada con un telescopio ORI-25 de 25-cm en nuestro Observatorio !SON (Intemational Scientific Optical Network); algunos resultados de la dinámica de planetas, obtenidos mediante sin1ulaciones teóricas y computacionales; y los resultados obtenidos en nuestros esfuerzos para cooperar con la Campaña Mexicana de Fotometría de Asteroides (CMFA). Palabras clave: Astrofisica planetaria; Exoplanetas; Asteroides; Fotometría; Cubesat; Satélite; Telescopio. Colin, A., et al. (2018). Emerging planetary astrophysics and related techn ologies research in Northeastern Mexico. Celerinet. 6 (2), 6-21. �RESEARCH/ ASTROPHYSICS (TASP). This event is organized every two years by our group. Currently, the astrophysics Astronomy, astropltysics and outreaclt at and space sciencies staff is composed of nine UANL profesional astronomers and has collaboration agree1nents with other institutions such as the The Universidad Autónoma de Nuevo León Instituto de Astronomía UNAM, the Instituto (UANL) has a 63-year old Faculty of Physics de Astrofisica de Canarias (IAC) and other and Mathematical Sciences (FCFM). Early international research organizations. astronomy oriented activities commenced at The research activities of this group of this Faculty in the 1980s with a small group professional astronomers encouraged the FCFM of enthusiastic students and professors who administration to provide new funding for the promoted the design and construction of a small restructuring, rehabilitation and reactivation observatory, as well as performing outreach of the old observatory. The rededication of the events. The observatory was inaugurated in facilities was held in June of 20 16. The staff July of 1997, was located in the outskirts of the has now been assigned the resumption of the city of Monterrey, about 30 km away from the observatory 's old duties in performing both FCFM (Herrera, 2002), and was equipped with research an outreach activities in astronomy. a 12" LX200 Schmidt-Cassegrain telescope. The renewed facilities can be seen in Fig. 1. This facility was used mainly for trainning students in observational techniques and also for conducting astronomy outreach activities. It operated continously for around ten years and fostered collaborations with regional groups of amateur astronomers that worked together recording astronomical events. Lack of funding for maintainance, and local personal safety issues, forced the observatory to stop operations in 2006, but the outreach activities performed by this group of students (in collaboration with the authors) continue to this day. Professional research in astrophysics at the FCFM started in the year 2012 with a small group of academics assembled to conduct Fig. 1. Renewed facilities of the FCFM observatory, located research in the fields of astrophysics and at "Ex-Hacienda San Pedro·, in the outskirts of the city of Monterrey. (Picture credit: Esteban Castro). space sciences, including the development of astronomica1 instrumentation. In this same year a new postgraduate acade1nic program was created. lt was named: "Masters in Planetary Astrophysics and Related Technologies". Its first generation of students is expected to graduate in the middle of 2018 when four students will earn their master's degree. In march of 2017 the FCFM hosted the 3rd National Workshop in Planetary Astrophysics INTRODUCTION 7 �CELERINET JULY - DECEMBER 2018 The newly acquired equipment for this observatory is a 14" LX200-ACF f/10 optical telescope, equipped with a CCO Ca1nera and a computer system. This site will be part of the Laboratorio Nacional de Clima Espacial (LANCE), in a collaboration agreement with the Instituto de Geofsica UNAM and CONACyT. More information about LANCE, can be found at its own web page (http://www.lance.unam. mx/). Astrophyics and outreach at UDEM The astronomy program at the Universidad de Monterrey (UOEM) started in 1998 when one of the authors (PYS) oficially joined the Departamento de Física y Matemáticas as a fulltime professor. Initial research work involved characterization of the hydrocarbon chemistry and dynamics of jovian planetary stratospheres using ground-based high-resolution midinfrared spectroscopy as a complement for the observations performed in situ by spacebased instrurnents such as the Composite Infrared Spectrometer aboard the Cassini spacecraft (e.g. Hesman et al., 2009). This was accomplished in association with other researchers from NASA's Goddard Space Flight Center and working mostly at large astronomical facilities like Kitt Peak National Observatory and Mauna Kea Observatories. At the same time a program was developed to Iocally design and construct an astronomical observatory. Its purpose would be to carry out observations aimed at: i) covering the educational needs of students leaming basic astronomical techniques, and ii) contributing to original astronomical research projects. The first instrument used was a commercial 18-cm f/15 Maksutov telescope equipped with a basic 14-bit CCO camera. The first project involved follow-up astrometric measurements of asteroids. For this work the Minor Planet Center assigned the number 720 as the designation for the Universidad de Monterrey Observatory. This designation is useful predicting local observing circumstances for Solar System objects by a wide range of applications, such as the Jet Propulsion Laboratory's Horizons System (https://ssd.jpl.nasa.gov/horizons.cgi). Other observing projects which could be achieved with small telescopes were soon implemented. These included the timing of stellar occultations by the Moon and by asteroids (e.g. Sada and Pesnell 2000). These observations help us characterize binary stars, improve stellar coordinates, outline the limb topography of our Moon, and determine the size, shape and improved orbit of asteroids. This is also a useful technique to detect binary asteroids. A video system, Iinked with GPS-precision timing, was also implemented at the observatory to register these astronomical phenomena with greater precision. Using these video tools, meteoroid impacts were registered on the Moon (e.g. Ortiz et al. , 2000), and mutual events (eclipses and occultations) of planetary moon systems were recorded for Jupiter, Saturn and Uranus in order to improve the orbital elements of the satellites (see, for example, Arlot et al., 2009 and Mallama et al., 2009). The UOEM Observatory was upgraded in 2004 with the addition of a two-meter fi berglass dome that houses a commercial 36-cm f/10 (now an f/8) Schmidt-Cassegrain telescope equipped with a newer 16-bit CCO camera that uses standard photometric filters (see Fig. 2). These improvements allowed for observations of fainter targets within a larger field-of-view. Since this upgrade the projects that have engaged most of the observing time at the UDEM Observatory have been photometric in nature. �RESEARCH/ ASTROPHYSICS Fig. 2. Universidad de Monterrey Observatory - MPC 720. (Picture credit : Pedro Valdés-Sada). The two main avenues of research include: i) the characterization of extrasolar transiting planets ( in particular their sizes) through observation and analysis of their light curves and ii) the determination of the rotation period; of asteroids, also through the observation and analysis of their light curve shapes. So far 340 light curves of extrasolar transiting planets have been recorded at the UDEM Observatory, and over 50 asteroids have been photometrically observed. These results and future work are discussed in more detail in Sections 2.1 and 2.4. Other related projects, such as the characterization of variable stars ( e.g. Sada, 20 l O), have also been carried out using photometric techniques. Outreach work at the Universidad de Monterrey, besides offering astronomy lectures and hosting star parties for the general public, have centered on the production and broadcast of the one-hour weekly radio program entitled: "Obsesión por el Cielo". The show is aimed at .ª general audience interested in astronomy, sc,ence and space exploration and covers topics of interest and astronomica1 news and events. "Obsesión por el Cielo", is broadcast live from the studios of the Universidad de Monterrey on-air radio station (Radio UDEM 90.5 MHz FM) and also streamed live through the web (http://www. udem. edu.mx/radioudem/). The show is also recorded and placed on the web as a podcast so that a wider audience can enjoy it at their leisure (https://obsesionporelcielo. podbean.com/). . "Obsesión por el Cielo", commenced airing 1n the year 2000 only during the school term, began to be streamed live through the web in 2006, and started its podcast format (now with 50 programs per year) in 2010. So far over 730 epi~odes of the show have been produced, of wh,ch over 360 are available as podcasts. The program aJso maintains itsown webpage (https:// obsesionporelcielo.net/) and Facebook (https:// www.facebook.com/obsesionporelcielo/) page to better serve the needs of its audience. PLANETARY SCIENCE AND SPACE TECHNOLOGY Cliaracterization o/ exoplanets The search and characterization of exoplanets is currently one of the most exciting and active topics of research in astronomy. The discovery of giant planets, in short-period orbits in particular, raises interesting questions and provides important constraints on models that describe planet formation and orbital migration theories. Many of these planets have orbital plane inclinations nearly perpendicular to the plane of the sky which allows us ' from Earth' to literally see the planets cross the disk of their stars. This effect manifests itself as a temporary dimming of the star' s brightness as the planet crosses irl front of their disks. These are called transiting planets, and their light curves yield a wealth of information about the system. Of particular irnportance is the size of the planet in con1parison to the star which, co1nbined with its mass derived from the orbit, can give us the average density of the planet; a first step in understanding its structure. A lot of the effort in this feld has been . 9 �CELERINET JULY - DECEMBER 2018 concentrated on the discovery of exoplanets, but their follow-through and improved characterization is also an important aspect of the venture which has not garnered as much attention. This is of particular interest if we want to know, for example, if the system has other non-transiting planets. This can be achieved with the systematic observation of transits of the known planet and recording long-term transit timing variations (TTV). This method has already been used to confirm the planetary nature of systems with multiple transiting planets (e.g. Holman et al. , 201 O). These followthrough observing programs are ideally suited for dedicated medium-sized telescopes from smaller institutions with groups of students in the process of learning basic astronomical observing techniques. There are enough known exoplanet transiting systems that almost every night one or more events can be recorded at a given site. In addition, these observations could be done at various wavelengths, not only to record the mid-transit time, but also to characterize the limb-darkening of the host star, and to refine the basic parameters of the planetary system; in particular the inclination of the orbital plane - i, the radius of the planet with respect to the star - Rp/R*, and the distance of the planet in stellar radii units - a/R* (e.g. Sada et al., 2012). Transits of exoplanets have been recorded at the UDEM Observatory since 2004 using the equipment described in Section 1.2. These observations have been used to complement those obtained through other wavelengths with larger telescopes at other observatories, sorne ofthem space-based such as Spitzer and Kepler (e.g. Todorov et al., 2012). One particular technique that has been successfully developed and applied has been the combination of severa! light curves obtained with modest-sized 10 HAT- P- 3 1 o + - le 0.90 0.80 0.75 - 0 . 10 -0.05 0.00 0.05 Fig. 3. Six transits of the exoplanet system HAT-P-3 were obtained at the UDEM Observatory (MPC 720) through a standard lc-band photometric flter (upper light curves) on various occasions. Note the relatively high scatter of the individual observations due to the small telescope aperture. The bottom light curve (diamond symbols) represents the combination of the previous six light curves. Note the improved S/N which allows far an improved model fit (salid line far each light curve). These data were analyzed in Ricci et al, 2017. These individual light curves are relati vely noisy and yield little useful information, but the combination of severa! of these, obtained with the same equipment, significantly improves the signal-to-noise of the final transit light curve. This light curve has the same quality as one obtained with a larger instrument and can be analyzed and modeled to yield useful information on the exoplanet system (e.g. Sada and Ramón-Fox, 2016). This can be achieved economically without having to apply for expensive and competitive large-telescope observing time. Figure 3 shows an example of how six �RESEARCH/ ASTROPHYSICS individual light curves obtained with a smaJI telescope can be combined to yield an improved light curve with higher S/N that can be modeled and analyzed. The main goals of the RT-SAT are to conduct photometric studies of nearby bright stars for ·- -- Developnient ofll nunillture spllce teles cope in ll 2-U CubeSat The demand of space technologies for research and education in Mexico has greatly increased it the past decade. However, plans to develop space 1nissions, satellites or spacecrafts are sti11 scarce; not only because of the implicit high costs for these kinds of projects, but also due to a lack of individuals specialized in space engineering and with the capacity for carrying through space 1nission projects from start to finish. Up until now, there have been only two small satellites built and successfully launched by a Mexican university (UNAMSAT- 1 and UNAMSAT-B in the early 1990s), but only one of them completed its mission (https://nssdc. gsfc . nasa .gov /nmc/spacecraftD is play. do? id= l 996-052B). There are severa! promising satellite projects that are being developing at Mexican institutions today, mainly for communications research (Pacheco, 2009), but there are none planned for planetary astrophysics research. To address this, we are studing the viability of a space mission for observing and monitoring bright stars with transiting exoplanetary systems. To achieve this, we have proposed the implementation of a miniature space telescope with a diameter of 80-mm, called RT-SAT (Refractor Telescope Satellite), and designed to operate in Low Earth Orbit (LEO). This space telescope consists of an optical system built around an 80-mm f/5 achromatic lens coupled with a l620X l220 CCD camera. The telescope has an extensible optical tube that spands a 400-inm focal length with an estimated resolution of arow1d l.4 arcseconds. The whole devise fits within the small dimensions of a 2-U Cubesat, as can be seen in Fig. 4. ,._ -... "" -- - -.. --• ... - Fig. 4. Schematics and conceptual design for the RT-SAT in a 2-U Cubesat. For clarity, the optical tube at left is shown as transparent. The main concept and design for the RT-SAT is described in (Col in, 2016), whereas the satellite operating concept is brevely decribed as follows: Once the satellite's insertion into a Low Earth Orbit (LEO) at 400-km, and the power system and command links are stable, the telescope would be constantly observing the saine star unless new orders for pointing ata diffrent target are uplinked. In operating mode the telescope would nominally be pointing constantly at the target star, but would only be actively observing and taking data while the satellite is in the orbit nigth around the Earth. During the orbit day, the satell ite would be under sunshine and would thus be able to recharge its batteries and download the gathered data, or eventually to receive new instructions (downlink/uplink). At least two ground receiving stations should be located as far away as geographically possible in Mexico in order to maximize the data aquisition time. 1t is recomended that more ground receiving stations be used for redundancy. This is depicted 11 �CELERINET JULY - DECEMBER 2018 in Fig. 5. For the attitude determination and control system (ADCS), we propase to use six engines acting as reaction wheels, two for each x,y and z axis respectively, whose n101nent storage is around 8 mN•m•s at 1200 rpm, anda 1naximum torque of 6.5 mN• m. The communication system used to downlink the mission data to the ground station will be a Stensat radio beac?n transmitter module in a SoC (Syste1n on Chip) operating at a frequency of 437.465MHz at a speed of 9600 bps and with an omnidirectional monopole antenna. In general terms, the irnplementation plan for achieving a successful misión for the RT-SAT will consist of two phases. The first phase involves the development of the conceptual design, construction of the engineering model, and ground testing of the model. The second phase involves the construction of the ight model, ground testing, launching, operational observations (uplink:/downlink data) in orbit, and the activation of ground stations. The data analysis period by researchers and students at their own institutions is scheduled for 12 months, but n1ay be extended depending on the quantity/quality of the acquired data. sequence during an orbit (observation at orbit nigth and downlink data at orbit day). Back-ground picture was taken from: https//www.google.eom.mx/maps/@20.9148596,94.4769735,22965691m/data=!3m1 !le 3. Asununary ofthe irnplementation plan is shown in Table 1. Table 2 shows the estimated cost for the overall project. It should be pointed out that the overa!! project schedule presented here was designed for an ideal case in which a full funding progam has been established from ~e begining ali the way to a succesfu.11 conclus~on of the mission. In our case, dueto our fundtng limitations, we are still in the 1st phase of the project. At present we have acquired: a) a 2-U Cubesat stardardized structure, b) a 1620xl220 Color CCD Camera, c) a set of 80-mm achromatic doublet (lenses), d) a Lambda Sat computer board, e) a XRIYA power system boa_rd, t) a set of six 1nicro-motor (for use and test1ng as reaction wheels), g) an aluminum-606 1 piece for holding both the CCD camera and the reaction wheels respectively, and h) a set of 16 alumninum-6061 pieces to conform the extensible optical tube. A picture of the co1nponents acquired an fabricated so far can be seen in Fig. 6. Table l. RT-SAT implementation plan Task name 1st Phase Conceptual design Mission concept rev1ew Duration (months) 2 l Design (Blue prints 3 and 3D model) Subsystems assembly 3 and integration Fig. 5. Schematic diagram for the satellite's operations 12 �RESEARCH/ ASTROPHYSICS Task name Engineering model construction Ground testing 2nd Phase Fligth model construction Fligth model testing Launch Operational observation on orbit Data analysis TOTAL Duration (months) 2 6 3 1 12 12 48 .. .. - Fig. 6 . Sorne components and fabricated parts of the RTSAT engineering model. The next step of the project is to start the testing process for the assembly ofthe engineering model shown in Fig. 7 in order to validate the accuracy and performance ofthe telescope. Table 2. Estimted cost for the RT-SAT m 1ss1on. Description $USO 2/U Metalic structure 3,500.00 Payload (80mm telescope) Communication system C&DH 2,000.00 3,000.00 Attitude control 80,000.00 Power system 2.500.00 2,000.00 Tracking ground base 3,000.00 telescope 4,000.00 Ground station Qualifcation for space Launch 50,000.00 TOTAL 400,000.00 250,000.00 Fig. 7. The engineering model of the RT-SAT assembled. To help achieve this goal we planned an observing campaign during August of 2017. As a test, we observed one transit ofthe exoplanet system HD189733, which is bright (apparent 1nagnitude of 6.2) and also visible from the northern hemisphere during the summer. The equipment used was the 36-cm UDEM Observatory telescope described in section 1.2 but, for our purposes, the ful! 360-min aperture of the telescope was reduced down to a diameter of 75-mm, similar to that of the RT-SAT. Ali photometric measure1nents taken with this telescope were made unfiltered and with an exposure time of 13 �CELERINET JULY - DECEMBER 2018 60s for each image. The preliminary results are shown in Fig. 8. l-lere, the error bars denote the noise caused by atrnospheric perturbations such as turbulence and/or clouds. These are nonexistent observing fro1n space and thus the noise would be much smaller. ... ,C,t,ll:J'llil, . . . . . . Q.71'tJ •• • • t A 25-cm ORl-25 telescope was installed in September of 2016 on the roof of the Physics and Mathematics Research Center building of the UANL in the city of Monterrey (see Fig. 9) and since that ti.tne it has carried out observations of space debris. The ORI-25 telescope has a 3.3x3.3 degree field-of-view and operates with an FLI ML09000 CCD camera. This camera has good performance down to a limiting ,nagnitude of about 14 despite the surrounding light pollution problem. Residuals from measurements obtained so far range from 1-2 arcsec . • • l '"' 1 r·... ........ ..... -· .... , ~ ... '.. c:a,,.' ... ~ --- ... Fig. 8. Transit of the exoplanet system HD189733 obtained at the UDEM Observatory (MPC 720) in August 2017 w ith the nominal 360-mm telescope apertura reduced down to 75-mm to match the aperture of the RTSAT. (Credits: P. Valdés-Sada). The next observing campaign is scheduled for next year and will include the same target star, the UDEM Observatory telescope, the RT-SAT engineering model and a small motorized 80mm f/5 telescope. The results will be compared to validate the quality of our engineering model. 2.3. Monitoring of orbiting satellites and space debris The UANL has joined the lntemational Scientific Optical Network (ISON). The ISON Observatory at UANL is part of a global network of 37 observatories designed for observing space debris, Near Earth Asteroids (NEOs) and gam1na-ray-bursts (Zalles Barrera et al., 20 15). 14 Fig. 9. The ISON Network te lescope, provisionally mounted on the roof a building at the FCFM -UANL in the city of Monterrey. Our new observing location for the ISON Network covers the GEO survey longitudes between -177 and -41 degrees West Longitude (Molotov et al. , 2014), complementing the longitude range of the 1so·N observatory at Cosala (Autonomous University of Sinaloa) and duplicating the ISON observations from Tarija, Bolivia (Juan Misael Saracho Autonomous University). This duplication is i.tnport.ant due to varying weather conditions at the different latitudes (specially important in the winter season). There were 68 observing nights between October 20 16 and April 2017 that yielded 151903 1neasurements in 22520 tracklets. An �RESEARCH/ ASTROPHYSICS example of the first results obtained by our syste1n are shown in Fig. 1O. 0n the same building there is a 35-cm MEAD E telescope already installed that is used for educational purposes. This telescope will also be used for observations of space debris (by targeting) after equipping it with an FLI ML8300 CCD camera. This telescope is additionally planned to be used for bright asteroid astrometry and photometry. model. Fig. 10. Space debris detected with the ISON telescope at UANL. Monitoring ofasteroids as Near Earth Objects (NEOs) Asteroids, comets and meteoroids are minar, but plentiful, me1nbers of the Solar Systen1. Their study in general allows us to improve our understanding about the origin and evolution of the Solar System. Toe dynamics of these objects have been studied by measuring their positions in the sky at a given time (astrometry) and then, from that information, calculating the orbital elements that define their orbits. Photometric techniques in particular are useful for determining the rotation period of asteroids. Their generally irregular shape reects sunlight in proportion with the area exposed to sunlight, and this manifests itself as brightness variations in the light curve as the asteroid rotates. This technique can also be used to identify binary asteroids and to calculate their rotation and orbital periods. See Wamer (2003) for a full description of these photometric techniques and their uses. The UDEM Observatory has been contributing to the pool of knowledge regarding asteroid rotation periods since the year 2000 (Sada, 2000). Over 50 asteroids have been observed and their light curves registered and published (see, for exrunple, Fig. 11 , Sada, 2006 and Sada, 2008). A new observatory is under construction on an UANL suburban campus branch atan altitude of 1750 meters. The plan is to move both telescopes to this new location in 2018. In addition, a new 50-cm telescope will be jointly installed at this location to increase our cooperation with the ISON Network. • 1U2L•ce 15 �CELERINET JULY - DECEMBER 2018 Fig. 11. Upper panel - Path of Main Belt asteroid 1292 Luce for two consecutive observing sessions at the UDEM Observatory (MPC 720) during January 2008. The asteroid trajectory is shown for each night, and the comparison stars used are also indicated in purple (Jan. 7th) and yellow (Jan. 8th). The star within the red circle is GSC 1393-1461, a previously uncatalogued eclipsing binary star. The stars inside green squares were used as comparisons for its characterization (Sada, 2010). Lower panel - Light curve of asteroid 1292 Luce from Sada (2008). In Mexico, there has been a recent interest for the development of national expertise in the study ofNear Earth Objects (NEOs): asteroids, comets and meteoroids that come close to the orbit of the Earth and could collide with our planet in the future. Those objects that come particularly close to Earth, and are larger in size, are also known as PHOs, or Potentially Hazardous Objects. Thousands of NEOs and a few hundred PHOs are known. This interest has increased the number of Mexican research astronomers active in the study of asteroids. This effort resulted in the organization of the Campaña Mexicana de Fotometría de Asteroides (CMFA) (http ://www.astro.uson.mx/cmfa/CMFA2016/ CMFA2016/Bienvenida.html) at the 2nd Taller Nacional de Astrofísica Planetaria held on the UANL campus in Monterrey during 2015. The goal of this campaign is to organize, coordinate and share photo1netric observations of asteroids between interested parties at various national observatories and university research centers. The results of the first CMFA are published in Sada et al. (2016). In addition, a special workshop was organized in August of 2016 at the same UANL campus for the purpose of sharing observing and data reduction techniques, and a special session on NEOs was organized at the 3rd TaJler Nacional de Astrofisica Planetaria in 2017 (http://tasp.fcfin.uanl.mx/index.php/es/). Interest in contributing to the now yearly CMFA 16 has increased, and each year more targets are selected and more observers are participating. The members of the northeastern group are also engaged in this topic and are involved in the efforts to organize a national network for research of Near Earth Objects (NEOs). This network is currently composed by members of six mexican institutions: UANL, UDEM, IAUNAM, Universidad de Sonora (UNISON), Universidad de Guadalajara (UdeG), Instituto de Estudios Avanzados de Baja California (IdEABC) and Instituto Politécnico Nacional (IPN). The main goal of this network is to create a set of observational stations for the detection and monitoring ofNEO's, as well as the development of instrumentation and observational techniques that can provide a contribution to international efforts undertaken in this area. The NEO program has the following requirements: i) a field-of-view wider than 1.5 degrees for efficient survey work, and ii) the size of a stellar image at the focal plane should match the typical FWHM seeing at the site. Medium size telescopes will operate in tandem with other fast (with a small focal ratio) telescopes from the Mexican Network. Detection and tracking of NEOs is of great importance from a scientific and social point of view because of the risk involved from potentially hazardous impacts in densely populated regions. There are many intemational efforts aimed at detecting and tracking NEOs (e.g., Catalina Sky Survey and WlSE satellite) which have contributed to the detection of thousands of these objects. The basic process for the detection of asteroids, NEOs, and space debris, involves obtaining a large nwnber of wide field-of-view ünages. We will also use these images in other research progrruns, particularly for the detection and monitoring of transient phenomena such as comets, nova, supemova and other types of variable stars. �RESEARCH/ ASTROPHYSICS that is coupled with the sky through a 50 Ohm periodic-logarithmic antenna (Benz, MonsVarious manifestations of solar activity are tein and Meyer, 2005). The antenna (Fig. 12) considered as the cause for perturbations in in- is currently located on the roof of the FCFM terplanetary space. They have been the subject building, but the equipment will eventually be of interest because of their predicted effects on operating at its final destination at the location the Earth's magnetosphere and atmosphere, of the new UANL observatory atan altitude of and in particular, the effects on space-based and 1750 meters, and where low radio interference ground-based telecomunication facilities. Solar conditions are present. ares are the most energetic phenomena (1032 An interesting topic in solar are research is the erg) in the Solar System. Fiares are entirely estirnation of how partition energy proceeds driven by magnetic energy at chormospheric from primitive magnetic energy to various levels, producing acceleration of particles and other kinds such as thermal, non-thermal (parsudden radiation emission at practically ali wa- ticle acceleration) and radiation energies. A sovelengths of the electro111agnetic spectrun1. lar are was observed in X-rays, UV and Radio Observations in the X-ray spectral range have frequencies on May 15, 2013 by severa! orbirevealed spatial as well as spectral features tal and ground instrwnents. The basic plasma identifed with the standard model of solar ares. parameters were then estimated from the comlt is widely accepted that the prirnary accelera- bination of the observed data. lt was thus postion of particles is due to magnetic reconnec- sible to estímate for the first time the plasma tions between preexisting magnetic loop arcade bulk kinetic energy from the thermal, non-therstructures and emerging structures, carrying mal and magnetic energies. Time variations of plasma from chromospheric levels. Reconnec- these quantities clearly explained the transfer ted lines are oppositely directed, and accelera- between magnetic and non-thermal energies ted particles collide with ambient plas1na, emi- (Kontar et al., 2017). This type of energy-transtting Hard X-rays (HXR). Plasma in upward 1notion promotes the presence of turbulence and shock waves in the coronal environment. Perturbation of plasma emission is evidenced through radiobursts atinillitnetric to metric wavelengths. For downward precipitating particles from the reconection sites, collisions with loop aring structures causes HXR sources at looptop and loop footpoints. The former are located at coronal leves while the later are located at low Fig. 12. SO Ohm periodic-logarithmic antenna that chromospheric levels where high density plas- couples the sky signal with the Callista spectrometer. All 1na is heated up by collisions with the stream of equipment is currently located at the UANL campus. accelerated particles. Eventual evaporation of super hot plasma fills the loop structure making it bright at Soft X-Ray wavelengths. Our group at the UANL is in the proccess of becoming a collaborator of e-Callisto, a global network of researchers that monitors the radio solar emission through a heterodyne receiver system X-Ray fiares and radioburst observations 17 �CELERINET JULY - DECEMBER 2018 Theoretical and computational efforts at Uranus and Neptune closer to the Sun, compa- UANL red with their present positions), and ali ofthem in resonance with each other. They are also inAlong the observational endeavors made at the teracting with a disk of debris with an inner UANL, we are getting severa] theoretical ac- edge at 30 AU. Because of computational time complishments. The UANL Astronomy group limitations, in ali these studies the disk particles has worked in different theoretical research re- are treated as being able to feel the gravitational lated to the stellar and planetary dynamics. force of the four planets, but not any gravitatioOur group has obtained, thanks to a PROMEP naJ force from the other particles. This simpli(Programa de Mejoramiento del Profesorado, fication, that seems reasonable at first, <loes not SEP) 2013 grant, three high performance ser- model the system completely. In our models we vers. Each server has 64 cores (four 16-core do take into account gravitational inteactions AMD Opteron), support 1TB ofRAM me1nory, between particles. In their over-simplified in16 DlMM size. That adds up to a total 192 co- tegrations the systems are stable for over 200 res for the three of them. These type of servers Myrs, while in ali our results they become unsneed to be stored in a cool room. Our equipment table in less than 40 Myrs. We thus conclude is kept safe at the appropriate temperature and that the initial configuration as a multiresonant conditions at the Dirección de Tecnologías de la configuration is unlikely, unless a more realistic Información (DTI, UANL). We acquired ali the model says otherwise. pieces and the assembly was carried out by our Table 3 shows one of the possible initial congroup in collaboration with a researcher from ditions that the planets 1nay have had just after the Instituto de Astronomía, UNAM at Ensena- planet formation ended, these initial conditions da. This equipment allows us to perform multi- correspond to the 3J:2S, 4S:3U, and the 4U:3N ple numerical integrations simultaneously. resonance. These conditions suggest that the The UANL Astronomy group is also working giant planets were originally in a more compact in various theoretical research fields related to configuration. We can see their locations in the stellar and planetary dynamics. One example phase-space plane shown in Fig. 13. Black, is our work on a multiresonant self-consistent darkgrey, grey and light-grey dots, represent model for the initial architecture of the Solar Jupiter, Saturn, Uranus and Neptune respectiSystem. We have explored the long-term stabi- vely. The curves that appear are the maximum lity of the outer planets in multiresonant resonance width. That means that if any of the configuration with a self-gravitating planetesi- planets gets outside of this curves, dueto gravimal disk (Reyes-Ruiz et al. 20 15). In this work tational interaction with the rest of the planets, we studied the different possible initial configu- they will not be in resonance anymore and a ration for the four outer planets. According to chaotic behavior for the whole systen1 is expechydrodinamical studies, the initial ted. configuration of these four planets was likely resonant (Levison et al. 2007). These type of studies are called Nice-type models (Gomes et al. 2005, Tsiganis et al. 2005 and Morbidelli et aL 2005). In ali of these previous studies the four giant planets are placed in resonant orbits and in compact configurations (with Jupiter slightly farther away from the Sun, and Saturn, 18 �RESEARCH/ ASTROPHYSICS Table 3. lnitial conditions for planet formation. merical study for Kepler 453 and Kepler 1647. Future computational efforts are planned to improve our astrono1nical co1nputational faciPlanet a e lities. First, we want to increase the RAM me1nory to the maximum possible of l TB for the Jupiter 5.84724 0.00690581 three servers we have. Second, we want to conSaturn 7.83006 0.260594 nect ali iliree servers with each other in order to have a single server with l 92 cores, so it can Uranus 9.67303 0.0163112 also be used to run hydrodynamical simulations Neptune 11.6361 0.0179751 of planet formation and other parallel multicore research tasks. Additionally, we are applying We made 20 numerical integrations, exploring for different grants in order to acquire more serdifferent resonant configurations, with the full vers to increase our computational power. equations of motion for the four planets and 2000 lunar n1ass bodies; ali self-consistent. The integrations were performed for 100 Myrs. The computational challenge was large and it took months to finsih each integration, as can be •• u seen in Fig. 13. We also have studied the dynamical envi- f., ronment of circumbinary planets (Chavez et al. 2015), we studied the stability of the Kepler-field circumbinary planetary systems with one planet that were known in 2014. These Fig. 13. The dots represent the initial location of the four systems are: Kepler- 16, Kepler-34, Kepler35, giant planets according to the Nice model with resonances Kepler-38, Kepler-64 and Kepler 4 13. We per- 3J:2S, 4S:3U, and 4U:3N (see text for explanation). The curformed numerical simulations of the full equa- ves shown correspond to the maximum resonance width tions of motion of each system. Our aim was for each planet. to verify the stability of the planetary orbit. Three numerical experiments were completed. CONCLUSJONS In the first one we performed a 1Gyr numerical integration of the nominal solution for ali ln Mexico, research and education in the field of six Kepler systems. In the second experiment planetary sciences is on the rise thanks to mexiwe searched for the critica! semi-major axis for can institutions that provide a signifcant numall planets. Finally, in the third experiment, we ber of posgraduate students with skills in these constructed a two-dimensional stability map on areas. This includes not only the formation of the eccentricity vs. pericentre distance. In this astrophysicists, but also of engineers speciatype of plot, we can see the dynamical environ- lized in space technologies. This goal is also ment around the planet and where the unstable possible because of the young scientists and areas are located. We found that Kepler-64 is researches who retum to Mexico aft.er having very close to unstable areas, but its nominal so- the opportunity of completing a posgraduate lution is stable. The rest of the systems are also program at a foreign university. Furthermore, stable, and far away from any areas of instabi- the expertise acquired during postdoctoral stays 1ity. Currently, we are performing a similar nu- and/or collaboration stays of these researchers, .. ., . 19 �CELERINET JULY - DECEMBER 2018 specially when these individuals have participated in space missions organized by intemational consortia, is of great value. These skills are very important for the development of new 111odest space mission projects that can be achieved by individuals or with small groups of people. These projects also provide the opportunity for a high-quality education an training of new students in their own institutions. Miniaturized satellites for example, are important for multidisciplinary education programs in space sciences and provide a great oportunity to start collaboration's projects between engineers and astrophysicists. The newly-dedicated facilities of the astronomical observatory at the UANL are now focused on planetary science projects, on outreach, and on teaching and research in other areas of astronomy. Eventually they will also be used for the acquisition of asteroid and exoplanet transit lightcurves. From these last observations, we will also be able to compare the data acquired with the RT-SAT when it successfully concludes its mission in space. The members of northeastern Mexico's research group are involved to organize a national network for research of Near Earth Objects (NEOs), in which six mexican institutions participate to create a set of observational stations. The ultimate objetive of this research group is to foster research and to form future astrophysicists and technologists specialized in the general field of planetary sciences. ACKNOLEDGEMENTS REFERENCES [ l] Arlot, J. E., Thuillot, W., Ruatti, C., et al., 2009, A&A, 493, 1171 [2] Benz, A. O., Monstein, C. Meyer, H , 2005, Sol. Phys., 226, 143 [3] Chávez, C. E. , Georgakarakos, N. , Prodan, S. et al. 2015, MNRAS, 446, 1283 [4] Colin, A., Valdés-Sada P. , Olguín L., et al., 2016, lAC- 16, B4, 2,3, x33235 [5] Gomes, R., Levison, H. F., Tsiganis, K. , et al. , 2005, Nature, 435, 466 [6] Herrera, V., 2002, Ciencia UANL, 4, 539 [7] Hesman, B. E., Jennings, D. E. , Sada, P. V., et al. , 2009, lcarus, 202, 249 [8] Holman, M. J. , Fabrycky, D. C. , Ragozzine, D., et al., 20 l O, Science, 330, 51 [9] Kontar, E. P. Pérez, J.E., Harra, L. K ., et al., 2017, Phys. Rev. Lett., 118, 155 101 [ l O] Levison, H. F. Morbidelli, A. Gomes, R. et al., 2007, Planet Migration in Planetesimal Disks, Protostars and Planets V, B. Reipurth, D. Jewitt, and K. Keil (eds.), University of Arizona Press, 669 [1 1] Mallruna, A., SAoma, M., Sada, P. V., Modic, R. J. , and Ellington, Ch. K., 2009, lcarus, 200, 265 Part of the present projects are supported by: Agencia Espacial Mexicana (AEM), through the grant number: AEM-2014-1-248438; [ 12] Molotov, l., et al. , 2013, 6th European conUANL, through the grant number: PAI- ference on space debris, ESA special publicaCyT-IT401-15, and Direction's Department of tion, 723, 26 the FCFM-UANL. [ 13] Morbidelli, A., Levison, H. F., Tsiganis, K. , et al., 2005, Nature, 435, 462 20 �RESEARCH/ ASTROPHYSICS [ 14] Ortiz, J. L., Sada, P. V., Bellot R ubio, L. R., et al. , 2000, Nature, 405, 921 blishing [29] Zallez-Barrera, R , et al. , 2015, RevMexAA (SC), 46, 91 [15] Pacheco, E., et al., 2009, AlAA, 6410, l [ 16] Reyes-Ruiz, M., Aceves, H., Chavez, C. E., 2015, ApJ, 804, I.D. 91 [ 17] Ricci, D., Sada, P. V., Navarro-Meza, S. , et al. , 2017, PASP, 129:064401 , 8 [ 18] Sada, P. V., 2000, The Minor Planet Bulletin, Vol. 27, No. 3, 25. [19] Sada, P. V. and Pesnell, W. D., 2000, Ciencia UANL, Vol. 3, No. 2, 191 [20] Sada, P. V., 2006, The Minor Planet Bulletin, Vol. 33, No. 4, 78 [21] Sada, P. V., 2008, The Minor Planet Bulletin, Vol. 35, No. 3, 105 [22] Sada, P. V., 2010, JAAVSO, Vol. 38, No. l , 52 [23] Sada, P. V., Deming, D., Jennings, D. E., et al. 2012, PASP, 124, 212 [24] Sada, P. V. and Ram_on-Fox, F G ., 2016, PASP. 128:024402, 13 [25] Sada, P. V., Navarro-Meza, S., Reyes-Ruiz, M., et al., 2016, The Minor Planet Bulletin, Vol. 43, No. 2, 154 [26] Todorov, K. O. , Deming, D. Knutson, H. A. , et al., 2012, ApJ, 746, I.D. 111 [27] Tsiganis, K., Gomes, R. , Morbidelli, A., et al. , 2005, Nature, 435, 459 [28] Warner, B. D ., 2003, A Practica! Guide to Lightcurve Photometry and Analysis, Bdw Pu- 21 � Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Celerinet Description An account of the resource La revista Celerinet, inició en el 2012, sólo en formato digital, es semestral y se mantiene activa; ofrece información de las últimas investigaciones realizadas por docentes, estudiantes y egresados de la Facultad de Ciencias Físico Matemáticas, también se encarga de difundir las actividades institucionales más relevantes. La publicación incluye artículos de  investigación relacionados con las siguientes áreas: matemáticas, matemáticas aplicadas, física, ciencias computacionales, actuaría, multimedia y animación digital, y seguridad en tecnologías de información. Text A resource consisting primarily of words for reading. Examples include books, letters, dissertations, poems, newspapers, articles, archives of mailing lists. Note that facsimiles or images of texts are still of the genre Text. Título Uniforme Celerinet Año de publicación El año cuando se publico 2018 Año Año de la revista (Año 1, Año 2) No es es año de publicación. 6 Número Número de la revista 2 Mes de publicación Mes cuando se publicó Julio-Diciembre Día Día del mes de la publicación 1 Periodicidad La periodicidad de la publicación (diaria, semanal, mensual, anual) Semestral Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. 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La publicación incluye artículos de  investigación relacionados con las siguientes áreas: matemáticas, matemáticas aplicadas, física, ciencias computacionales, actuaría, multimedia y animación digital, y seguridad en tecnologías de información. 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Access Rights may include information regarding access or restrictions based on privacy, security, or other policies. Universidad Autónoma de Nuevo León Rights Holder A person or organization owning or managing rights over the resource. El diseño y los contenidos de La hemeroteca Digital UANL están protegidos por la Ley de derechos de autor, Cap. III. De dominio público. Art. 152. Las obras del dominio público pueden ser libremente utilizadas por cualquier persona, con la sola restricción de respetar los derechos morales de los respectivos autores. Astrophysics Emergin planetary Size variation of FE2O3 Technologies research