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A Method for Identifying the Pleiades Star Cluster in a Khipu From
Saez-Rodríguez. A. (2012). An Ethnomathematics Exercise for Analyzing a Khipu Sample from Pachacamac (Perú). Revista Latinoamericana de Etnomatemática. 5(1). 62-88 Artículo recibido el 1 de diciembre de 2011; Aceptado para publicación el 30 de enero de 2012 An Ethnomathematics Exercise for Analyzing a Khipu Sample from Pachacamac (Perú) Ejercicio de Etnomatemática para el análisis de una muestra de quipu de Pachacamac (Perú) Alberto Saez-Rodríguez1 Abstract A khipu sample studied by Gary Urton embodies an unusual division into quarters. Urton‟s research findings allow us to visualize the information in the pairing quadrants, which are determined by the distribution of S- and Z-knots, to provide overall information that is helpful for identifying the celestial coordinates of the brightest stars in the Pleiades cluster. In the present study, the linear regression attempts to model the relationship between two variables (which are determined by the distribution of the S- and Z-knots). The scatter plot illustrates the results of our simple linear regression: suggesting a map of the Pleiades represented by seven points on the Cartesian coordinate plane. Keywords: Inca khipu, Linear regression analysis, Celestial coordinate system, Pleiades. Resumen Una muestra de quipu estudiada por Gary Urton comporta una división por cuadrantes poco común. Utilizando dicho hallazgo de Urton, podemos visualizar la información contenida en los pares de cuadrantes, la cual está determinada por una distribución de nudos con orientaciones opuestas de „S‟ y de „Z‟, brindándonos, así, toda la información necesaria para identificar las coordenadas celestes de las estrellas más brillantes del cúmulo de las Pléyades. En el presente estudio se usa el análisis de la Regresión Lineal con el fin de construir un modelo que permita predecir el comportamiento de la variable dependiente y (valores de los nudos con orientación de „Z‟) en función de la variable independiente x (valores de los nudos con orientación de „S‟). -
Detection and Characterization of Hot Subdwarf Companions of Massive Stars Luqian Wang
Georgia State University ScholarWorks @ Georgia State University Physics and Astronomy Dissertations Department of Physics and Astronomy 8-13-2019 Detection And Characterization Of Hot Subdwarf Companions Of Massive Stars Luqian Wang Follow this and additional works at: https://scholarworks.gsu.edu/phy_astr_diss Recommended Citation Wang, Luqian, "Detection And Characterization Of Hot Subdwarf Companions Of Massive Stars." Dissertation, Georgia State University, 2019. https://scholarworks.gsu.edu/phy_astr_diss/119 This Dissertation is brought to you for free and open access by the Department of Physics and Astronomy at ScholarWorks @ Georgia State University. It has been accepted for inclusion in Physics and Astronomy Dissertations by an authorized administrator of ScholarWorks @ Georgia State University. For more information, please contact [email protected]. DETECTION AND CHARACTERIZATION OF HOT SUBDWARF COMPANIONS OF MASSIVE STARS by LUQIAN WANG Under the Direction of Douglas R. Gies, PhD ABSTRACT Massive stars are born in close binaries, and in the course of their evolution, the initially more massive star will grow and begin to transfer mass and angular momentum to the gainer star. The mass donor star will be stripped of its outer envelope, and it will end up as a faint, hot subdwarf star. Here I present a search for the subdwarf stars in Be binary systems using the International Ultraviolet Explorer. Through spectroscopic analysis, I detected the subdwarf star in HR 2142 and 60 Cyg. Further analysis led to the discovery of an additional 12 Be and subdwarf candidate systems. I also investigated the EL CVn binary system, which is the prototype of class of eclipsing binaries that consist of an A- or F-type main sequence star and a low mass subdwarf. -
Extraterrestrial Places in the Cthulhu Mythos
Extraterrestrial places in the Cthulhu Mythos 1.1 Abbith A planet that revolves around seven stars beyond Xoth. It is inhabited by metallic brains, wise with the ultimate se- crets of the universe. According to Friedrich von Junzt’s Unaussprechlichen Kulten, Nyarlathotep dwells or is im- prisoned on this world (though other legends differ in this regard). 1.2 Aldebaran Aldebaran is the star of the Great Old One Hastur. 1.3 Algol Double star mentioned by H.P. Lovecraft as sidereal The double star Algol. This infrared imagery comes from the place of a demonic shining entity made of light.[1] The CHARA array. same star is also described in other Mythos stories as a planetary system host (See Ymar). The following fictional celestial bodies figure promi- nently in the Cthulhu Mythos stories of H. P. Lovecraft and other writers. Many of these astronomical bodies 1.4 Arcturus have parallels in the real universe, but are often renamed in the mythos and given fictitious characteristics. In ad- Arcturus is the star from which came Zhar and his “twin” dition to the celestial places created by Lovecraft, the Lloigor. Also Nyogtha is related to this star. mythos draws from a number of other sources, includ- ing the works of August Derleth, Ramsey Campbell, Lin Carter, Brian Lumley, and Clark Ashton Smith. 2 B Overview: 2.1 Bel-Yarnak • Name. The name of the celestial body appears first. See Yarnak. • Description. A brief description follows. • References. Lastly, the stories in which the celes- 3 C tial body makes a significant appearance or other- wise receives important mention appear below the description. -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
Angular Momentum Mixing Chemical Mixing Conclusions Content
Be Stars and Rotational Mixing Th. Rivinius, L.R. R´ımulo & A.C. Carciofi With many thanks for discussions to make things clearer to myself to S. Justham, N. Langer, P. Marchant, G. Meynet, F. Schneider European Southern Observatory, Chile IAG, Sao˜ Paulo, Brasil March 21, 2017 Some Be stars. Credit: Robert Gendler via APOD (January 9, 2006) Pleione, Alkyone, Electra, Merope Intro Angular Momentum Mixing Chemical Mixing Conclusions Content 1 Short Introduction to Be Stars 2 Angular Momentum Mixing 3 Chemical Mixing 4 Conclusions Intro Angular Momentum Mixing Chemical Mixing Conclusions Be star classification Definition (Be stars) A non-supergiant B star whose spectrum has, or had at some time, one or more Balmer lines in emission. (Jaschek et al., 1981; Collins, 1987) (Non-sg B star: 3 to 15 solar masses, 10 000 to 28 000 K) Observational corollary (Disk angular momentum) • Disk is rotationally supported (i.e. Keplerian) ¥ Evidence: Spectro-interferometry, spectroscopy of shell stars, time behaviour of perturbed disks Intro Angular Momentum Mixing Chemical Mixing Conclusions Physical properties of classical Be stars Definition (Classical Be stars) • Emission is formed in a disk ¥ Evidence: Interferometry, polarimetry • Disk is created by central star through mass loss ¥ Evidence: Disks come and go in weeks to decades, absence of mass-transferring companion More physical definition, still based on observational properties, but hard to apply. Though necessary to understand physics. Intro Angular Momentum Mixing Chemical Mixing Conclusions Physical properties of classical Be stars Definition (Classical Be stars) • Emission is formed in a disk ¥ Evidence: Interferometry, polarimetry • Disk is created by central star through mass loss ¥ Evidence: Disks come and go in weeks to decades, absence of mass-transferring companion More physical definition, still based on observational properties, but hard to apply. -