A Collection of Curricula for the STARLAB® Maya Skies Cylinder
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The Astronomical Garden of Venus and Mars-NG915: the Pivotal Role Of
The astronomical garden of Venus and Mars - NG915 : the pivotal role of Astronomy in dating and deciphering Botticelli’s masterpiece Mariateresa Crosta Istituto Nazionale di Astrofisica (INAF- OATo), Via Osservatorio 20, Pino Torinese -10025, TO, Italy e-mail: [email protected] Abstract This essay demonstrates the key role of Astronomy in the Botticelli Venus and Mars-NG915 painting, to date only very partially understood. Worthwhile coin- cidences among the principles of the Ficinian philosophy, the historical characters involved and the compositional elements of the painting, show how the astronomi- cal knowledge of that time strongly influenced this masterpiece. First, Astronomy provides its precise dating since the artist used the astronomical ephemerides of his time, albeit preserving a mythological meaning, and a clue for Botticelli’s signature. Second, it allows the correlation among Botticelli’s creative intention, the historical facts and the astronomical phenomena such as the heliacal rising of the planet Venus in conjunction with the Aquarius constellation dating back to the earliest represen- tations of Venus in Mesopotamian culture. This work not only bears a significant value for the history of science and art, but, in the current era of three-dimensional mapping of billion stars about to be delivered by Gaia, states the role of astro- nomical heritage in Western culture. Finally, following the same method, a precise astronomical dating for the famous Primavera painting is suggested. Keywords: History of Astronomy, Science and Philosophy, Renaissance Art, Educa- tion. Introduction Since its acquisition by London’s National Gallery on June 1874, the painting Venus and Mars by Botticelli, cataloged as NG915, has remained a mystery to be interpreted [1]1. -
A Temperate Rocky Super-Earth Transiting a Nearby Cool Star Jason A
LETTER doi:10.1038/nature22055 A temperate rocky super-Earth transiting a nearby cool star Jason A. Dittmann1, Jonathan M. Irwin1, David Charbonneau1, Xavier Bonfils2,3, Nicola Astudillo-Defru4, Raphaëlle D. Haywood1, Zachory K. Berta-Thompson5, Elisabeth R. Newton6, Joseph E. Rodriguez1, Jennifer G. Winters1, Thiam-Guan Tan7, Jose-Manuel Almenara2,3,4, François Bouchy8, Xavier Delfosse2,3, Thierry Forveille2,3, Christophe Lovis4, Felipe Murgas2,3,9, Francesco Pepe4, Nuno C. Santos10,11, Stephane Udry4, Anaël Wünsche2,3, Gilbert A. Esquerdo1, David W. Latham1 & Courtney D. Dressing12 15 16,17 M dwarf stars, which have masses less than 60 per cent that of Ks magnitude and empirically determined stellar relationships , the Sun, make up 75 per cent of the population of the stars in the we estimate the stellar mass to be 14.6% that of the Sun and the stellar Galaxy1. The atmospheres of orbiting Earth-sized planets are radius to be 18.6% that of the Sun. We estimate the metal content of the observationally accessible via transmission spectroscopy when star to be approximately half that of the Sun ([Fe/H] = −0.24 ± 0.10; the planets pass in front of these stars2,3. Statistical results suggest 1σ error), and we measure the rotational period of the star to be that the nearest transiting Earth-sized planet in the liquid-water, 131 days from our long-term photometric monitoring (see Methods). habitable zone of an M dwarf star is probably around 10.5 parsecs On 15 September 2014 ut, MEarth-South identified a potential away4. A temperate planet has been discovered orbiting Proxima transit in progress around LHS 1140, and automatically commenced Centauri, the closest M dwarf5, but it probably does not transit and high-cadence follow-up observations (see Extended Data Fig. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Effemeridi Astronomiche (Di Milano) Dall'ab. A. De Cesaris [And Others]
Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali. -
Milan Dimitrijevic Avgust.Qxd
1. M. Platiša, M. Popović, M. Dimitrijević, N. Konjević: 1975, Z. Fur Natur- forsch. 30a, 212 [A 1].* 1. Griem, H. R.: 1975, Stark Broadening, Adv. Atom. Molec. Phys. 11, 331. 2. Platiša, M., Popović, M. V., Konjević, N.: 1975, Stark broadening of O II and O III lines, Astron. Astrophys. 45, 325. 3. Konjević, N., Wiese, W. L.: 1976, Experimental Stark widths and shifts for non-hydrogenic spectral lines of ionized atoms, J. Phys. Chem. Ref. Data 5, 259. 4. Hey, J. D.: 1977, On the Stark broadening of isolated lines of F (II) and Cl (III) by plasmas, JQSRT 18, 649. 5. Hey, J. D.: 1977, Estimates of Stark broadening of some Ar III and Ar IV lines, JQSRT 17, 729. 6. Hey, J. D.: Breger, P.: 1980, Stark broadening of isolated lines emitted by singly - ionized tin, JQSRT 23, 311. 7. Hey, J. D.: Breger, P.: 1981, Stark broadening of isolated ion lines by plas- mas: Application of theory, in Spectral Line Shapes I, ed. B. Wende, W. de Gruyter, 201. 8. Сыркин, М. И.: 1981, Расчеты электронного уширения спектральных линий в теории оптических свойств плазмы, Опт. Спектроск. 51, 778. 9. Wiese, W. L., Konjević, N.: 1982, Regularities and similarities in plasma broadened spectral line widths (Stark widths), JQSRT 28, 185. 10. Konjević, N., Pittman, T. P.: 1986, Stark broadening of spectral lines of ho- mologous, doubly ionized inert gases, JQSRT 35, 473. 11. Konjević, N., Pittman, T. P.: 1987, Stark broadening of spectral lines of ho- mologous, doubly - ionized inert gases, JQSRT 37, 311. 12. Бабин, С. -
Ioptron CEM40 Center-Balanced Equatorial Mount
iOptron®CEM40 Center-Balanced Equatorial Mount Instruction Manual Product CEM40 (#7400A series) and CEM40EC (#7400ECA series, as shown) Please read the included CEM40 Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper operation will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while using a telescope. 2 Table of Contents Table of Contents ........................................................................................................................................ 3 1. CEM40 Introduction ............................................................................................................................... 5 2. CEM40 Overview ................................................................................................................................... 6 2.1. Parts List ......................................................................................................................................... -
Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis, -
Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗
Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗ Mario Mateo1 e-mail: [email protected] Edward W. Olszewski2 e-mail: [email protected] Heather L. Morrison3 e-mail: [email protected] Received ; accepted ∗BasedonobservationsobtainedwiththeBlancoTelescopeatCTIO,whichisoperated by the National Optical Astronomy Observatory, under contract to AURA. 1Department of Astronomy, University of Michigan, 821 Dennison Bldg., Ann Arbor, MI 48109–1090 2Steward Observatory, 933 N. Cherry, University of Arizona, Tucson, AZ 85721-0065 3Cottrell Scholar of Research Corporation, and NSF Career Fellow; Department of Astronomy and Department of Physics, Case Western Reserve University, Cleveland OH 44106 –2– ABSTRACT We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy, and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main-sequence within the resulting color-magnitude diagrams (CMDs), we unambiguously detect Sgr stars in the southeast over the range 10–34◦ from the galaxy’s center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68◦, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy’s minor-axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V-band surface brightness (SB) profile ranges from 27.3-30.5 mag arcsec−2 over this radial range and exhibits a change in slope ∼ 20◦ from the center of Sgr. -
Planets and Exoplanets
NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable. -
R Aquarii: Evidence for a Two-Sided Radio Jet and a Circumbinary Sio Maser Menas Kafatos Chapman University, [email protected]
Chapman University Chapman University Digital Commons Mathematics, Physics, and Computer Science Science and Technology Faculty Articles and Faculty Articles and Research Research 1989 R Aquarii: Evidence for a Two-Sided Radio Jet and a Circumbinary SiO Maser Menas Kafatos Chapman University, [email protected] J. M. Hollis Blue Bay Res Inc F. Yusef-Zadeh Northwestern University A. G. Michalitsianos NASA, Goddard Space Flight Center M. Elitzur University of Kentucky Follow this and additional works at: http://digitalcommons.chapman.edu/scs_articles Part of the Instrumentation Commons, and the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Kafatos, M., Hollis, J.M., Yusef-Zadeh, F., Michalitsianos, A.G., Elitzur, M. (1989) R Aquarii: Evidence for a Two-Sided radio Jet and a Circumbinary SiO Maser, The Astrophysical Journal, 346:991-996. doi: 10.1086/168081 This Article is brought to you for free and open access by the Science and Technology Faculty Articles and Research at Chapman University Digital Commons. It has been accepted for inclusion in Mathematics, Physics, and Computer Science Faculty Articles and Research by an authorized administrator of Chapman University Digital Commons. For more information, please contact [email protected]. R Aquarii: Evidence for a Two-Sided Radio Jet and a Circumbinary SiO Maser Comments This article was originally published in Astrophysical Journal, volume 346, in 1989. DOI: 10.1086/168081 Copyright IOP Publishing This article is available at Chapman University Digital Commons: http://digitalcommons.chapman.edu/scs_articles/110 THE ASTROPHYSICAL JOURNAL, 346:991-996, 1989 November 15 © 1989. The American Astronomical Society. All rights reserved. Printed in U.S.A. -
December 2019 BRAS Newsletter
A Monthly Meeting December 11th at 7PM at HRPO (Monthly meetings are on 2nd Mondays, Highland Road Park Observatory). Annual Christmas Potluck, and election of officers. What's In This Issue? President’s Message Secretary's Summary Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner – The Green Odyssey Messages from the HRPO Friday Night Lecture Series Science Academy Solar Viewing Stem Expansion Transit of Murcury Edge of Night Natural Sky Conference Observing Notes: Perseus – Rescuer Of Andromeda, or the Hero & Mythology Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 25 December 2019 President’s Message I would like to thank everyone for having me as your president for the last two years . I hope you have enjoyed the past two year as much as I did. We had our first Members Only Observing Night (MOON) at HRPO on Sunday, 29 November,. New officers nominated for next year: Scott Cadwallader for President, Coy Wagoner for Vice- President, Thomas Halligan for Secretary, and Trey Anding for Treasurer. Of course, the nominations are still open. If you wish to be an officer or know of a fellow member who would make a good officer contact John Nagle, Merrill Hess, or Craig Brenden. We will hold our annual Baton Rouge “Gastronomical” Society Christmas holiday feast potluck and officer elections on Monday, December 9th at 7PM at HRPO. I look forward to seeing you all there. ALCon 2022 Bid Preparation and Planning Committee: We’ll meet again on December 14 at 3:00.pm at Coffee Call, 3132 College Dr F, Baton Rouge, LA 70808, UPCOMING BRAS MEETINGS: Light Pollution Committee - HRPO, Wednesday December 4th, 6:15 P.M. -
Observing List
day month year Epoch 2000 local clock time: 4.00 Observing List for 24 7 2019 RA DEC alt az Constellation object mag A mag B Separation description hr min deg min 60 75 Andromeda Gamma Andromedae (*266) 2.3 5.5 9.8 yellow & blue green double star 2 3.9 42 19 73 111 Andromeda Pi Andromedae 4.4 8.6 35.9 bright white & faint blue 0 36.9 33 43 72 71 Andromeda STF 79 (Struve) 6 7 7.8 bluish pair 1 0.1 44 42 58 80 Andromeda 59 Andromedae 6.5 7 16.6 neat pair, both greenish blue 2 10.9 39 2 89 34 Andromeda NGC 7662 (The Blue Snowball) planetary nebula, fairly bright & slightly elongated 23 25.9 42 32.1 75 84 Andromeda M31 (Andromeda Galaxy) large sprial arm galaxy like the Milky Way 0 42.7 41 16 75 85 Andromeda M32 satellite galaxy of Andromeda Galaxy 0 42.7 40 52 75 82 Andromeda M110 (NGC205) satellite galaxy of Andromeda Galaxy 0 40.4 41 41 60 84 Andromeda NGC752 large open cluster of 60 stars 1 57.8 37 41 57 73 Andromeda NGC891 edge on galaxy, needle-like in appearance 2 22.6 42 21 89 173 Andromeda NGC7640 elongated galaxy with mottled halo 23 22.1 40 51 82 10 Andromeda NGC7686 open cluster of 20 stars 23 30.2 49 8 47 200 Aquarius 55 Aquarii, Zeta 4.3 4.5 2.1 close, elegant pair of yellow stars 22 28.8 0 -1 35 181 Aquarius 94 Aquarii 5.3 7.3 12.7 pale rose & emerald 23 19.1 -13 28 30 173 Aquarius 107 Aquarii 5.7 6.7 6.6 yellow-white & bluish-white 23 46 -18 41 26 221 Aquarius M72 globular cluster 20 53.5 -12 32 27 220 Aquarius M73 Y-shaped asterism of 4 stars 20 59 -12 38 40 181 Aquarius NGC7606 Galaxy 23 19.1 -8 29 28 219 Aquarius NGC7009