Boletin Asociacion Argentina Astronomia N°. 36

Total Page:16

File Type:pdf, Size:1020Kb

Boletin Asociacion Argentina Astronomia N°. 36 BOLETIN DE LA ASOCIACION ARGENTINA DE ASTRONOMIA N°. 36 1990 ASOCIACION ARGENTINA DE ASTRONOMIA Personeria Juridica 11.811 Provincia de Buenos Aires PRESIDENTE Dr. Juan J. Claria VICE PRESIDENTE Dr- Hugo Levato SECRETARIO Dr. Emilio Lapasset TESORERO Lic. Raul Perdomo VOCAL PRIMERO Dra. Estela Brandi VOCAL SECUNDO Sr. Juan G. Sanguin VOCAL SUPLENTE Lic. Monica Villada BOLETIN DE LA ASOCIACION ARGENTINA DE ASTRONOMIA N 36 SAN JUAN, 1990. BOLETIN DE LA ASOCIA CION ARGENTINA DE ASTRONOM I A N# 36 Editor Direccion Juan Josd Claria Observatorio Astronomico Laprida 854 - 5000 Cordoba Argentina Telex 51-822 BUCOR, Obs.Astr. Secretaria Editorial Complejo Astronbmico EI Leoncito Silvia Galliani de Santa Fd 198 (0) Pico Casilla de Correo 467 5400 San Juan Argentina Telex 59134 entop-AR Pubiicado con ayuda econbmica dei Consejo Nacional de Investigaciones Cientificas y Tdcnicas (CONICET) de Argentina B O L E T I N DE L A AS OCIACION ARGENTIN A DE A S T RO N O M I A N* 36 REUNION DE LA ASOCIACION ARGENTINA DE ASTRONOMIA REALIZADA EN LA CIUDAD DE SAN JUAN (ARGENTINA) ENTRE EL 18 Y EL 22 DE SETIEMBRE DE 1990 INSTITUCIONES PARTICIPANTES QIC Comisidn de Investigaciones de la Provincia de Buenos Aires CONICET Consejo Nacional de Investigaciones Cientlficas y Tecnologicas CASILEO Complejo Astrondmico EI Leoncito COSICOR CEICYT Centro de Investigaciones Cientificas y Tecnologicas (Mendoza) CIOp Centro de Investigaciones Opticas Departamento de Astronomia, Universidad de Chile Department of Astronomy, University of California, USA Departamento de Fisica, Facultad de Ciencias Exactas, Universidad Nacional de La Piata FCAGLP Facultad de Ciencias Astronomicas y Geofisicas de la Universidad Nacional de La Piata IER3/CB Paris, Francia IAR Instituto Argentino de Radioastronomia IAFE Instituto de Astronomia y Fisica dei Espacio Instituto de Fisica de Rosario Instituto de Biologla Celular, FMC, Universidad Nacional de Cordoba Instituto Ant&rtico Argentino Instituto de Fisica, UFRGS, Porto Alegre Brasil Max-Planck-Institut fur Radioastronomie National Optical Astronomy Observatories Nanjing Astronomical Instrument Research Center, Academia Sinica, Nanjing, China OAFA Observatorio Astronomico "Felix Aguilar" (San Juan) OAC Observatorio Astronomico de Cordoba OAM Observatorio Astronomico de Mercedes, Provincia de Buenos Aires OICT Observatorio Astronomico de Cerro Tololo Chile Observatorio Astrondmico Municipal de Rosario Steward Observatory, University of Arizona, USA Yale Southern Observatory INDICE GENERAL Palabras dei Presidente de la A.A.A. J.J. Claria XVII ESTRUCTURA Y EVOLUCION ESTELAR Ctimulos globulares galicticos con matalicidades extremadamente bajas J.J. Claria; D. Geisler; D. Minniti 3 EI ctimulo abierto NGC 5662 y su Cefeida vecina V Centauri J.J. Claria; E. Lapasset; M.A. Bosio 15 Dimensiones absolutas y estado evolutivo de RS Sagitarii M.A. Cerruti? M.A. De Laurenti 28 EI mdtodo de grilla aplicado al anaiisis fotome- trico de los sistemas de contacto AW Virginis y BP Velorum M. Gomez; E. Lapasset; R. Farinas 38 Hacia la busqueda de una taxonomia de objetos ce- lestes. I. Cumulos abiertos. H.L. Tignanelli; C. Mostaccio; S. Gordillo; A. Plastino; R.A. Vazquez; A. Feinstein 45 Seguimiento espectroscopico de estrellas simbio- ticas australes. R.H. Barbi; E.E. Brandi; O.E. Ferrer; L.G. Garcia 57 Bol. Asoc. Arg. de Astr. I Observaciones en OH de fuentes seleccionadas dei I.R.A.S. desde el hemisferio sur. A.M. Silva; I. Azc&rate; W.G.L. Poppel; L. Likkel 72 ESTRUCTURA GALACTICA Y DINAMICA ESTELAR Informe Invitado: La distancia al centro gal&ctico. V.M. Blanco 87 Expansion dei HI interestelar vinculado a ARA OBI. J.R. Rizzo; E. Bajaja 107 HI en expansibn en la zona de CAR OB2. J.R. Rizzo; E.M. Arnal; E. Bajaja 118 MATERIAL INTERESTELAR Observaciones en el continuo de radio de la nebulosa de Gum. J.C. Testori; F.R. Colomb 133 Halo extendido de HI en NGC 4449. E. Bajaja; W. Huchtmeier; U. Klein 147 GALAXIAS Y COSMOLOGIA Distribucion espacial y formacion de cumulos estelares en la region de la Barra de la Nube Mayor de Magallanes. E. Bica; J.J. Claris; H. Dottori 153 II Bol. Asoc. Arg. de Astr. Sobre el problema de generar puntos al azar en el espacio. D.D. Carplntero 166 Fotometria fotogr&fica digital de NGC 5253. J.L. Sdrsic; C.J. Donzelli 175 Propiedades estadlsticas de las galaxias de bajo brillo superficial. M.C. Martin? E. Bajaja 183 8I8TEMA SOLAR Periodo de rotacion y curva de luz dei aste- roide 423 Diotima. R. Gil Hutton 193 Comparacion de catalogos mediante observacio- nes de asteroides. J •G •, Sanguin; R.L Branham, Jr. 201 Sobre la conceptualizacion dei sistema Tierra- Sol-Luna en ninos de seis a once anos. H. Tignanelli; M. Espindola; F. Suarez; S. Durilen 209 An&lisis de los afelios de 179 cometas de largo periodo considerando el efecto de la marea ver- tical de la galaxia. A. Brunini; D.M. Canosa 225 Bol. Asoc. Arg. de Astr. III ASTROMETRIA Observaciones de radio estrellas y estrellas dei cata­ logo S.A.O. con el Circulo Meridiano Repsold dei Observatorio Astronomico "F£lix Aguilar" de San Juan. R.A. Carestia; W.L. Castro; M. Gallego; C.C. Malla- maci; L.F. Marmolejo; J.L. Navarro; J.A. Perez; J.A. Sedeño. 245 Descripcion analitica dei Cuarto Catalogo dei Circulo Meridiano de San Juan (CMSJ4). C.C. Mallamaci 248 Latitud inedia dei Observatorio Astronomico "Felix Aguilar". Estudio de su variacion. W.T. Manrique; J.F. Baldivieso 264 Variacion de la latitud instantanea, Pilar Astro- labio Danjon dei OAFA. W. Manrique; F. Baldivieso; A. Serafino; E. Actis; E. Alonso; R. Podesta 274 INSTRUMENTAL Y TECNICAS DE REDUCCION Nuevas calibraciones empiricas de abundanda meta- lica para fotometria de Washington de gigantes G y K. D. Geisler; J.J. Claria; D. Minitti 287 Dos nuevos telescopios para Astronomia en China. J . Cheng 301 IV Bol. Asoc. Arg. de Astr. Sisterna de procesamiento de imagenes aplicado a la fotometria superficial de galaxias. M.A. Bosio; C.J. Donzelli 311 Btisqueda de sitio astrondmico en bases anttir- ticas argentinas. J.H. Calderon; P.G. Recabarren; M.J. Lombardo H.A. Ochoa 316 Sistema digitalizador de senales de video. P. Recabarren; J.H. Calderon; G. Giovanola; J. Sanchez; L. Espinosa 326 Elementos de Software para diseno optico. J. Campitelli 334 Nuevo fotopolarimetro automatico para el CASLEO: electronica dei instrumento. E. Martinez; J.L. Aballay; A. Martin; H. Ruartes 343 Automatizacion dei espectrografo Cassegrain dei CASLEO. E. Martinez; J.L. Aballay; A. Martin; H. Ruartes 386 RESUMENES DE TRABAJOS Reduccion digitalizada de interferogramas G. Goldes; G. Carranza 401 Efectos de alineamiento en ctimulos de galaxias H. Muriei; M. Nicotra; D. Garcia Lambas; L. Ruiz 403 Bol. Asoc. Arg. de Astr. V Funcion de correlacion angular cruzada de cumulos de galaxias. D. Garcia Lambas; M. Nicotra 404 Dos nebulosas planetarias en las cercanias dei centro galactico. A. Gutidrrez-Moreno; H. Moreno; G. Cortes 406 Consideraciones flsicas acerca de la region nuclear de NGC 3256. E . L. Aguero; S.L. Lipari 408 cEs la masa de mercurio 1/6000000? R.L. Branham, Jr. 409 Anomalias de abundancias en la estrella CP HD 22920. Z. Lopez Garcia; S.M. Malaroda; M.G. Grosso 411 Formacion de galaxias en modelos disipativos. M.B. Mosconi; D. Garcia Lambas 413 Hidrogeno neutro en direccion a la nebulosa de Gum. G. Dubner; E. Giacani? C. Cappa de Nicolau; E. Reynoso 415 HiUna burbuja de polvo en el cumulo globular NGC 6624? J.C. Forte; S. CeiIone; M. Mendez; I. Vega 418 El proyecto SAC-B: objetivo e instrumentacion H. S. Ghielmetti; A.M. Hernandez; J.M. Gulich 419 VI Bol. Asoc. Arg. de Astr. AnAlisis comparativo de fulguraciones en rayos X A.M. Hern&ndez; M.G. Rovira? C.H. Mandrini; M.E. Machado 421 Evaluacion de los procedimientos de optimiza- ci6n de las soluciones fotometricas en siste- mas de contacto. E. Lapasset; M. Gomez; R. Farinas 423 Busqueda de burbujas de HI alrededor de estre- llase WR: HD 50896. C. Cappa de Nicolau; V.S. Niemela 424 Estudio de la fotosfera de /3 Monocerotis A. C. Maranon Di Leo; A.E. Ringuelet 425 La fase de "onset" en las fulguraciones de dos bandas. M.G. Rovira; C.H. Mandrini; A.M. Hernandez; M.E. Machado 426 Formacion de lineas en atmosferas extendidas en expansion tratadas con geometria esferica. L. S. Cidale; A.E. Ringuelet 427 Modelo de atmosfera extendida para HD 50138. A. Vazquez; A.E. Ringuelet 429 Determinacion de velocidades de rotacion en estrellas B Be: procesos fisicos y metodos. A.R. Diaz; A.E. Ringuelet 430 Simulaciones numericas cosmologicas. M. Abadi; D. Garcia Lambas 433 EI sistema de referencia celeste dei Internatio- Bol. Asoc. Arg. de Astr. VII nal Earth Rotation Service (IERS). E.F. Arias 435 Analisis de coherencia entre ”frames” celestes extragal&cticos elaborados con la tecnica VLBI. E.F. Arias 440 Un nuevo metodo de analisis y reduccidn de ob- servaciones VLBI. E.F. Arias; M.S. De Biasi 446 Hipparcos-VLBI: el camino a un sistema celeste primario ideal. E.F. Arias 449 El espectro de la estrella CP HR 8137. M.G. Grosso; S.M. Malaroda; Z. Lopez Garcia 454 ¿Es HD 37129 una estrella peculiar?. S.M. Malaroda; 0.1. Pintado 455 VIII Bol Asoc. Arg. de Astr. INDEX Palabras dei Presidente de la A.A.A. J.J. Claria XVII STRUCTURE AND 8TELLAR EVOLUTION Galactic globular clusters with extremely low metallicities J.J. ClariA; D. Geisler; D. Minniti 3 The open cluster NGC 5662 and its neighbouring cepheid V Centauri J.J. Claria; E. Lapasset? M.A. Bosio 15 Absolute dimensions and evolutive state of RS Sagitarii M.A. Cerruti? M.A. De Laurenti 28 The grid technique applied to the photometric analysis of contact systems AW Virginis and BP Velorum M.
Recommended publications
  • Stsci Newsletter: 1997 Volume 014 Issue 01
    January 1997 • Volume 14, Number 1 SPACE TELESCOPE SCIENCE INSTITUTE Highlights of this issue: • AURA science and functional awards to Leitherer and Hanisch — pages 1 and 23 • Cycle 7 to be extended — page 5 • Cycle 7 approved Newsletter program listing — pages 7-13 Astronomy with HST Climbing the Starburst Distance Ladder C. Leitherer Massive stars are an important and powerful star formation events in sometimes dominant energy source for galaxies. Even the most luminous star- a galaxy. Their high luminosity, both in forming regions in our Galaxy are tiny light and mechanical energy, makes on a cosmic scale. They are not them detectable up to cosmological dominated by the properties of an distances. Stars ~100 times more entire population but by individual massive than the Sun are one million stars. Therefore stochastic effects times more luminous. Except for stars prevail. Extinction represents a severe of transient brightness, like novae and problem when a reliable census of the supernovae, hot, massive stars are Galactic high-mass star-formation the most luminous stellar objects in history is atempted, especially since the universe. massive stars belong to the extreme Massive stars are, however, Population I, with correspondingly extremely rare: The number of stars small vertical scale heights. Moreover, formed per unit mass interval is the proximity of Galactic regions — roughly proportional to the -2.35 although advantageous for detailed power of mass. We expect to find very studies of individual stars — makes it few massive stars compared to, say, difficult to obtain integrated properties, solar-type stars. This is consistent with such as total emission-line fluxes of observations in our solar neighbor- the ionized gas.
    [Show full text]
  • Arxiv:1809.07342V1 [Astro-Ph.SR] 19 Sep 2018
    Draft version September 21, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 FAR-ULTRAVIOLET ACTIVITY LEVELS OF F, G, K, AND M DWARF EXOPLANET HOST STARS* Kevin France1, Nicole Arulanantham1, Luca Fossati2, Antonino F. Lanza3, R. O. Parke Loyd4, Seth Redfield5, P. Christian Schneider6 Draft version September 21, 2018 ABSTRACT We present a survey of far-ultraviolet (FUV; 1150 { 1450 A)˚ emission line spectra from 71 planet- hosting and 33 non-planet-hosting F, G, K, and M dwarfs with the goals of characterizing their range of FUV activity levels, calibrating the FUV activity level to the 90 { 360 A˚ extreme-ultraviolet (EUV) stellar flux, and investigating the potential for FUV emission lines to probe star-planet interactions (SPIs). We build this emission line sample from a combination of new and archival observations with the Hubble Space Telescope-COS and -STIS instruments, targeting the chromospheric and transition region emission lines of Si III,N V,C II, and Si IV. We find that the exoplanet host stars, on average, display factors of 5 { 10 lower UV activity levels compared with the non-planet hosting sample; this is explained by a combination of observational and astrophysical biases in the selection of stars for radial-velocity planet searches. We demonstrate that UV activity-rotation relation in the full F { M star sample is characterized by a power-law decline (with index α ≈ −1.1), starting at rotation periods & 3.5 days. Using N V or Si IV spectra and a knowledge of the star's bolometric flux, we present a new analytic relationship to estimate the intrinsic stellar EUV irradiance in the 90 { 360 A˚ band with an accuracy of roughly a factor of ≈ 2.
    [Show full text]
  • 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.
    [Show full text]
  • The NICMOS Snapshot Survey of Nearby Galaxies
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The NICMOS snapshot survey of nearby galaxies T. B¨oker1, D. Calzetti, W. Sparks, D. Axon1, L. E. Bergeron, H. Bushouse, L. Colina1, D. Daou, D. Gilmore, S. Holfeltz, J. MacKenty, L. Mazzuca, B. Monroe, J. Najita, K. Noll, A. Nota1,C. Ritchie, A. Schultz, M. Sosey, A. Storrs, A. Suchkov (the STScI NICMOS group) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. ABSTRACT We present “snapshot” observations with the NearInfrared Camera and MultiObject Spectrometer (NICMOS) on board the Hubble Space Telescope (HST) of 94 nearby galaxies from the Revised Shapley Ames Catalog. Images with 0.200 resolution were obtained in two filters, a broad-band continuum filter (F160W, roughly equivalent to the H-band) and a narrow band filter centered on the Pa α line (F187N or F190N, depending on the galaxy redshift) with the 5100 5100 field of view of the NICMOS camera 3. A first- order continuum subtraction is performed,× and the resulting line maps and integrated Pa α line fluxes are presented. A statistical analysis indicates that the average Pa α surface brightness in the central regions is highest in early-type (Sa-Sb) spirals. Subject headings: infrared:galaxies—infrared:ISM:lines and bands—galaxies:nuclei— galaxies:starburst—galaxies:statistics 1Affiliated with the Astrophysics Division, Space Science Department, European Space Agency 1 1. Introduction with the NIC3 F190N filter. The velocity range was chosen such that the Pa α line falls well inside the NICMOS is a second generation HST instrument, high transmission region of the respective filter, with installed during the HST servicing mission in Febru- only minor corrections ( 5%) needed to account for ary 1997.
    [Show full text]
  • Appendix A: Scientific Notation
    Appendix A: Scientific Notation Since in astronomy we often have to deal with large numbers, writing a lot of zeros is not only cumbersome, but also inefficient and difficult to count. Scientists use the system of scientific notation, where the number of zeros is short handed to a superscript. For example, 10 has one zero and is written as 101 in scientific notation. Similarly, 100 is 102, 100 is 103. So we have: 103 equals a thousand, 106 equals a million, 109 is called a billion (U.S. usage), and 1012 a trillion. Now the U.S. federal government budget is in the trillions of dollars, ordinary people really cannot grasp the magnitude of the number. In the metric system, the prefix kilo- stands for 1,000, e.g., a kilogram. For a million, the prefix mega- is used, e.g. megaton (1,000,000 or 106 ton). A billion hertz (a unit of frequency) is gigahertz, although I have not heard of the use of a giga-meter. More rarely still is the use of tera (1012). For small numbers, the practice is similar. 0.1 is 10À1, 0.01 is 10À2, and 0.001 is 10À3. The prefix of milli- refers to 10À3, e.g. as in millimeter, whereas a micro- second is 10À6 ¼ 0.000001 s. It is now trendy to talk about nano-technology, which refers to solid-state device with sizes on the scale of 10À9 m, or about 10 times the size of an atom. With this kind of shorthand convenience, one can really go overboard.
    [Show full text]
  • GU Monocerotis: a High-Mass Eclipsing Overcontact Binary in the Young Open Cluster Dolidze 25? J
    A&A 590, A45 (2016) Astronomy DOI: 10.1051/0004-6361/201628224 & c ESO 2016 Astrophysics GU Monocerotis: A high-mass eclipsing overcontact binary in the young open cluster Dolidze 25? J. Lorenzo1, I. Negueruela1, F. Vilardell2, S. Simón-Díaz3; 4, P. Pastor5, and M. Méndez Majuelos6 1 Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Escuela Politécnica Superior, Universidad de Alicante, Carretera de San Vicente del Raspeig s/n, 03690 San Vicente del Raspeig, Alicante, Spain e-mail: [email protected] 2 Institut d’Estudis Espacials de Catalunya, Edifici Nexus, c/ Capitá, 2−4, desp. 201, 08034 Barcelona, Spain 3 Instituto de Astrofísica de Canarias, Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, Facultad de Física y Matemáticas, Avda. Astrofísico Francisco Sánchez s/n, 38205 La Laguna, Tenerife, Spain 5 Departamento de Lenguajes y Sistemas Informáticos, Universidad de Alicante, Apdo. 99, 03080 Alicante, Spain 6 Departamento de Ciencias, IES Arroyo Hondo, c/ Maestro Manuel Casal 2, 11520 Rota, Cádiz, Spain Received 30 January 2016 / Accepted 3 March 2016 ABSTRACT Context. The eclipsing binary GU Mon is located in the star-forming cluster Dolidze 25, which has the lowest metallicity measured in a Milky Way young cluster. Aims. GU Mon has been identified as a short-period eclipsing binary with two early B-type components. We set out to derive its orbital and stellar parameters. Methods. We present a comprehensive analysis, including B and V light curves and 11 high-resolution spectra, to verify the orbital period and determine parameters.
    [Show full text]
  • A New Form of Estimating Stellar Parameters Using an Optimization Approach
    A&A 532, A20 (2011) Astronomy DOI: 10.1051/0004-6361/200811182 & c ESO 2011 Astrophysics Modeling nearby FGK Population I stars: A new form of estimating stellar parameters using an optimization approach J. M. Fernandes1,A.I.F.Vaz2, and L. N. Vicente3 1 CFC, Department of Mathematics and Astronomical Observatory, University of Coimbra, Portugal e-mail: [email protected] 2 Department of Production and Systems, University of Minho, Portugal e-mail: [email protected] 3 CMUC, Department of Mathematics, University of Coimbra, Portugal e-mail: [email protected] Received 17 October 2008 / Accepted 27 May 2011 ABSTRACT Context. Modeling a single star with theoretical stellar evolutionary tracks is a nontrivial problem because of a large number of unknowns compared to the number of observations. A current way of estimating stellar age and mass consists of using interpolations in grids of stellar models and/or isochrones, assuming ad hoc values for the mixing length parameter and the metal-to-helium enrichment, which is normally scaled to the solar values. Aims. We present a new method to model the FGK main-sequence of Population I stars. This method is capable of simultaneously estimating a set of stellar parameters, namely the mass, the age, the helium and metal abundances, the mixing length parameter, and the overshooting. Methods. The proposed method is based on the application of a global optimization algorithm (PSwarm) to solve an optimization problem that in turn consists of finding the values of the stellar parameters that lead to the best possible fit of the given observations.
    [Show full text]
  • MAS Mentoring Project Overview 2020
    Macarthur Astronomical Society Student Projects in Astronomy A Guide of Teachers and Mentors 2020 (c) Macarthur Astronomical Society, 2020 DRAFT The following Project Overviews are based on those suggested by Dr Rahmi Jackson of Broughton Anglican College. The Focus Questions and Issues section should be used by teachers and mentors to guide students in formulating their own questions about the topic. References to the NSW 7-10 Science Syllabus have been included. Note that only those sections relevant are included. For example, subsections a and d may be used, but subsections b and c are omitted as they do not relate to this topic. A generic risk assessment is provided, but schools should ensure that it aligns with school- based policies. MAS Student Projects in Astronomy page 1 Project overviews Semester 1, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter X X X Moderate to high (extension) NOT available Semester 1 2 Astrophotography X X X Moderate to high 3 Light pollution X X Moderate 4 Variable stars X X Moderate to high 5 Spectroscopy X X High 6 A changing lunarscape X X Low to moderate Recommended project 7 Magnitude of stars X X Moderate to high Recommended for technically able students 8 A survey of southern skies X X Low to moderate 9 Double Stars X X Moderate to high 10 The Phases of the Moon X X Low to moderate Recommended project 11 Observing the Sun X X Moderate MAS Student Projects in Astronomy page 2 Project overviews Semester 2, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter
    [Show full text]
  • The Chemical Composition of Solar-Type Stars and Its Impact on the Presence of Planets
    The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Munchen¨ 2013 The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Dissertation der Fakultat¨ fur¨ Physik der Ludwig-Maximilians-Universitat¨ Munchen¨ durchgefuhrt¨ am Max-Planck-Institut fur¨ Astrophysik vorgelegt von Patrick Baumann aus Munchen¨ Munchen,¨ den 31. Januar 2013 Erstgutacher: Prof. Dr. Achim Weiss Zweitgutachter: Prof. Dr. Joachim Puls Tag der mündlichen Prüfung: 8. April 2013 Zusammenfassung Wir untersuchen eine mogliche¨ Verbindung zwischen den relativen Elementhaufig-¨ keiten in Sternatmospharen¨ und der Anwesenheit von Planeten um den jeweili- gen Stern. Um zuverlassige¨ Ergebnisse zu erhalten, untersuchen wir ausschließlich sonnenahnliche¨ Sterne und fuhren¨ unsere spektroskopischen Analysen zur Bestim- mung der grundlegenden Parameter und der chemischen Zusammensetzung streng differenziell und relativ zu den solaren Werten durch. Insgesamt untersuchen wir 200 Sterne unter Zuhilfenahme von Spektren mit herausragender Qualitat,¨ die an den modernsten Teleskopen gewonnen wurden, die uns zur Verfugung¨ stehen. Mithilfe der Daten fur¨ 117 sonnenahnliche¨ Sterne untersuchen wir eine mogliche¨ Verbindung zwischen der Oberflachenh¨ aufigkeit¨ von Lithium in einem Stern, seinem Alter und der Wahrscheinlichkeit, dass sich ein oder mehrere Sterne in einer Um- laufbahn um das Objekt befinden. Fur¨ jeden Stern erhalten wir sehr exakte grundle- gende Parameter unter Benutzung einer sorgfaltig¨ zusammengestellten Liste von Fe i- und Fe ii-absorptionslinien, modernen Modellatmospharen¨ und Routinen zum Erstellen von Modellspektren. Die Massen und das Alter der Objekte werden mithilfe von Isochronen bestimmt, was zu sehr soliden relativen Werten fuhrt.¨ Bei jungen Sternen, fur¨ die die Isochronenmethode recht unzuverlssig¨ ist, vergleichen wir verschiedene alternative Methoden.
    [Show full text]
  • ¼¼Çwªâðw¦¹Á¼ºëw£Àêëw ˆ†ˆ€ «ÆÊ¿Àäàww«¸ÂÀ ‰‡‡Œ†ˆ‰†‰Œ
    ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. P.A. w R.A. Size Size Chart N a he ss d l Object Type Con. Mag. Class t NGC Description l AS o o sc e s r ( h m ) max min No. C a ( ' ) ( ) sc R AAS e r e M C T e B H H NGC 7192 GALXY IND 22 06.8 -64 19 11.2 1.9 m 1.8 m Elliptical pB,S,R,pmbM 134 NGC 7219 GALXY TUC 22 13.1 -64 51 12.5 1.7 m 1 m 27 SBa pB,S,R,2st nr 134 NGC 7329 GALXY TUC 22 40.4 -66 29 11.3 3.7 m 2.7 m 107 SBbc Ring pB,pS,mE90 134 NGC 7417 GALXY TUC 22 57.8 -65 02 12.3 1.9 m 1.3 m 2 SBab Ring pB,cS,R,gpmbM 134 NGC 7637 GALXY OCT 23 26.5 -81 55 12.5 2.1 m 1.9 m Sc vF,pL,R,vlbM,* nr 134 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. P.A. w R.A. Size Size Chart N a he ss d l Object Type Con. Mag. Class t NGC Description l AS o o sc e s r ( h m ) max min No. C a ( ' ) ( ) sc R AAS e r e M C T e B H H Mel 227 OPNCL OCT 20 12.1 -79 19 5.3 50.0 m II 2 p 135 NGC 6872 GALXY PAV 20 17.0 -70 46 11.8 6.3 m 2.2 m 66 SBb/P F,pS,lE,glbM,1st of 4 135 NGC 6876 GALXY PAV 20 18.3 -70 52 11.1 3 m 2.6 m 80 E3 pB,S,R,eS* sf,2nd of 4 135 NGC 6877 GALXY PAV 20 18.6 -70 51 12.2 2 m 1 m 169 E6 vF,vS,R,3rd of 4 135 NGC 6880 GALXY PAV 20 19.5 -70 52 12.2 2.1 m 1.3 m 35 SBO-a F,S,R,r,vS* att,4 of 4 135 NGC 6920 GALXY OCT 20 44.0 -80 00 12.5 1.8 m 1.5 m SO pB,cS,R,psmbM 135 NGC 6943 GALXY PAV 20 44.6 -68 45 11.4 4 m 2.2 m 130 SBc pF,L,mE,vglbM vS* 135 IC 5052 GALXY PAV 20 52.1 -69 12 11.2 5.9 m 0.9 m 143 SBcd F,L,eE 140 deg 135 NGC 7020 GALXY PAV 21 11.3 -64 02 11.8 3.5 m 1.6 m 165 SBO-a Ring pB,cS,lE,pgbM 135 NGC 7083 GALXY IND 21 35.7 -63 54 11.2 3.6 m 2.1 m 5 Sbc pF,cL,vlE,vgpmbM,r 135 NGC 7096 GALXY IND 21 41.3 -63 55 11.9 1.8 m 1.6 m 130 Sa vF,S,R,vS** nf 135 NGC 7098 GALXY OCT 21 44.3 -75 07 11.3 4 m 2.6 m 74 SB Ring pF,R,g,psmbM,am st 135 NGC 7095 GALXY OCT 21 52.4 -81 32 11.5 4 m 3.3 m Sc F,pL,R,vglbM,*13 inv 135 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec.
    [Show full text]
  • Arxiv:0908.2624V1 [Astro-Ph.SR] 18 Aug 2009
    Astronomy & Astrophysics Review manuscript No. (will be inserted by the editor) Accurate masses and radii of normal stars: Modern results and applications G. Torres · J. Andersen · A. Gim´enez Received: date / Accepted: date Abstract This paper presents and discusses a critical compilation of accurate, fun- damental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and α Centauri) that satisfy our criterion that the mass and radius of both stars be known to ±3% or better. All are non-interacting systems, so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with un- precedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay be- tween convection, diffusion, and other non-classical effects in stellar models.
    [Show full text]
  • FY13 High-Level Deliverables
    National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................
    [Show full text]