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A&A 583, A85 (2015) Astronomy DOI: 10.1051/0004-6361/201526795 & c ESO 2015 Astrophysics Reaching the boundary between stellar kinematic groups and very wide binaries III. Sixteen new stars and eight new wide systems in the β Pictoris moving group F. J. Alonso-Floriano1, J. A. Caballero2, M. Cortés-Contreras1,E.Solano2,3, and D. Montes1 1 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain 3 Spanish Virtual Observatory, ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain Received 19 June 2015 / Accepted 8 August 2015 ABSTRACT Aims. We look for common proper motion companions to stars of the nearby young β Pictoris moving group. Methods. First, we compiled a list of 185 β Pictoris members and candidate members from 35 representative works. Next, we used the Aladin and STILTS virtual observatory tools and the PPMXL proper motion and Washington Double Star catalogues to look for companion candidates. The resulting potential companions were subjects of a dedicated astro-photometric follow-up using public data from all-sky surveys. After discarding 67 sources by proper motion and 31 by colour-magnitude diagrams, we obtained a final list of 36 common proper motion systems. The binding energy of two of them is perhaps too small to be considered physically bound. Results. Of the 36 pairs and multiple systems, eight are new, 16 have only one stellar component previously classified as a β Pictoris member, and three have secondaries at or below the hydrogen-burning limit. -
Synthetic Properties of Bright Metal-Poor Variables II
A&A 471, 893–900 (2007) Astronomy DOI: 10.1051/0004-6361:20066541 & c ESO 2007 Astrophysics Synthetic properties of bright metal-poor variables II. BL Hercules stars M. Di Criscienzo1,2,F.Caputo3, M. Marconi1, and S. Cassisi4 1 INAF – Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy e-mail: [email protected] 2 Università degli Studi di Roma “Tor Vergata”, via della Ricerca Scientifica 1, 00133 Roma, Italy 3 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Italy 4 INAF – Osservatorio Astronomico di Collurania, via Maggini, 64100 Teramo, Italy Received 11 October 2006 / Accepted 16 May 2007 ABSTRACT We investigate the properties of the so-called BL Her stars, i.e., Population II Cepheids with periods shorter than 8 days, using updated pulsation models and evolutionary tracks computed by adopting a metal abundance in the range of Z = 0.0001 to Z = 0.004. We derive the predicted period-magnitude (PM) and period-Wesenheit (PW) relations at the various photometric bands and we show that the slopes of these relations are in good agreement with the slopes determined by observed variables in Galactic globular clusters, independently of the adopted MV (RR)−[Fe/H] relation to get the cluster RR Lyrae-based distance. Moreover, we show that the distances provided by the predicted PM and PW relations for BL Her stars agree within the errors with the RR Lyrae-based values. Using the predicted relations with W Vir stars, which are Population II Cepheids with periods longer than 8 days, provides no clear evidence for or against a change in the PM and PW slopes around P ∼ 10 days. -
The Rossiter–Mclaughlin Effect in Exoplanet Research
The Rossiter–McLaughlin effect in Exoplanet Research Amaury H.M.J. Triaud Abstract The Rossiter–McLaughlin effect occurs during a planet’s transit. It pro- vides the main means of measuring the sky-projected spin–orbit angle between a planet’s orbital plane, and its host star’s equatorial plane. Observing the Rossiter– McLaughlin effect is now a near routine procedure. It is an important element in the orbital characterisation of transiting exoplanets. Measurements of the spin–orbit an- gle have revealed a surprising diversity, far from the placid, Kantian and Laplacian ideals, whereby planets form, and remain, on orbital planes coincident with their star’s equator. This chapter will review a short history of the Rossiter–McLaughlin effect, how it is modelled, and will summarise the current state of the field before de- scribing other uses for a spectroscopic transit, and alternative methods of measuring the spin–orbit angle. Introduction The Rossiter–McLaughlin effect is the detection of a planetary transit using spec- troscopy. It appears as an anomalous radial-velocity variation happening over the Doppler reflex motion that an orbiting planet imparts on its rotating host star (Fig.1). The shape of the Rossiter–McLaughlin effect contains information about the ratio of the sizes between the planet and its host star, the rotational speed of the star, the impact parameter and the angle l (historically called b, where b = −l), which is the sky-projected spin–orbit angle. The Rossiter–McLaughlin effect was first reported for an exoplanet, in the case of HD 209458 b, by Queloz et al.(2000). -
Extrasolar Planets and Their Host Stars
Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it. -
Wolf-Rayet Stars
NAT-L INST OF STANDARDS & TECH R.I.C. A11101110167 Symposium on Wolf-Ra/Wolf-Ravet -star*- n QC100 .U57 V307;1968 C^°NBi%^^!'^^i^.o Sjy ( : \ F.cr^i' 8ii|: llie IJuited Slates DepsFlmesit of Ccmiioj^v UNITED STATES DEPARTMENT OF COMMERCE • C. R. Smith, Secretary NATIONAL BUREAU OF STANDARDS • A. V. Astin, Director Wolf-Rayet Stars Proceedings of a Symposium held at The Joint Institute for Laboratory Astrophysics University of Colorado Boulder, Colorado, June 10-14, 1968 Edited by Katharine B. Gebbie and Richard N. Thomas JILA Institute for Basic Standards National Bureau of Standards Boulder, Colorado 80302 Held under the joint sponsorship of The American Astronomical Society, Harvard College Observatory The Joint Institute for Laboratory Astrophysics Smithsonian Astrophysical Observatory Partially Supported by the National Science Foundation , \) National Bureau of Standards Special Publication 307 , » » »- Issued December 1968 For sale by the Superintendent of Documents, U.S. Government printing Office Washington, D.C. 20402 - Price $3 National Bureau ef Standards JAN 1 4 1369 142810 at 100 ABSTRACT A symposium on Wolf-Rayet stars was held at the Joint Institute for Laboratory Astrophysics on the campus of the University of Colorado, Boulder, Colorado, 10-14 June 1968. The Wolf-Rayet stars represent the most extreme example studied of an interaction between aerodynamic motions and a radia- tion field to produce a high temperature, large- scale plasma in a steady but non-equilibrium state. As such these stars provide a perfect example of the kind of gaseous ensemble that JILA was created to study. In order to understand them, we require a knowledge of gases with temperatures between 10** and 10 °K and differential velocities between 0 and 10^ km/sec. -
Observatorio Astronómico "Félix Aguilar" Facultad De Ciencias Exactas, Físicas Y Naturales - Universidad Nacional De San Juan
Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales San Juan ANUARIO ASTRONÓMICO 2011 Volumen XXI 2 Anuario Astronómico 2011 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan UNIVERSIDAD NACIONAL DE SAN JUAN FACULTAD DE CIENCIAS EXACTAS, FÍSICAS Y NATURALES OBSERVATORIO ASTRONÓMICO “FELIX AGUILAR” ANUARIO ASTRONÓMICO 2011 Claudio Carlos Mallamaci - José Alberto Pérez San Juan - República Argentina - 2011 4 Anuario Astronómico 2011 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan Contenido Introducción 7 Fenómenos 9 Sol 11 Fases de la Luna 11 Eclipses y Tránsitos 11 Artículos del calendario 12 Entrada del Sol en los signos del Zodíaco 12 Reporte de las estaciones 12 Perigeo y apogeo de la Luna 12 Fenómenos planetarios geo y heliocéntricos 13 (Mercurio, Venus y planetas superiores) Datos de Planetas 13 Configuración diaria del Sol, Luna y Planetas 14 Sol 19 Luna 27 Tiempo sidéreo y coordenadas del Sol 35 Planetas 43 Posiciones aparentes de estrellas 53 Tablas 95 Refracción Astronómica Normal 95 Correcciones a las Refracciones Normales 96 Calendario 97 5 Anuario Astronómico 2011 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan 6 Anuario Astronómico 2011 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan Introducción Este anuario astronómico, preparado y publicado por el Observatorio Astronómico "Félix Aguilar", tiene como objeto principal proporcionar, a docentes y aficionados en general, datos útiles sobre temas astronómicos. -
Audre Lorde Collection 1950-2002 Spelman College Archives
Audre Lorde Collection 1950-2002 Spelman College Archives Provenance The Audre Lorde Papers were donated to Spelman College in Lorde‘s will and received by the institution in 1995. Preferred Citation Published citations should take the following form: Identification of item, date (if known); Audre Lorde Papers; box number; folder number; Spelman College Archives. Restrictions Access Restrictions Open to researchers. Appointments are necessary for use of manuscript and archival materials. Use Restrictions Collection use is subject to all copyright laws. Permission to publish materials must be obtained in writing from the Director of Spelman College Archives. For more information, contact Descriptive Summary Creator Taronda Spencer, Brenda S. Banks and Kerrie Cotten Williams Title The Audre Lorde Papers Dates ca. 1950-2002 Quantity 40 linear ft. Biographical Note Poet, writer. Born Audre Geraldine Lorde on February 18, 1934, in New York, New York. Raised in New York, Lorde attended Hunter College. After graduating in 1959, she went on to get a master‘s degree in library science from Columbia University in 1961. Audre Lorde worked as a librarian in Mount Vernon, New York, and in New York City. She married attorney Edwin Rollins in 1962, and the couple had two children—Elizabeth and Jonathan. The couple later divorced. Lorde‘s professional career as a writer began in earnest in 1968 with the publication of her first volume of poetry, First Cities, was published in 1968. A second volume, Cables to Rage in 1970 was completed while Lorde was writer-in-residence at Tougaloo College in Mississippi. Lorde‘s third volume of poetry, From a Land Where Other People Live, written in 1973 was nominated for a National Book Award. -
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Baltic Astronomy, vol. 6, 499-572, 1997. CLASSIFICATION OF POPULATION II STARS IN THE VILNIUS PHOTOMETRIC SYSTEM. II. RESULTS A. Bartkevicius1 and R. Lazauskaite1 '2 1 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 2 Department of Theoretical Physics, Vilnius Pedagogical University, Studenty. 39, Vilnius 2340, Lithuania Received April 20, 1997. Abstract. The results of photometric classification of 848 true and suspected Population II stars, some of which were found to be- long to Population I, are presented. The stars were classified using a new calibration described in Paper I (Bartkevicius & Lazauskaite 1996). We combine these results with our results from Paper I and discuss in greater detail the following groups of stars: UU Herculis-type stars and other high-galactic-latitude supergiants, field red horizontal-branch stars, metal-deficient visual binaries, metal- deficient subgiants, stars from the Catalogue of Metal-deficient F-M Stars Classified Photometrically (MDPH; Bartkevicius 1993) and stars from one of the HIPPARCOS programs (Bartkevicius 1994a). It is confirmed that high galactic latitude supergiants from the Bartaya (1979) catalog are giants or even dwarfs. Some stars, identified by Rose (1985) and Tautvaisiene (1996a) as field RHB stars, appear to be ordinary giants according to our classification. Some of the visual binaries studied can be considered as physical pairs. Quite a large fraction of stars from the MDPH catalog are found to have solar metallicity. A number of new possible UU Herculis-type stars, RHB stars and metal-deficient subgiants are identified. Key words: techniques: photometric - stars: fundamental para- meters (classification) - stars: Population II 500 A. -
Observatorio Astronómico "Félix Aguilar"
Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales San Juan ANUARIO ASTRONÓMICO 2020 Volumen XXX 2 Anuario Astronómico 2020 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan UNIVERSIDAD NACIONAL DE SAN JUAN FACULTAD DE CIENCIAS EXACTAS, FÍSICAS Y NATURALES OBSERVATORIO ASTRONÓMICO “FELIX AGUILAR” ANUARIO ASTRONÓMICO 2020 Claudio Carlos Mallamaci - José Alberto Pérez San Juan - República Argentina - 2020 4 Anuario Astronómico 2020 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan Contenido Introducción 7 Fenómenos 9 Sol 11 Fases de la Luna 11 Eclipses y Tránsitos 11 Artículos del calendario 12 Entrada del Sol en los signos del Zodíaco 12 Reporte de las estaciones 12 Perigeo y apogeo de la Luna 12 Fenómenos planetarios geo y heliocéntricos 13 (Mercurio, Venus y planetas superiores) Datos de Planetas 13 Configuración diaria del Sol, Luna y Planetas 14 Sol 19 Luna 27 Tiempo sidéreo y coordenadas del Sol 35 Planetas 43 Posiciones aparentes de estrellas 53 Tablas 95 Refracción Astronómica Normal 95 Correcciones a las Refracciones Normales 96 Calendario 97 5 Anuario Astronómico 2020 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan 6 Anuario Astronómico 2020 – C.C. Mallamaci - J.A.Pérez - Observatorio Astronómico "Félix Aguilar" Facultad de Ciencias Exactas, Físicas y Naturales - Universidad Nacional de San Juan Introducción Este anuario astronómico, preparado y publicado por el Observatorio Astronómico "Félix Aguilar", tiene como objeto principal proporcionar, a docentes y aficionados en general, datos útiles sobre temas astronómicos. -
Astronomy Magazine Subject Index (1973–2000)
Astronomy magazine subject index (1973–2000) # 11/97:48–49 100-inch Hooker Telescope, 9/81:58–59 55 Canri (star), 2/99:24 11999UX 18 (17th moon of Jupiter), 10/00:32, 624 Hektor (asteroid), 5/80:61–62 8/79:62 1208+1001 (quasar), 11/86:81–82 A 128 Nemesis (asteroid), 8/79:62 A0620-00 (binary star), 2/91:24 1937+214 (pulsar), 11/83:60 as candidate for black hole, 3/92:30–37, 7/92:22 1957D (supernova), 4/89:14 general discussion, 2/91:22 1984QA (asteroid), 2/85:62, 64 AAT (Anglo-Australian Telescope), 2/77:57, 1986 DA (asteroid), 10/91:26 5/78:60–62 1986 TO (asteroid), 3/98:30 Abell 2218 (luminous arc), 4/87:77 1987A (supernova) Abell 370 (luminous arc), 4/87:77 companion to, 9/87:74–75 Abell (galaxy cluster), 5/95:30 explosion of, 7/87:68–69, 7/88:10 AC 114 (galaxy cluster), 7/92:20, 22, 1/93:22 gamma ray bursts from, 4/88:74 Acton, Dr. Loren, 10/86:28, 30 observing, 6/87:90–95 Adams ring, 1/00:34, 36 remnant of, 9/87:75 adaptive optics, 3/90:10, 12, 9/91:22, 1/98:37–41 rings of light encircling, 11/88:12, 14 Adler Planetarium (Chicago), 6/91:28 1988 A (supernova), 8/88:88 20-inch telescope introduced, 8/87:64–65 1988 U (supernova), 12/89:12 art exhibit, 9/96:28 1989 FC (asteroid), 8/89:10 Advanced X-ray Astrophysics Facility (AXAF), 1989 PB (asteroid), 4/90:38–40 12/88:14, 8/92:21 1990 MF (asteroid), 11/90:24 AE-5 (Explorer-5 satellite), 9/81:59–60 1990 (year), length of, 12/90:24 Africa, skylore of, 1/79:61 1992 AD (asteroid), 6/92:22, 24 AIC Miranda Laborec Astrocamera, 10/75:28–37 1992 (year), length of, 6/92:24, 26 airplanes, observation -
Constellations by Season
Observer Constellations 1 Volume 8 Issue 6 April 2019 Hidden Gems of the Night sky Learn how to spot any constellation with the naked eye and find what’s written in the stars... Long before the creation of the modern-day calendar, humans used constellations to remember the stars’ positions as a way to tell time recognizing that certain constellations appeared during different times of the year. Farmers, especially, found these patterns useful because they knew when to harvest crops and when to plant them based on which constellations they saw for that season. Navigators, on the other hand, could always figure their latitude just by looking at how high the North Star, Polaris, appeared in the sky. While remembering constellations had its practical uses, people from all cultures enjoyed observing constellations and naming them based on mythological deities, animals, and objects. From there on, they would use constellations to tell stories about them with each culture offering a unique interpretation for each constellation. Today, astronomers have used constellations to divide the night sky which allows them to classify each star according to the constellation it belongs to. As you can see, people don’t need equipment to see constellations when in fact, they can stargaze just like their ancestors, and it’s not that difficult to get started. With that said, here is a comprehensive beginner’s guide on stargazing and navigating the night sky for constellations. By Abigail Tarun Design Manager Image from Pinterest by Anime Candy Continued… 2 of 11 All Background Images from Pinterest Observer Constellations 2 Volume 8 Issue 6 April 2019 Constellations by Before you go on a stargazing adventure, it’s crucial that you Season know when the stars are most visible at night. -
HARLOW SHAPLEY November 2,1885-October 20,1972
NATIONAL ACADEMY OF SCIENCES H ARLO W S HAPLEY 1885—1972 A Biographical Memoir by BART J. BOK Any opinions expressed in this memoir are those of the author(s) and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 1978 NATIONAL ACADEMY OF SCIENCES WASHINGTON D.C. HARLOW SHAPLEY November 2,1885-October 20,1972 BY BART J. BOK ARLOW SHAPLEY was born November 2, 1885, on a farm H five miles from Nashville, Missouri. He was one of fra- ternal twins. Besides his twin, Horace, he had one older sister, Lillian, and a younger brother, John. He went to school in Jasper, Missouri, but he did not go at first beyond elementary school; he and his brother John had a brief period in a normal school, where they were only permitted to take a business course. At the time when most boys would go to high school, Harlow studied by himself at home. He had one year of early schooling in Hampton, New York, where he went on a family visit. At the age of fifteen he became a crime reporter for the Daily Sun in Chanute, Kansas, and he also worked off and on as a police reporter for the Joplin (Missouri) Times. He learned to take notes in shorthand, which, in later life, became a -medium of communication between him and his wife. In Chanute he found a Carnegie library, and there he really started reading and studying on his own. When funds became available, he and his younger brother, John, decided to go to Carthage High School, a prestigious school located in the nearest city to Nash- ville, Missouri.