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Université De Montréal Relevé Polarimétrique D'étoiles Candidates
Université de Montréal Relevé polarimétrique d’étoiles candidates pour des disques de débris par Amélie Simon Département de physique Faculté des arts et des sciences Mémoire présenté à la Faculté des études supérieures en vue de l’obtention du grade de Maître ès sciences (M.Sc.) en physique Août, 2010 c Amélie Simon, 2010 Université de Montréal Faculté des études supérieures Ce mémoire intitulé: Relevé polarimétrique d’étoiles candidates pour des disques de débris présenté par: Amélie Simon a été évalué par un jury composé des personnes suivantes: Serge Demers, président-rapporteur Pierre Bastien, directeur de recherche Gilles Fontaine, membre du jury Mémoire accepté le: Sommaire Le relevé DEBRIS est effectué par le télescope spatial Herschel. Il permet d’échantillonner les disques de débris autour d’étoiles de l’environnement solaire. Dans la première partie de ce mémoire, un relevé polarimétrique de 108 étoiles des candidates de DEBRIS est présenté. Utilisant le polarimètre de l’Observatoire du Mont-Mégantic, des observations ont été effec- tuées afin de détecter la polarisation due à la présence de disques de débris. En raison d’un faible taux de détection d’étoiles polarisées, une analyse statistique a été réalisée dans le but de comparer la polarisation d’étoiles possédant un excès dans l’infrarouge et la polarisation de celles n’en possédant pas. Utilisant la théorie de diffusion de Mie, un modèle a été construit afin de prédire la polarisation due à un disque de débris. Les résultats du modèle sont cohérents avec les observations. La deuxième partie de ce mémoire présente des tests optiques du polarimètre POL-2, construit à l’Université de Montréal. -
Total Solar Eclipse of 2002 December 4
NASA/TP—2001–209990 Total Solar Eclipse of 2002 December 04 F. Espenak and J. Anderson Central Lat,Lng = -28.0 132.0 P Factor = 0.46 Semi W,H = 0.35 0.28 Offset X,Y = 0.00-0.00 1999 Oct 26 10:40:42 AM High Res World Data [WPD1] WorldMap v2.00, F. Espenak Orthographic Projection Scale = 8.00 mm/° = 1:13915000 Central Lat,Lng = -10.0 26.0 P Factor = 0.31 Semi W,H = 0.70 0.50 Offset X,Y = 0.00-0.00 1999 Oct 26 10:17:57 AM September 2001 The NASA STI Program Office … in Profile Since its founding, NASA has been dedicated to • CONFERENCE PUBLICATION. Collected the advancement of aeronautics and space papers from scientific and technical science. The NASA Scientific and Technical conferences, symposia, seminars, or other Information (STI) Program Office plays a key meetings sponsored or cosponsored by NASA. part in helping NASA maintain this important role. • SPECIAL PUBLICATION. Scientific, techni- cal, or historical information from NASA The NASA STI Program Office is operated by programs, projects, and mission, often con- Langley Research Center, the lead center for cerned with subjects having substantial public NASA’s scientific and technical information. The interest. NASA STI Program Office provides access to the NASA STI Database, the largest collection of • TECHNICAL TRANSLATION. aeronautical and space science STI in the world. English-language translations of foreign scien- The Program Office is also NASA’s institutional tific and technical material pertinent to NASA’s mechanism for disseminating the results of its mission. -
A Roman Frontier Post and Its People
CHAPTER IX Dress and Armour As we gather together the relics brought to light from the abandoned wells and rubbish-pits at Newstead, the figure of the Roman soldier inevitably rises before us. It is a figure rendered familiar by the great monuments which commemorate Imperial triumphs, and by the portrait-reliefs which once stood above the graves of centurions, cavalry soldiers, or standard-bearers recalling to the passers-by the likeness of the dead. It is to such memorials, and to the scanty finds of weapons and armour which have been preserved to our time, that we owe most of the knowledge we possess regarding the arms and equipment of the army of the Empire. The columns and the triumphal arches furnish us with a series of pictures of the soldier in action. The victories of Trajan over the Dacians are sculptured on the column which he had set up in Rome in A.D. 104. The triumphs of Marcus Aurelius over the Marcomanni are unfolded in the reliefs decorating the huge pillar that gives its name to the Piazza Colonna. We follow each stage in the campaigns, the army making roads, building bridges, constructing forts, attacking and attacked. Many details are given which help us to realise vividly the scenes commemorated. No doubt in such sculptures, executed, as they were, in Rome, the artists drew their inspiration to some extent from older Hellenic models, and there thus enters into the treatment a somewhat conventional element. The grave stones of the legionaries or auxiliaries, on the other hand, are probably more exact in details. -
![Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs](https://docslib.b-cdn.net/cover/4203/arxiv-2105-11583v2-astro-ph-ep-2-jul-2021-keck-hires-apf-levy-and-lick-hamilton-spectrographs-364203.webp)
Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i, -
Two Rings but No Fellowship: Lotr 1 and Its Relation to Planetary Nebulae
Mon. Not. R. Astron. Soc. 000, 1–16 (2013) Printed 17 October 2018 (MN LATEX style file v2.2) Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing barium central stars. A.A. Tyndall1,2⋆, D. Jones2, H.M.J. Boffin2, B. Miszalski3,4, F. Faedi5, M. Lloyd1, J.A. L´opez6, S. Martell7, D. Pollacco5, and M. Santander-Garc´ıa8 1Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, M13 9PL, UK 2European Southern Observatory, Alonso de C´ordova 3107, Casilla 19001, Santiago, Chile 3South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa 4Southern African Large Telescope. PO Box 9, Observatory 7935, South Africa 5Department of Physics, University of Warwick, CV4 7AL, UK 6Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ensenada, Baja California, C.P. 22800, Mexico 7Australian Astronomical Observatory, North Ryde, 2109 NSW, Australia 8Observatorio Astron´omico National, Madrid, and Centro de Astrobiolog´ıa, CSIC-INTA, Spain Accepted xxxx xxxxxxxx xx. Received xxxx xxxxxxxx xx; in original form xxxx xxxxxxxx xx ABSTRACT LoTr 1 is a planetary nebula thought to contain an intermediate-period binary central star system ( that is, a system with an orbital period, P, between 100 and, say, 1500 days). The system shows the signature of a K-type, rapidly rotating giant, and most likely constitutes an accretion-induced post-mass transfer system similar to other PNe such as LoTr 5, WeBo 1 and A70. Such systems represent rare opportunities to further the investigation into the formation of barium stars and intermediate period post-AGB systems – a formation process still far from being understood. -
PDF Catalogue
1 GAUL, Massalia, c. 200-120 BCE, AR obol. 0.60g, 9mm. Obv: Bare head of Apollo left Rev: M A within wheel of four spokes. Depeyrot, Marseille 31 From the JB (Edmonton) collection. Obverse off-centre, but high grade, superb style, perfect metal, and spectacular toning. Estimate: 100 Starting price: 50 CAD 2 CIMMERIAN BOSPORUS, Pantikapaion, c. 310-303BC, AE 22. 7.61g, 21.5mm Obv: Bearded head of Satyr (or Pan), right Rev: P-A-N, forepart of griffin left, sturgeon left below Anokhin 1023; MacDonald 69; HGC 7, 113 Ex Lodge Antiquities Estimate: 100 Starting price: 50 CAD 3 CIMMERIAN BOSPOROS, Pantikapaion, c. 325-310 BCE, AE17. 3.91g, 17mm. Obv: Head of satyr left Rev: ΠΑΝ; Head of bull left. MacDonald 67; Anokhin 1046 From the JB (Edmonton) collection. Starting price: 30 CAD 4 THESSALY, Atrax, 3rd c. BCE, AE trichalkon. 6.03g, 18mm. Obv: Laureate head of Apollo right Rev: ATP-A-Γ-IΩN, horseman, raising right hand, advancing right. Rogers 169-71; BCD Thessaly II 59.6-10 Starting price: 30 CAD 5 THESSALY, Krannon, circa 350-300 BCE, AE chalkous. 2.41g, 15.4mm. Obv: Thessalian warrior on horse rearing right. Rev: KPAN, bull butting right; above, trident right. BCD Thessaly II 118.5; HGC 4, 391 From the zumbly collection; ex BCD Collection, with his handwritten tag stating, “V. Ex Thess., Apr. 94, DM 35” Starting price: 30 CAD 6 THESSALY, Phalanna, c. 350 BCE, AE 18 (dichalkon or trichalkon). 6.53g, 17.5mm. Obv: Head of Ares right, A to left . -
Low-Tech Armortm
LOADOUTS:TM LOW-TECH ARMORTM Written by DAN HOWARD Edited by JASON “PK” LEVINE Illustrated by DAVID DAY, DAN HOWARD, and SHANE L. JOHNSON GURPS System Design ❚ STEVE JACKSON e23 Manager ❚ STEVEN MARSH GURPS Line Editor ❚ SEAN PUNCH Marketing Director ❚ LEONARD BALSERA Managing Editor ❚ PHILIP REED Director of Sales ❚ ROSS JEPSON Assistant GURPS Line Editor ❚ JASON “PK” LEVINE Prepress Checker ❚ NIKKI VRTIS Production Artist & Indexer ❚ NIKOLA VRTIS Page Design ❚ PHIL REED and JUSTIN DE WITT Art Direction ❚ MONICA STEPHENS GURPS FAQ Maintainer ❚ VICKY “MOLOKH” KOLENKO Lead Playtester: Douglas H. Cole Playtesters: Roger Burton West, Nathan Joy, Rob Kamm, Stephen Money, David Nichols, and Antoni Ten Monrós GURPS, Warehouse 23, and the all-seeing pyramid are registered trademarks of Steve Jackson Games Incorporated. Pyramid, Loadouts, Low-Tech Armor, e23, and the names of all products published by Steve Jackson Games Incorporated are registered trademarks or trademarks of Steve Jackson Games Incorporated, or used under license. GURPS Loadouts: Low-Tech Armor is copyright © 2013, 2017 by Steve Jackson Games Incorporated. Some art © 2013 JupiterImages Corporation. All rights reserved. The scanning, uploading, and distribution of this material via the Internet or via any other means without the permission of the publisher is illegal, and punishable by law. Please purchase only authorized electronic editions, and do not participate in or encourage the electronic piracy of copyrighted materials. Your support of the author’s rights is appreciated. STEVE JACKSON GAMES Stock #37-1581 Version 1.0.1 – June 2017 ® CONTENTS INTRODUCTION . 3 Padded Jacks . 41 Recommended Books . 3 How a Man Shall Be Armed . 42 Additional Rules . -
Kod Nazwa 337975 Smartfon Samsung A705f
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Transition from Spot to Faculae Domination--An Alternate
Astronomy & Astrophysics manuscript no. AC2_arxiv c ESO 2018 October 30, 2018 Transition from spot to faculae domination An alternate explanation for the dearth of intermediate Kepler rotation periods Timo Reinhold1; 2, Keaton J. Bell1; 2, James Kuszlewicz1; 2, Saskia Hekker1; 2, Alexander I. Shapiro1 1 Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany 2 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, 120 Ny Munkegade, Building 1520, DK- 8000 Aarhus C, Denmark Received day month year / Accepted day month year ABSTRACT Context. The study of stellar activity cycles is crucial to understand the underlying dynamo and how it causes magnetic activity signatures such as dark spots and bright faculae. Having knowledge about the dominant source of surface activity might allow us to draw conclusions about the star’s age and magnetic field topology, and to put the solar cycle in context. Aims. We investigate the underlying process that causes magnetic activity by studying the appearance of activity signatures in con- temporaneous photometric and chromospheric time series. Methods. Lomb-Scargle periodograms are used to search for cycle periods present in the photometric and chromospheric time series. To emphasize the signature of the activity cycle we account for rotation-induced scatter in both data sets by fitting a quasi-periodic Gaussian process model to each observing season. After subtracting the rotational variability, cycle amplitudes and the phase differ- ence between the two time series are obtained by fitting both time series simultaneously using the same cycle period. Results. We find cycle periods in 27 of the 30 stars in our sample. -
The Rotation of the Sun As a Star from the Integrated Coronal Green-Line Emission M
ISSN 1063-7729, Astronomy Reports, 2009, Vol. 53, No. 4, pp. 343–354. c Pleiades Publishing, Ltd., 2009. Original Russian Text c M.M. Katsova, I.M. Livshits, J. Sykora, 2009, published in Astronomicheski˘ı Zhurnal, 2009, Vol. 86, No. 4, pp. 379–391. The Rotation of the Sun as a Star from the Integrated Coronal Green-Line Emission M. M. Katsova1, I. M. Livshits2,andJ.Sykora3 1Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899, Russia 2Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, IZMIRAN, Troitsk, Moscow Region, 142190, Russia 3Institute of Astronomy, Slovak Academy of Sciences, Tatranska Lomnica, Slovakia Received 2008; in final form, July 2, 2008 Abstract—A new representation for the database collected by J. Sykora on the Fe XIV 5303 A˚ line emission observed from 1939 to 2001 is proposed. Observations of the corona at an altitude of 60 above the limb reduced to a single photometric scale provide estimates of the emission of the entire visible solar surface. It is proposed to use the resulting series of daily measurements as a new index of the solar activity, GLSun (The Green-Line Sun). This index is purely observational and is free of the model-dependent limitations imposed on other indices of coronal activity. GLSun describes well both the cyclic activity and the rotational modulation of the brightness of the corona of the Sun as a star. The GLSun series was subject to a wavelet analysis similar to that applied to long-term variations in the chromospheric emission of late active stars. The brightness irregularities in the solar corona rotate more slowly during epochs of high activity than their average rotational speed over the entire observational interval. -
Mag Sep PA Spectra Colors Seen Luminosity a 7.3 N/A N/A A1 V W 60 B 8.2 62 7 B 25 C 7.1 302 243 W 70 Observations: Observed at 104X
33 Doubles in Canis Major and Canis Minor Observed 1988-1996 with a C-8 (Celestron) from Columbia, Missouri (USA) and Kansas City, Missouri. Observer: Richard Harshaw Dates and sky conditions were not logged at this time in my observations. South 516 (HD 44144; SAO 171562) Rating: 3 Position: 0619-2459 Year of last measure: 1959 Assumed distance (l.y.): 770 Assumed luminosity (suns): 155 Mag Sep PA Spectra Colors Seen Luminosity A 7.3 n/a n/a A1 V W 60 B 8.2 62 7 B 25 C 7.1 302 243 W 70 Observations: Observed at 104x. Rich field. Notes: Hipparcos/Tycho data show different distances for these stars; they may be an optical system. The stars have different proper motions. South 518 (ADS 5034; HD 45016; SAO 151462) Rating: 2 Position: 0624-1614 Year of last measure: 1917 Assumed distance (l.y.): 890 Assumed luminosity (suns): 123 Mag Sep PA Spectra Colors Seen Luminosity A 7.0 n/a n/a A9 V W 100 B 8.6 16 88 A B 23 Observations: Observed at 83x. Rich field. Notes: Hipparcos/Tycho data show different distances for these stars; they may be an optical system. h3863 (ADS 5128; HD 45941; SAO 171831) Rating: 3 Position: 0629-2236 Year of last measure: 1959 Assumed distance (l.y.): 1,190 Assumed luminosity (suns): 237 Mag Sep PA Spectra Colors Seen Luminosity A 6.8 n/a n/a A2 V Y 200 B 8.7 3 119 Y 37 Observations: Observed at 280x. Rich field. Notes: First measure: 2.7" @ 119 (Doolittle). -
Section 3.6 Selected Stars from the Hipparcos
Section 3.6 Selected Stars from the Hipparcos Catalogue 481 3.6. Selected Stars from the Hipparcos Catalogue In this section certain key results from the Hipparcos Catalogue are presented for various sets of stars selected according to a number of criteria. Table 3.6.1 lists results for the 150 stars closest to the Sun, as deduced from the Hipparcos parallaxes. No criterion was applied to the precision of the individual parallax determinations. The entries in the table are sorted by decreasing parallax (increasing distance). Table 3.6.2 gives the results for the 150 stars with the largest total proper motions in the Hipparcos Catalogue, again without further selection on precision. Table 3.6.3 gives the results for the 150 stars with the largest total transverse velocity, as deduced from the Hipparcos proper motions and parallaxes. In the latter table, only stars with relative distance precision σπ /π < 0.1 were included. The entries in these tables are sorted by decreasing total proper motion and total transverse velocity, respectively. For Table 3.6.4, the table with 150 stars with the highest absolute luminosity, the se- lection was more delicate. Although Hipparcos has determined for each entry at least a lower limit for the distance, and consequently for the luminosity, the inclusion of stars with only such a lower limit in the table was not considered meaningful. The stars in the table meet the two following criteria: (i) relative distance precision σπ /π < 0.3; (ii) ab- solute magnitude MV when computed with the 2-σ lower distance limit 1/(π + 2σπ ) smaller than −2 mag.