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The Desert Sky Observer
Desert Sky Observer Volume 32 Antelope Valley Astronomy Club Newsletter February 2012 Up-Coming Events February 10: Club Meeting* February 11: Moon Walk @ Prime Desert Woodlands February 13: Executive Board Meeting @ Don’s house February 18: Telescope Night and Star Party @ Devil's Punchbowl * Monthly meetings are held at the S.A.G.E. Planetarium on the Cactus School campus in Palmdale, the second Friday of each month. The meeting location is at the northeast corner of Avenue R and 20th Street East. Meetings start at 7 p.m. and are open to the public. Please note that food and drink are not allowed in the planetarium President Don Bryden Well I gave a star party and no one showed up! Not that I can blame them – it was raining and windy and cold – it even hailed! Still I dragged out the scope and got it ready to go. Briefly, between the clouds I looked at Jupiter and it was quite a treat. The Galilean moons were all tight to the planet either coming from just in front or behind. It gave a bejeweled look like a large ruby surrounded by four small diamonds. Even with the winds and clouds the sky was surprisingly steady and I went as high as 260x with ease, exposing the shadow of Europa transiting the planet. But soon more clouds came and inside we had a nice fire so I put the Artist's rendering DVD “400 Years of the Telescope” on and settled in for the night. My daughter had a few friends over after a skating party that afternoon and later when I went out for one more look they came out to see what was up. -
The Observer's Handbook for 1929
The O bserver’s H andbook FOR 1929 PUBLISHED BY The Royal A stronomical Society of Canada E d ited by C. A. CHANT TWENTY-FIRST YEAR OF PUBLICATION TORONTO 198 College Street Printed for the Society 1929 CALENDAR The O bserver’s H andbook FOR 1929 PUBLISHED BY The Royal Astronomical Society of Canada TORONTO 198 C ollege Street Prin ted for the Society 1929 CONTENTS Preface ------- 3 Anniversaries and Festivals - 3 Symbols and Abbreviations - 4 Solar and Sidereal Time - 5 Ephemeris of the Sun - - - 6 Occultations of Fixed Stars by the Moon - 8 Times of Sunrise and Sunset - 9 Planets for the Year ------ 22 Eclipses in 1929 - - - - 26 The Sky and Astronomical Phenomena for each Month 28 Phenomena of Jupiter’s Satellites - 52 Meteors and Shooting Stars - - - 54 Elements of the Solar System - 55 Satellites of the Solar System - 56 Double Stars, with a short list - 57 Variable Stars, with a short list 59 Distances of the Stars - 61 The Brightest Stars, their magnitudes, types, proper motions, distances and radial velocities - 63 Astronomical Constants - 71 Index - - - - - - - 72 PREFACE It may be stated that four circular star-maps, 9 inches in diameter, roughly for the four seasons, may be obtained from the Director of University Extension, University of Toronto, for one cent each; also a set of 12 circular maps, 5 inches in diameter, with brief explanation, is supplied by Popular Astronomy, Northfield, Minn., for 15 cents. Besides these may be mentioned Young’s Uranography, containing four maps with R.A. and Decl. circles and excellent descriptions of the constellations, price 72 cents; Norton's Star Atlas and Telescopic Handbook (10s. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Photometry Request-B Persei.Pdf
Will the radio source b Persei be eclipsed? R. T. Zavala1 & J. J. Sanborn2 December 14, 2012 The ellipsoidal variable star b Persei (HR1324, HD26961, V=4.6) consists of a non-eclipsing close binary (A-B) with a 1.5 day orbital period within a hierarchical triple system (AB-C) with a 701 day orbit (Hill et al. 1976). As with other close binary systems (e.g. β Per) b Per exhibits flares of non- thermal radio emission (Hjellming & Wade 1973). As noted by Hill et al. (1976) the evolutionary nature of the close binary in b Per is uncertain. It may already be a mass-transferring Algol binary, or it may be a precursor to the mass-transfer stage. The absence of eclipses in the close binary and b Per’s status as a single-lined spectroscopic binary limit our knowledge of this stellar radio source. Our observations using the Navy Precision Optical Interferometer (NPOI) resolved the AB-C components for the first time. The triple system orbit is nearly edge-on with an inclination of approximately 90 degrees (Fig. 1). This suggests the possibility of observing eclipses of the non- eclipsing (i ~ 40 degrees; Hill et al. 1976) close binary and the third star. The third star may eclipse both components of the close binary depending on the close binary orbital phase. Eclipses are important as they allow us to add lightcurve modeling to our arsenal of techniques for investigating the evolutionary state of the close binary components. The reality of our edge-on orbit for b Per C is supported by Hill et al. -
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, -
Stellar Chromospheric Activity and Age Relation from Open Clusters in the LAMOST Survey
Publications 12-12-2019 Stellar Chromospheric Activity and Age Relation from Open Clusters in the LAMOST Survey Jiajun Zhang University of Chinese Academy of Sciences, Terry Oswalt Embry-Riddle Aeronautical University, [email protected] Jingkun Zhao University of Chinese Academy of Sciences, Xiangsong Fang National Astronomical Observatories Gang Zhao Chinese Academy of Sciences, See next page for additional authors Follow this and additional works at: https://commons.erau.edu/publication Part of the Stars, Interstellar Medium and the Galaxy Commons Scholarly Commons Citation Zhang, J., Oswalt, T., Zhao, J., Fang, X., Zhao, G., Liang, X., Ye, X., & Zhong, J. (2019). Stellar Chromospheric Activity and Age Relation from Open Clusters in the LAMOST Survey. The Astrophysical Journal, 887(1). Retrieved from https://commons.erau.edu/publication/1383 This Article is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Authors Jiajun Zhang, Terry Oswalt, Jingkun Zhao, Xiangsong Fang, Gang Zhao, Xilong Liang, Xianhao Ye, and Jing Zhong This article is available at Scholarly Commons: https://commons.erau.edu/publication/1383 Draft version October 1, 2019 Typeset using LATEX default style in AASTeX62 Stellar chromospheric activity and age relation from open clusters in the LAMOST Survey Jiajun Zhang,1, 2 Jingkun Zhao,1 Terry D. Oswalt,3 Xiangsong Fang,4, 5 Gang Zhao,1, 2 Xilong Liang,1, 2 Xianhao Ye,1, 2 and Jing Zhong6 1Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
B Persei, a Fundamental Star Among the Radiostars
242 B PERSEI, A FUNDAMENTAL STAR AMONG THE RADIOSTARS Suzanne DEBARBAT Observatoire de Paris, DANOF/URA 1125 61 avenue de 1'Observatoire 75014 Paris ABSTRACT. Optical fluctuations of the radiostar (3 Persei are seen from 13 campaigns performed with the astrolabe located at the Paris Observatory. 1. INTRODUCTION Among the radiostars, fSPersei (Algol) - a fundamental star - was chosen by radioastronomers as a zero reference for right ascensions in radioastrometry. Since 1975 this fundamental star has been included in the observing programme performed by the "Astrolabe et systemes de re"fdrence" group in charge of the instrument at the Paris Observatory. The eight first campaigns published have been presented at the IAU Colloquium n° 100 (Belgrade 1987). The average of the mean square errors given were 0.004s in right ascension and 0.13" in declination, according to the FK4 and the constants in use at that time. 2. DETERMINATIONS AND ERRORS There are now thirteen campaigns available from 1975/76 to 1987/88 and they have been reduced in the FK5 system with the new fundamental constants according to the formulas established by Chollet (1984). Due to the fact that the group and the internal smoothing corrections (according to De"barbat et Guinot, 1970) are not yet available in the case of the FK5, the reduction have been performed for both FK4 and FK5. As an example of residuals, for the zenith distance, to which accuracy this quantity is obtainable when 12 transits (at east and at west) are observed, Table I gives the values for the 1983/1984 campaign (J 2000, FK4 and FK5). -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Reflectionsreflections the Newsletter of the Popular Astronomy Club February 2020 President’S Corner FEBRUARY 2020 Mercury’S Disk
Affiliated with ReflectionsReflections The Newsletter of the Popular Astronomy Club February 2020 President’s Corner FEBRUARY 2020 Mercury’s disk. A bit higher in the sky, the planet Neptune is very much dim- Welcome to another edition of mer at magnitude 8. Binoculars or a “Reflections”, the telescope will be needed to see it. Final- universe’s best as- ly, follow the ecliptic up past Venus to tronomy newsletter. find Uranus, which at magnitude 5.8 is easier to find, but you will still want to Page Topic This issue has some 1-2 Presidents Corner great articles about use a pair of binoculars. A telescope will 3 Announcements/ astronomical events reveal Uranus’ diminutive pale blue disk. Info Alan Sheidler occurring during the 4-7 Contributions month of February. For starters, this If you happen to be an early riser, Feb- 8 Paul Castle ruary’s morning sky has some treats in Observatory Prog- month will be a great one for those of ect us who love to observe planets. During store for you. Saturn, Jupiter and Mars 9 NCRAL Messier the first half of the month, right after will be visible before sunrise. February’s Marathon/ 2020 sunset, the planet Mercury will be big event will be the occultation of Mars Sky Guide/ th about as high in the sky as it will be and by the moon on the 18 . If you have 2020 an ideal object for your telescope. never seen an occultation, you should Celestial Calendar put this on your calendar. Binoculars 10 Astronomy in Print While you are observing Mercury 11 First Light by (closest to the horizon), three other will help you see Mars as the moon ap- David Levy planets will also be visible, strung out proaches, but if you have a telescope, I 12 Upcoming Events like pearls on the ecliptic: Neptune, recommend you get it ready for this 13 Sign up Report Venus and Uranus. -
Binary Studies with the Navy Precision Optical Interferometer
ISSN 1845–8319 BINARY STUDIES WITH THE NAVY PRECISION OPTICAL INTERFEROMETER C. A. HUMMEL1, R. T. ZAVALA2 and J. SANBORN3 1European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 2U.S. Naval Observatory, Flagstaff Station, 10391 W. Naval Obs. Rd, Flagstaff, AZ 86001, USA 3Lowell Observatory and Northern Arizona University, Flagstaff, AZ 86001, USA Abstract. We present recent results from observations of binary and multiple systems made with the Navy Precision Optical Interferometer (NPOI) on ζ and σ Orionis A, ξ Tauri, HR 6493, and b Persei. We explain how the orbital modeling is performed and show that even triple systems can be constrained with the data. Key words: interferometry - binaries 1. Introduction Observations of binary stars are the bread-and-butter for optical interferom- eters. An easy exploit for the unrivaled angular resolution of long baseline interferometers, the measurement of the orbits of double-lined spectroscopic binaries affords the determination of fundamental parameters of stars as well as their distance from Earth. Interferometry thus extends the reach of using spectroscopic binaries to non-eclipsing pairs, as a special but unlikely geom- etry for seeing eclipses, which also allow the determination of high-precision stellar masses, is no longer required. After about a decade of developing the technique of long baseline optical interferometers, i.e. those combining independent telescopes observing in the visual or near-infrared bands with baselines in between them ranging from a few meters to over a hundred, three major facilities are now available for regular scientific observations, CHARA on Mt Wilson, California, NPOI on Anderson Mesa, Arizona, and VLTI on Cerro Paranal, Chile. -
The Desert Sky Observer
Desert Sky Observer Volume 31 Antelope Valley Astronomy Club Newsletter January 2011 Up-Coming Events January 8: Star Party @ Vasquez Rocks January 14: Club Meeting* January 17: Board meeting @ Don’s house * Monthly meetings are held at the S.A.G.E. Planetarium on the Cactus School campus in Palmdale, the second Friday of each month. The meeting location is at the northeast corner of Avenue R and 20th Street East. Meetings start at 7 p.m. and are open to the public. Please note that food and drink are not allowed in the planetarium President Don Bryden Happy New Year! I hope this reaches you before the star party on the eighth. This is our Dark Sky Star Party for January and it’s going to be a joint effort with the Local Group – the Astro club from Santa Clarita. We have a unique opportunity to observe from Vasquez Rocks State Park – the site of many classic TV shows and movies – my personal favorite is “Arena”, the Star Trek episode featuring the Gorn. Maybe we can show up early and try to construct a bamboo and gunpowder cannon (though I’d just settle for finding some big diamonds lying around on the ground). There are many other great events planned for 2011 including the annual Messier Marathon, RTMC (over Memorial weekend this year!), and of course our summertime weekends at Mt. Pinos. I’m hoping to debut the club’s new 13” truss dob at the Messier Marathon as well. This scope, a former Coulter dobsonian that was donated to the club, has been refigured and transformed into a very portable, very easy to use visual scope.