Abundances and Radial Velocity Analysis of BW Vulpeculae?
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Binocular Universe: Sly Fox September 2010 Phil Harrington
Binocular Universe is available every month on Cloudynights.com Binocular Universe: Sly Fox September 2010 Phil Harrington ast month's Stellafane convention, held atop Breezy Hill outside of Springfield, Vermont, was the best in recent memory. The skies were the Lclearest we've had in years, giving us a chance to enjoy the beauty of the summer Milky Way, which stretched from horizon to horizon. Armed with my trusty 10x50 and 16x70 binoculars, I sat back in my reclining chair and swept the plane of our Galaxy in pursuit of some old friends and new conquests. Above: Summer star map from Star Watch by Phil Harrington Binocular Universe is available every month on Cloudynights.com Above: Finder chart for this month's Binocular Universe. Chart adapted from Touring the Universe through Binoculars Atlas (TUBA), www.philharrington.net/tuba.htm Binocular Universe is available every month on Cloudynights.com Here are a few gems I bumped into along the way as I viewed the tiny constellation of Vulpecula the Fox. Vulpecula is a faint summertime constellation wedged between Cygnus (the Swan) to the north and Sagitta (the Arrow) to the south. None of Vulpecula’s stars shine brighter than magnitude 4.5, so seeing a fox here is a tall order indeed. But the sly Fox holds many binocular treasures for those who the time to seek them out. Vulpecula was created in 1687 by the Polish astronomer Johannes Hevelius. His original drawing showed a small fox carrying a hapless goose in its mouth. He called the combination Vulpecula et Anser ("the little fox and the goose"). -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
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. -
CONSTELLATION VULPECULA, the (LITTLE) FOX Vulpecula Is a Faint Constellation in the Northern Sky
CONSTELLATION VULPECULA, THE (LITTLE) FOX Vulpecula is a faint constellation in the northern sky. Its name is Latin for "little fox", although it is commonly known simply as the fox. It was identified in the seventeenth century, and is located in the middle of the northern Summer Triangle (an asterism consisting of the bright stars Deneb in Cygnus (the Swan), Vega in Lyra (the Lyre) and Altair in Aquila (the Eagle). Vulpecula was introduced by the Polish astronomer Johannes Hevelius in the late 17th century. It is not associated with any figure in mythology. Hevelius originally named the constellation Vulpecula cum ansere, or Vulpecula et Anser, which means the little fox with the goose. The constellation was depicted as a fox holding a goose in its jaws. The stars were later separated to form two constellations, Anser and Vulpecula, and then merged back together into the present-day Vulpecula constellation. The goose was left out of the constellation’s name, but instead the brightest star, Alpha Vulpeculae, carries the name Anser. It is one of the seven constellations created by Hevelius. The fox and the goose shown as ‘Vulpec. & Anser’ on the Atlas Coelestis of John Flamsteed (1729). The Fox and Goose is a traditional pub name in Britain. STARS There are no stars brighter than 4th magnitude in this constellation. The brightest star is: Alpha Vulpeculae, a magnitude 4.44m red giant at a distance of 297 light-years. The star is an optical binary (separation of 413.7") that can be split using binoculars. The star also carries the traditional name Anser, which refers to the goose the little fox holds in its jaws. -
Annual Report 2016–2017 AAVSO
AAVSO The American Association of Variable Star Observers Annual Report 2016–2017 AAVSO Annual Report 2012 –2013 The American Association of Variable Star Observers AAVSO Annual Report 2016–2017 The American Association of Variable Star Observers 49 Bay State Road Cambridge, MA 02138-1203 USA Telephone: 617-354-0484 Fax: 617-354-0665 email: [email protected] website: https://www.aavso.org Annual Report Website: https://www.aavso.org/annual-report On the cover... At the 2017 AAVSO Annual Meeting.(clockwise from upper left) Knicole Colon, Koji Mukai, Dennis Conti, Kristine Larsen, Joey Rodriguez; Rachid El Hamri, Andy Block, Jane Glanzer, Erin Aadland, Jamin Welch, Stella Kafka; and (clockwise from upper left) Joey Rodriguez, Knicole Colon, Koji Mukai, Frans-Josef “Josch” Hambsch, Chandler Barnes. Picture credits In additon to images from the AAVSO and its archives, the editors gratefully acknowledge the following for their image contributions: Glenn Chaple, Shawn Dvorak, Mary Glennon, Bill Goff, Barbara Harris, Mario Motta, NASA, Gary Poyner, Msgr. Ronald Royer, the Mary Lea Shane Archives of the Lick Observatory, Chris Stephan, and Wheatley, et al. 2003, MNRAS, 345, 49. Table of Contents 1. About the AAVSO Vision and Mission Statement 1 About the AAVSO 1 What We Do 2 What Are Variable Stars? 3 Why Observe Variable Stars? 3 The AAVSO International Database 4 Observing Variable Stars 6 Services to Astronomy 7 Education and Outreach 9 2. The Year in Review Introduction 11 The 106th AAVSO Spring Membership Meeting, Ontario, California 11 The -
On the Polar Distances of the Greenwich Transit Circle
fi 1260-1263. l'he prominence, which iR due in many astronoiiiicsl re- ortlcr to restore this uniforiiiify , which is otiviously of the searches to the long and excellent series of the Greenwich iiiost esseritial iiriporhiicbe, 1 have rel'errctl all the otiser- mericliorial oliservations, gives to any changes of the instrri- vatioiis to the Circle reatlirigs. which corresporrtl to the Naclir nients, by means of which these ohservatioiis are procurecl, observations of the wire. It iiiight have heen tlcsirahle to a higher and more general importance, than they woulcl other- get rid, as much as pnssilile, of' pere~nalecpitions in the wise possess. Hence the interest, with which astrononicrs reading of iiiicroscope - iiiicronieters etc. hy iisiclg for each are wont to regRrtl the construction and cfhiency of any new observer his own Zenithpoints. A closer inspec:tiori sjiotv,, instrunient of superior pretensions, is greatly enhanced in however, that, owing to several ciiwes, this (:nurse is for the case of the powerful Greenwich Transit Circle, and the the past observations inipracticable. I have 'coiiserperitly asiral question, concerning the degree of correctness, which considered it best to adopt the same periods of uri;iltered the results of a new apparatus have attained, acquires addi- Zenithpoints, as have Iieerl used in the Greenwiclr rechictioris. tional claims to be answered. As I an1 not aware, that a The values of the corrections, which it was accordingly seces- strict determination of this point has yet been attempted, 1 sary to apply to the single ohservations, fluctuate I)ct\veeri shall here niake it the suhject of inquiry with reepect to -fO"45 and TO"71. -
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). -
The Professor Comet's Report Late Summer/Early Autumn – September
The Professor Comet’s Report 1 Messier 71 and C/2009 P1 Garradd © Steve Grimsley of Houston Astronomical Society, 2011 Welcome to the comet report which is a monthly article on the observations of comets by the amateur astronomy community and comet hunters from around the world! This article is dedicated to the latest reports of available comets for observations, current state of those comets, future predictions, & projections for observations in comet astronomy! Late Summer/Early Autumn – September 2011 The Professor Comet’s Report 2 The Current Status of the Predominant Comets for July 2011! Comets Designation Orbital Magnitude Trend Observation Constellations Visibility (IAU – MPC) Status Visual (Range in Lat.) (Night Sky Location) Period Garradd 2009 P1 C 7.0 – 7.2 Getting 60°N – 60°S Between Sagitta and Vulpecula All Night Brighter (heading WNW towards Hercules) Honda – 45P P 8.0 Getting 50°N – 85°S Undergoing a wide retrograde motion! Early Morning Mrkos - Brighter Currently the comet is north of Hydra Pajdusakova heading NE towards Leo Elenin 2010 X1 C 8.6 – 9.4 Getting 45°N – 75°S Currently undergoing retrograde Early Evening Brighter motion in the S region of Leo (Just after Dusk) Crommelin 27P P 9.5 Possibly N/A Poor Elongation N/A Fading? (lost in the daytime glare!) LINEAR 2011 M1 C 10.4 Brightening 60°N – 45°N Moving SE of Ursa Major and All Night heading across the E edge of Leo Minor Hill 2010 G2 C 11.1 Fading 60°N – 10°N Between Ursa Major and Lynx All Night (Moving SSW of Muscida) Gibbs 2011 A3 C 11.4 Brightening 55°N -
2001 Astronomy Magazine Index
2001 Astronomy magazine index Subject index Chandra X-ray Observatory, telescope of, free-floating planets, 2:20, 22 12:76 A Christmas Star, 1:102 absolute visual magnitude, 1:86 cold dark matter, 3:24, 26 G active region 9393, 7:22 colors, of celestial objects, 9:82–83 Gagarin, Yuri, 4:36–41 Africa, observation from, 4:107–112, 10:48– Comet Borrelly, 9:33–37 galaxies 53 comets, 2:93 clusters of Andromeda Galaxy computers, accessing image archives with, in constellation Leo, 5:28 constellations of, 11:64–69 7:40–45 Massive Cluster Survey (MACS), consuming other galaxies, 12:25 corona of Sun, 1:24, 26 3:28 warp in disk of, 5:22 cosmic rays collisions of, 6:24 animal astronauts, 4:43–47 general information, 1:36–39 space between, 9:81 apparent visual magnitude, 1:86 origin of, 1:43–47 gamma ray bursts, 1:28, 30 Apus (constellation), 7:80–84 cosmology Ganymede (Jupiter's moon), 5:26 Aquila (constellation), 8:66–70 and particle physics, 6:39–43 Gemini Telescope, 2:26, 28 Ara (constellation), 7:80–84 unanswered questions, 6:46–52 Giodorno Bruno crater, 11:28, 30 Aries (constellation), 11:64–69 Gliese 876 (red dwarf star), 4:18 artwork, astronomical, 12:80–85 globular clusters, viewing, 8:72 asteroids D green stars, 3:82–85 around Zeta Leporis (star), 11:26 dark matter Groundhog Day, 2:96–97 cold, 3:24, 26 near Earth, 8:44–49 astronauts, animal as, 4:43–47 distribution of, 12:30, 32 astronomers, amateur, 10:88–89 whether exists, 8:26–31 H Hale Telescope, 9:46–53 astronomical models, 9:22, 24 deep sky objects, 7:87 HD 168443 (star), 4:18 Astronomy.com website, 1:78–84 Delphinus (constellation), 10:72–76 HD 82943 (star), 8:18 astrophotography DigitalSky Voice software, 8:65 HH 237 (meteor), 6:22 black holes, 1:26, 28 Dobson, John, 9:68–71 HR 1998 (star), 11:26 costs of basic equipment, 5:86 Dobsonian telescopes HST. -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
Variable Star Section Circular
British Astronomical Association Variable Star Section Circular No 77, August 1993 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG Section Officers Director Tristram Brelstaff, 3 Malvern Court, Addington Road, Reading, Berks, RG1 5PL Tel: 0734-268981 Assistant Director Storm R Dunlop 140 Stocks Lane, East Wittering, Chichester, West Sussex, P020 8NT Tel: 0243-670354 Telex: 9312134138 (SD G) Email: CompuServe:100015,1610 JANET:SDUNLOP@UK. AC. SUSSEX.STARLINK Secretary Melvyn D Taylor, 17 Cross Lane, Wakefield, West Yorks, WF2 8DA Tel: 0924-374651 Chart John Toone, Hillside View, 17 Ashdale Road, Secretary Cressage, Shrewsbury, SY5 6DT Tel: 0952-510794 Nova/Supernova Guy M Hurst, 16 Westminster Close, Kempshott Rise, Secretary Basingstoke, Hants, RG22 4PP Tel & Fax: 0256-471074 Telex: 9312111261 (TA G) Email: Telecom Gold:10074:MIK2885 STARLINK:RLSAC::GMH JANET:GMH0UK. AC. RUTHERFORD.STARLINK. ASTROPHYSICS Pro-Am Liaison Roger D Pickard, 28 Appletons, Hadlow, Kent, TN11 0DT Committee Tel: 0732-850663 Secretary Email: JANET:RDP0UK.AC.UKC.STAR STARLINK:KENVAD: :RDP Computer Dave McAdam, 33 Wrekin View, Madeley, Telford, Secretary Shropshire, TF7 5HZ Tel: 0952-432048 Email: Telecom Gold 10087:YQQ587 Eclipsing Binary Director Secretary Circulars Editor Director Circulars Assistant Director Subscriptions Telephone Alert Numbers Nova and Supernova First phone Nova/Supernova Secretary. If only Discoveries answering machine response then try the following: Denis Buczynski 0524-68530 Glyn Marsh 0772-690502 Martin Mobberley 0245-475297 (weekdays) 0284-828431 (weekends) Variable Star Gary Poyner 021-3504312 Alerts Email: JANET:[email protected] STARLINK:BHVAD::GP For subscription rates and charges for charts and other publications see inside back cover Forthcoming Variable Star Meeting in Cambridge Jonathan Shanklin says that the Cambridge University Astronomical Society is planning a one-day meeting on the subject of variable stars to be held in Cambridge on Saturday, 19th February 1994. -
A Review of the O--C Method and Period Change
A Review of The O–C Method and Period Change ∗ ZHOU Ai-Ying Beijing Astronomical Observatory, Chinese Academy of Sciences E-mail: [email protected] Abstract The classical O–C curves are discussed in different cases in which various period changes involved. Among them, the analytic O–C curves with frequency, amplitude mod- ulations and with double modes are closely inspected, respectively. As a special, the light-time effect is illustrated. The features of period change noise and period change to metallicity are added at the end. Keywords: O–C method–period change 1 Introduction The O–C diagram is a plot showing the observed times of maximum light(O) minus those calculated according to an adopted ephemeris(C) plotted as a function of time, mostly, the number of elapsed cycles. In the same way, the O–C diagram can also be constructed by the difference between the observed times of maximum radial velocity and the times predicted from an adopted ephemeris. One may find the minima are used instead of maxima for some variables. In particular, the spectroscopic and photometric O–C values are combined to produce a single arXiv:astro-ph/0304066v1 3 Apr 2003 O–C diagram. The employment of the O–C diagram almost means normal or regular periodic light curve with a large amplitude is concerned. In other words, the times of maximum light can be determined sufficiently well from the observed light data. One can find ‘O’ by fitting a single sinusoid with an assumed pulsation period to observations. ‘O’ may be derived through local fit to the light curves around individual maxima as well.