00E the Construction of the Universe Symphony
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Fully Automated and Do Not Require Human Intervention
ВІСНИК КИЇВСЬКОГО НАЦІОНАЛЬНОГО УНІВЕРСИТЕТУ ІМЕНІ ТАРАСА ШЕВЧЕНКА ISSN 1723-273х АСТРОНОМІЯ 1(51)/2014 Засновано 1958 року Викладено результати оригінальних досліджень із питань релятивістської астрофізики. фізики Сон- ця, астрометрії, небесної механіки. Для наукових працівників, аспірантів, студентів старших курсів, які спеціалізуються в галузі астрономії. Изложены результаты оригинальных исследований по вопросам релятивистской астрофізики, фи- зики Солнца, астрометрии, небесной механики. Для научных работников, аспирантов, студентов старших курсов, специализирующихся в области астрономии. The Herald includes results of original investigations on relativistic astrophysics, solar physics, astrom- etry, celestial mechanics. It is intended for scientists, post-graduate students and student-astronomers. ВІДПОВІДАЛЬНИЙ РЕДАКТОР В.М. Івченко, д-р фіз.-мат. наук, проф. РЕДАКЦІЙНА В.М. Єфіменко, канд. фіз.-мат. наук (заст. відп. ред.); О.В. Федорова, КОЛЕГІЯ канд. фіз.-мат. наук (відп. секр.); Б.І. Гнатик, д-р фіз.-мат. наук; В.І. Жданов, д-р фіз.-мат. наук; В.В. Клещонок, канд. фіз.-мат. наук; Р.І. Костик, д-р фіз.-мат. наук; В.Г. Лозицький, д-р фіз.-мат. наук; Г.П. Міліневський, д-р фіз.-мат. наук; С.Л. Парновський, д-р фіз.-мат. наук; І.Д. Караченцев, д-р фіз.-мат.наук; О.А. Соловйов, д-р фіз.-мат. наук; К.І. Чурюмов, д-р фіз.-мат. наук. Адреса редколегії 04053, Київ-53, вул. Обсерваторна, 3, Астрономічна обсерваторія (38044) 486 26 91, 481 44 78, [email protected] Затверджено Вченою радою Астрономічної обсерваторії 05.06.2014 (протокол № 9) Атестовано Вищою атестаційною комісією України. Постанова Президії ВАК України № 1-05/5 від 01.07.2010 Зареєстровано Міністерством інформації України. Свідоцтво про державну реєстрацію КВ № 20329-101129 Р від 25.07.2013 Засновник Київський національний університет імені Тараса Шевченка, та видавець Видавничо-поліграфічний центр "Київський університет" Свідоцтво внесено до Державного реєстру ДК № 1103 від 31.10.02 Адреса видавця 01601, Київ-601, б-р Т.Шевченка, 14, кімн. -
Durham E-Theses
Durham E-Theses First visibility of the lunar crescent and other problems in historical astronomy. Fatoohi, Louay J. How to cite: Fatoohi, Louay J. (1998) First visibility of the lunar crescent and other problems in historical astronomy., Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/996/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk me91 In the name of Allah, the Gracious, the Merciful >° 9 43'' 0' eji e' e e> igo4 U61 J CO J: lic 6..ý v Lo ý , ý.,, "ý J ýs ýºý. ur ý,r11 Lýi is' ý9r ZU LZJE rju No disaster can befall on the earth or in your souls but it is in a book before We bring it into being; that is easy for Allah. In order that you may not grieve for what has escaped you, nor be exultant at what He has given you; and Allah does not love any prideful boaster. -
A-Level Physics a Question Paper Unit 05
Please write clearly in block capitals. Centre number Candidate number Surname –––––––––––––––––––––––––––––––––––––––––––––––––––––––––– Forename(s) –––––––––––––––––––––––––––––––––––––––––––––––––––––––––– Candidate signature –––––––––––––––––––––––––––––––––––––––––––––––––––––––––– A-level PHYSICS A Unit 5A Astrophysics Section B Tuesday 28 June 2016 Morning Time allowed: The total time for both sections of this paper is Materials For this paper you must have: 1 hour 45 minutes. You are a calculator advised to spend approximately a pencil and a ruler a Data and Formulae Booklet (enclosed). 50 minutes on this section. Instructions Use black ink or black ball-point pen. Fill in the boxes at the top of this page. Answer all questions. You must answer the questions in the spaces provided. Do not write outside the box around each page or on blank pages. Do all rough work in this book. Cross through any work you do not want to be marked. Show all your working. Information The marks for questions are shown in brackets. The maximum mark for this section is 35. You are expected to use a calculator where appropriate. A Data and Formulae Booklet is provided as a loose insert. You will be marked on your ability to: – use good English – organise information clearly – use specialist vocabulary where appropriate. (JUN16PHYA52A01) WMP/Jun16/E4 PHYA5/2A Do not write 2 outside the box Section B The maximum mark for this section is 35. You are advised to spend approximately 50 minutes on this section. 1 A converging lens of focal length 0.15 m is used as the eyepiece of an astronomical refracting telescope in normal adjustment. 1 (a) The angular magnification of the telescope is 5.0 Calculate the distance between the eyepiece lens and the objective lens of the telescope. -
HST/WFC3 OBSERVATIONS of an OFF-NUCLEAR SUPERBUBBLE in ARP 220 Kelly E
The Astrophysical Journal, 810:149 (11pp), 2015 September 10 doi:10.1088/0004-637X/810/2/149 © 2015. The American Astronomical Society. All rights reserved. HST/WFC3 OBSERVATIONS OF AN OFF-NUCLEAR SUPERBUBBLE IN ARP 220 Kelly E. Lockhart1, Lisa J. Kewley2, Jessica R. Lu1, Mark G. Allen3, David Rupke4, Daniela Calzetti5, Richard I. Davies6, Michael A. Dopita2, Hauke Engel6, Timothy M. Heckman7, Claus Leitherer8, and David B. Sanders1 1 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2 Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek ACT 2611, Australia 3 Observatoire de Strasbourg, UMR 7550, Strasbourg, F-67000, France 4 Department of Physics, Rhodes College, Memphis, TN 38112, USA 5 Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 6 Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany 7 Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA 8 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 2015 March 7; accepted 2015 June 8; published 2015 September 9 ABSTRACT We present a high spatial resolution optical and infrared study of the circumnuclear region in Arp 220, a late-stage galaxy merger. Narrowband imaging using Hubble Space Telescope/WFC3 has resolved the previously observed peak in Hα+[N II] emission into a bubble-shaped feature. This feature measures 1″. 6 in diameter, or 600 pc, and is only 1″ northwest of the western nucleus. The bubble is aligned with the western nucleus and the large-scale outflow axis seen in X-rays. -
A CANDIDATE YOUNG MASSIVE PLANET in ORBIT AROUND the CLASSICAL T TAURI STAR CI TAU* Christopher M
The Astrophysical Journal, 826:206 (22pp), 2016 August 1 doi:10.3847/0004-637X/826/2/206 © 2016. The American Astronomical Society. All rights reserved. A CANDIDATE YOUNG MASSIVE PLANET IN ORBIT AROUND THE CLASSICAL T TAURI STAR CI TAU* Christopher M. Johns-Krull1,9, Jacob N. McLane2,3, L. Prato2,9, Christopher J. Crockett4,9, Daniel T. Jaffe5, Patrick M. Hartigan1, Charles A. Beichman6,7, Naved I. Mahmud1, Wei Chen1, B. A. Skiff2, P. Wilson Cauley1,8, Joshua A. Jones1, and G. N. Mace5 1 Department of Physics and Astronomy, Rice University, MS-108, 6100 Main Street, Houston, TX 77005, USA 2 Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA; [email protected], [email protected] 3 Department of Physics & Astronomy, Northern Arizona University, S San Francisco Street, Flagstaff, AZ 86011, USA 4 Science News, 1719 N Street NW, Washington, DC 20036, USA 5 Department of Astronomy, University of Texas, R. L. Moore Hall, Austin, TX 78712, USA 6 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 7 NASA Exoplanet Science Institute (NExScI), California Institute of Technology, 770 S. Wilson Avenue, Pasadena, CA 91125, USA 8 Department of Astronomy, Wesleyan University, 45 Wyllys Avenue, Middletown, CT 06459, USA Received 2015 October 1; revised 2016 May 7; accepted 2016 May 16; published 2016 August 1 ABSTRACT The ∼2 Myr old classical T Tauri star CI Tau shows periodic variability in its radial velocity (RV) variations measured at infrared (IR) and optical wavelengths. We find that these observations are consistent with a massive planet in a ∼9 day period orbit. -
Ioptron AZ Mount Pro Altazimuth Mount Instruction
® iOptron® AZ Mount ProTM Altazimuth Mount Instruction Manual Product #8900, #8903 and #8920 This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. AZ Mount ProTM Altazimuth Mount Overview...................................................................................... 5 2. AZ Mount ProTM Mount Assembly ........................................................................................................ 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. Go2Nova® 8407 Hand Controller .................................................................................................... 8 2.3.1. Key Description ....................................................................................................................... -
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. -
Modeling of PMS Ae/Fe Stars Using UV Spectra ,
A&A 456, 1045–1068 (2006) Astronomy DOI: 10.1051/0004-6361:20040269 & c ESO 2006 Astrophysics Modeling of PMS Ae/Fe stars using UV spectra, P. F. C. Blondel1,2 andH.R.E.TjinADjie1 1 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: [email protected] 2 SARA, Kruislaan 415, 1098 SJ Amsterdam, The Netherlands Received 13 February 2004 / Accepted 13 October 2005 ABSTRACT Context. Spectral classification of PMS Ae/Fe stars, based on visual observations, may lead to ambiguous conclusions. Aims. We aim to reduce these ambiguities by using UV spectra for the classification of these stars, because the rise of the continuum in the UV is highly sensitive to the stellar spectral type of A/F-type stars. Methods. We analyse the low-resolution UV spectra in terms of a 3-component model, that consists of spectra of a central star, of an optically-thick accretion disc, and of a boundary-layer between the disc and star. The disc-component was calculated as a juxtaposition of Planck spectra, while the 2 other components were simulated by the low-resolution UV spectra of well-classified standard stars (taken from the IUE spectral atlases). The hot boundary-layer shows strong similarities to the spectra of late-B type supergiants (see Appendix A). Results. We modeled the low-resolution UV spectra of 37 PMS Ae/Fe stars. Each spectral match provides 8 model parameters: spectral type and luminosity-class of photosphere and boundary-layer, temperature and width of the boundary-layer, disc-inclination and circumstellar extinction. -
A Spectroscopic Study of the Scorpio-Centaurus Association
PranllQa. Vol. 7, No.3, 1976, pp 160-\ 80. © Prmted in India. A spectroscopic study of the Scorpio-Centaurus association R RAJAMOHAN Indian Institute of Astrophysics, Bangaiore 560034 MS recehcl 5 April 1976 • I' Abstract. Rotational .... elocities as well as hydrogen and he Jlum Ine I'ntensities of .' have been one hundred. and twelve members of the Scorplo-Centaurus aSSOclatlO~ . b h derived. For stars with M~ < 0'0, the distribution of rotational velocitieS of °lt are SJlnlar the upper Scorplus subgroup and the upper Centaurus-Lupus Su b grou P 1 . I and closely resemble those of the field stars. Stars with M, > O' 0, all of w lie 1 are found in th.e dense upper Scorpius region, rotate much faster than their counter parts amongst field stars, the Pleiades and Alpha-Persei cluster members. The measured equivalent width of H'Y for 77 stars provide a distance nlOd~\U~ of 6·0±0·09 magnitudes for the association. Evolutionary effects in the del1;~e hydrogen line intensities are found between the two subgroups. The hydrogen- me intensities at all spectral types in the upper Centaurus-Lupus subgroup are systematically smaller than thOse of members in the upper Scorpius subgrouP. Analysis of high dispersion spectra of five members of the association y.ield a helium abundance of Nae(N. = 0·096 ± 0 004. Along with data available In the literature, the mean helium abundance of thirteen stars of this association is found to be 0·098 :±: O· 004 by number. For the two main subgroups of this association, we deflve a value of 0 105 ± 0 001 for the upper Centaurus-Lupus group from three stars and 0·096 ± 0·005 for the upper Scorpius group from ten stars. -
Occurrence and Core-Envelope Structure of 1–4× Earth-Size Planets Around Sun-Like Stars
Occurrence and core-envelope structure of 1–4× SPECIAL FEATURE Earth-size planets around Sun-like stars Geoffrey W. Marcya,1, Lauren M. Weissa, Erik A. Petiguraa, Howard Isaacsona, Andrew W. Howardb, and Lars A. Buchhavec aDepartment of Astronomy, University of California, Berkeley, CA 94720; bInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822; and cHarvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138 Edited by Adam S. Burrows, Princeton University, Princeton, NJ, and accepted by the Editorial Board April 16, 2014 (received for review January 24, 2014) Small planets, 1–4× the size of Earth, are extremely common planets. The Doppler reflex velocity of an Earth-size planet − around Sun-like stars, and surprisingly so, as they are missing in orbiting at 0.3 AU is only 0.2 m s 1, difficult to detect with an − our solar system. Recent detections have yielded enough informa- observational precision of 1 m s 1. However, such Earth-size tion about this class of exoplanets to begin characterizing their planets show up as a ∼10-sigma dimming of the host star after occurrence rates, orbits, masses, densities, and internal structures. coadding the brightness measurements from each transit. The Kepler mission finds the smallest planets to be most common, The occurrence rate of Earth-size planets is a major goal of as 26% of Sun-like stars have small, 1–2 R⊕ planets with orbital exoplanet science. With three years of Kepler photometry in periods under 100 d, and 11% have 1–2 R⊕ planets that receive 1–4× hand, two groups worked to account for the detection biases in the incident stellar flux that warms our Earth. -
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).