Instruction Manual Meade Instruments Corporation

Total Page:16

File Type:pdf, Size:1020Kb

Instruction Manual Meade Instruments Corporation Instruction Manual 7" LX200 Maksutov-Cassegrain Telescope 8", 10", and 12" LX200 Schmidt-Cassegrain Telescopes Meade Instruments Corporation NOTE: Instructions for the use of optional accessories are not included in this manual. For details in this regard, see the Meade General Catalog. (2) (1) (1) (2) Ray (2) 1/2° Ray (1) 8.218" (2) 8.016" (1) 8.0" Secondary 8.0" Mirror Focal Plane Secondary Primary Baffle Tube Baffle Field Stops Correcting Primary Mirror Plate The Meade Schmidt-Cassegrain Optical System (Diagram not to scale) In the Schmidt-Cassegrain design of the Meade 8", 10", and 12" models, light enters from the right, passes through a thin lens with 2-sided aspheric correction (“correcting plate”), proceeds to a spherical primary mirror, and then to a convex aspheric secondary mirror. The convex secondary mirror multiplies the effective focal length of the primary mirror and results in a focus at the focal plane, with light passing through a central perforation in the primary mirror. The 8", 10", and 12" models include oversize 8.25", 10.375" and 12.375" primary mirrors, respectively, yielding fully illuminated fields- of-view significantly wider than is possible with standard-size primary mirrors. Note that light ray (2) in the figure would be lost entirely, except for the oversize primary. It is this phenomenon which results in Meade 8", 10", and 12" Schmidt-Cassegrains having off-axis field illuminations 10% greater, aperture-for-aperture, than other Schmidt-Cassegrains utilizing standard-size primary mirrors. The optical design of the 4" Model 2045D is almost identical but does not include an oversize primary, since the effect in this case is small. LX200 Schmidt-Cassegrain telescopes now feature new baffle tube designs. These computer-optimized designs incorporate a series of 7 to 11 (depending on the focal ratio and size of the LX200) internal field-stops to eliminate almost all internal reflections, yielding the best image contrast available in any Schmidt-Cassegrain available today. Field Stops 8.25" 7" Focal Plane Primary Baffle Tube Secondary Baffle Primary Mirror (f/2.5) The Meade 7” Maksutov-Cassegrain Optical System (Diagram not to scale) The Meade 7" Maksutov-Cassegrain design optimizes imaging performance by utilizing a combination of two-sided spherical meniscus lens (right), a strongly aspheric f/2.5 primary mirror, and a spherical secondary mirror. The convex secondary mirror multiplies the effective focal length of the primary by a factor of six, resulting in an overall f/15 system at the Cassegrain focus. The oversize 8.25" primary mirror results in a fully-illuminated (unvignetted) field of view significantly wider than can be obtained with Maksutov optics incorporating primary mirrors of the same aperture as their meniscus correcting lenses. Computer-optimized primary and secondary mirror baffles, as well as a sequence of field stops internal to the primary mirror baffle, yield lunar, planetary, stellar, and deep-space images of uncommonly high contrast and resolution. - 3 - 0 WARNING! 0 Never use the LX200 telescope to look at the Sun! Looking at or near the Sun will cause instant and irreversible damage to your eye. Eye damage is often painless, so there is no warning to the observer that damage has occurred until it is too late. Do not point the telescope or its viewfinder at or near the Sun. Do not look through the telescope or its viewfinder as it is moving. Children should always have adult supervision while observing. 1 18 2 14 3 13 4 6 5 12 7 8 9 10 11 15 16 17 Fig. 1: 8” LX200 Telescope. Captions for Figure 1 1. Viewfinder Dew Shield 10. Right Ascension Setting Circle 2. Viewfinder Collimation Screws 11. Power Panel 3. Declination (Dec) Setting Circle 12. Keypad Hand Controller 4. Declination Pointer 13. Diagonal Mirror 5. Focus Knob 14. Eyepiece 6. Eyepiece Holder 15. Bubble Level 7. Right Ascension (R.A) Lock 16. Hour Angel (HA) Pointer 8. Right Ascension Slow-Motion Controls 17. Drive Base 9. Right Ascension Vernier Pointer 18. Viewfinder Focus Lock Ring - 4 - Contents 7" LX200 Maksutov-Cassegrain Telescope 8”, 10”, & 12" LX200 Schmidt-Cassegrain Telescope Introduction. 5 Mode Functions . 16 1. What is the LX200? An Overview . 5 1. Mode 1: Telescope/Object Library . 16 a. Heavy-Duty Mounts . 5 a. Telescope Menu File . 16 b. Built-In 64,359 Object Library. 5 b. Object Library Menu File . 20 c. Altazimuth Mode Operation . 5 2. Mode 2: Coordinates/GO TO . 22 d. Terrestrial Operation. 5 a. Coordinates Menu File . 22 e. Keypad and Power Panel Functions . 5 b. GO TO Menu Option . 22 2. Standard Equipment. 5 3. Mode 3: Clock/Calendar. 22 Unpacking and Inspection . 6 4. Mode 4: TIMER/FREQ . 22 1. What You Should Have . 6 a. TIMER = Menu Option . 23 2. Please Look Everything Over. 6 b. FREQ = Menu Option. 22 3. Inspecting the Optics . 6 5. Mode 5: Keypad Off/Brightness Adjust . 23 4. Caution: All LX200 Owners . 6 Magnification and Field of View . 24 5. Caution: 10” and 12” LX200 Owners . 6 1. Magnification . 24 6. Keypad Version Number . 6 2. Apparent Field and Actual Field . 24 Telescope Assembly . 7 Appendix A: Equatorial Wedge. 25 1. The Field Tripod . 7 1. 8” Equatorial Wedge. 25 2. Mounting the Viewfinder. 8 a. Azimuth Control . 25 a. Attaching the Viewfinder. 8 b. Deluxe Latitude Adjuster . 25 b. Focusing the Viewfinder . 8 2. Superwedge . 26 c. Collimating the Viewfinder . 8 3. Mounting the Telescope . 26 3. Attaching the Diagonal Mirror and Eyepiece . 8 4. Magnetic Compass. 27 4. Collimation . 8 a. Setting Magnetic Declination . 27 5. 12” Tube Swing-Through Limits . 8 b. Compass Installation . 27 6. 7” Tube Swing-Through Limit . 8 c. Finding True North . 28 7. Maksutov Fan. 8 Appendix B: Equatorial Use . 29 Quick Start . 9 1. Celestial Coordinates . 29 1. Using the LX200 Manually . 9 2. Lining Up with the Celestial Pole . 29 2. Using the LX200 in LAND . 9 3. Precise Polar Alignment . 30 3. Using the LX200 in ALTAZ . 10 Appendix C: Star Library and Star Charts . 31 a. Entering Basic Information . 10 1. Alignment Stars . 31 b. Location of the Observing Site. 10 2. Star Charts . 32 c. Local Time and Date . 11 d. Setting Up the Telescope . 11 Appendix D: Object Library . 34 e. Using the MODE key . 12 1. The LX200 64,359 Object Library . 34 f. Library Object Keys . 13 a. SAO Catalog. 34 4. Star Alignment . 13 b. UGC Catalog . 34 a. 1-Star with Known SITE . 13 c. CNGC Catalog . 34 b. 2-Star with Known SITE . 13 d. IC Catalog. 35 c. Unknown SITE . 13 e. GCVS Catalog . 35 d. Which Alignment Method to Use . 13 f. Star Catalog . 35 g. M (Messier) Catalog . 35 The LX200 Keypad Hand Controller . 14 h. Planet Catalog . 35 1. ENTER Key . 14 2. CNGC Catalog . 36 2. MODE Key . 14 3. STAR Catalog. 43 3. GO TO Key. 14 4. M (Messier) Catalog . 49 4. Direction Keys . 14 5. Speed Keys . 14 Appendix E: Maintaining Your LX200. 51 6. RET Key . 14 1. Keeping Your Telescope Clean . 51 7. FOCUS Key . 15 2. Collimation of the Optical System . 52 8. MAP Key. 15 3. Right Ascension Lock . 53 9. Object Keys . 15 4. Behind the Power Panel. 53 10.PREV and NEXT Keys . 15 5. Factory Servicing and Repairs ..
Recommended publications
  • Arxiv:2012.09981V1 [Astro-Ph.SR] 17 Dec 2020 2 O
    Contrib. Astron. Obs. Skalnat´ePleso XX, 1 { 20, (2020) DOI: to be assigned later Flare stars in nearby Galactic open clusters based on TESS data Olga Maryeva1;2, Kamil Bicz3, Caiyun Xia4, Martina Baratella5, Patrik Cechvalaˇ 6 and Krisztian Vida7 1 Astronomical Institute of the Czech Academy of Sciences 251 65 Ondˇrejov,The Czech Republic(E-mail: [email protected]) 2 Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, 119234, Moscow, Russia 3 Astronomical Institute, University of Wroc law, Kopernika 11, 51-622 Wroc law, Poland 4 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotl´aˇrsk´a2, 611 37 Brno, Czech Republic 5 Dipartimento di Fisica e Astronomia Galileo Galilei, Vicolo Osservatorio 3, 35122, Padova, Italy, (E-mail: [email protected]) 6 Department of Astronomy, Physics of the Earth and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University in Bratislava, Mlynsk´adolina F-2, 842 48 Bratislava, Slovakia 7 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary Received: September ??, 2020; Accepted: ????????? ??, 2020 Abstract. The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type ob- jects. Of all flares, 63 % were detected in sample of cool stars (Teff < 5000 K), and 29 % { in stars of spectral type G, while 23 % in K-type stars and ap- proximately 34% of all detected flares are in M-type stars.
    [Show full text]
  • Spring Fever Strikes
    The MARCH 2002 DENVER OBSERVER Newsletter of the Denver Astronomical Society One Mile Nearer the Stars How Many in One Night?? Gearing up for the Messier Marathon? Those folks who are new to astronomy may not yet be able to relate to the sheer joy of braving the early-spring temperatures (brrrrr) for a full night (and morning—I’m talking dusk to dawn, here) of observing some of the most beautiful objects in the heavens. Why now? Because for only a few weeks during the year is it possible to see all of the Messier objects in one night. Astronomers will dig in their heels and tripods, get out the star charts (See Page 7), and knock off one object after the next. Some people actually catalog 70 of the available 110 targets and submit their achievements to the Astronomical League for the coveted Messier Certificate. Others just like to look at the beautiful celestial wonders like the one in the photo to the left. Either way, get out to the The Pleaides (M45) DSS on the weekend of the 15th and enjoy Image © Joe Gafford, 2002 the views!—PK Spring Fever Strikes President’s Corner .......... 2 MARCH SKIES 2002 f you’ve been reading your astronomy magazines, you know that by month’s Schedule of Events ......... 2 Iend, four naked-eye planets will grace the night skies. Jupiter is the main show-stopper but Saturn, Mars, and finally Venus will sparkle for all, moon or no moon. Remember that a Officers ......................... 2 little high-cloud haze can be good for telescopic planet observations.
    [Show full text]
  • 02 Southern Cross
    Asterism Southern Cross The Southern Cross is located in the constellation Crux, the smallest of the 88 constellations. It is one of the most distinctive. With the four stars Mimosa BeCrux, Ga Crux, A Crux and Delta Crucis, forming the arms of the cross. The Southern Cross was also used as a remarkably accurate timepiece by all the people of the southern hemisphere, referred to as the ‘Southern Celestial Clock’ by the portuguese naturalist Cristoval D’Acosta. It is perpendicular as it passes the meridian, and the exact time can thus be calculated visually from its angle. The german explorer Baron Alexander von Humboldt, sailing across the southern oceans in 1799, wrote: “It is a timepiece, which advances very regularly nearly 4 minutes a day, and no other group of stars affords to the naked eye an observation of time so easily made”. Asterism - An asterism is a distinctive pattern of stars or a distinctive group of stars in the sky. Constellation - A grouping of stars that make an imaginary picture in the sky. There are 88 constellations. The stars and objects nearby The Main-Themes in asterism Southern Cross Southern Cross Ga Crux A Crux Mimosa, Be Crux Delta Crucis The Motives in asterism Southern Cross Crucis A Bayer / Flamsteed indication AM Arp+Madore - A Catalogue of Southern peculiar Galaxies and Associations [B10] Boss, 1910 - Preliminary General Catalogue of 6188 Stars C Cluster CCDM Catalogue des composantes d’étoiles doubles et multiples CD Cordoba Durchmusterung Declination Cel Celescope Catalog of ultraviolet Magnitudes CPC
    [Show full text]
  • Observing List
    day month year Epoch 2000 local clock time: 23.98 Observing List for 23 7 2019 RA DEC alt az Constellation object mag A mag B Separation description hr min deg min 20 50 Andromeda Gamma Andromedae (*266) 2.3 5.5 9.8 yellow & blue green double star 2 3.9 42 19 28 69 Andromeda Pi Andromedae 4.4 8.6 35.9 bright white & faint blue 0 36.9 33 43 30 55 Andromeda STF 79 (Struve) 6 7 7.8 bluish pair 1 0.1 44 42 16 52 Andromeda 59 Andromedae 6.5 7 16.6 neat pair, both greenish blue 2 10.9 39 2 45 67 Andromeda NGC 7662 (The Blue Snowball) planetary nebula, fairly bright & slightly elongated 23 25.9 42 32.1 31 60 Andromeda M31 (Andromeda Galaxy) large sprial arm galaxy like the Milky Way 0 42.7 41 16 31 61 Andromeda M32 satellite galaxy of Andromeda Galaxy 0 42.7 40 52 32 60 Andromeda M110 (NGC205) satellite galaxy of Andromeda Galaxy 0 40.4 41 41 17 55 Andromeda NGC752 large open cluster of 60 stars 1 57.8 37 41 17 48 Andromeda NGC891 edge on galaxy, needle-like in appearance 2 22.6 42 21 45 69 Andromeda NGC7640 elongated galaxy with mottled halo 23 22.1 40 51 46 57 Andromeda NGC7686 open cluster of 20 stars 23 30.2 49 8 30 121 Aquarius 55 Aquarii, Zeta 4.3 4.5 2.1 close, elegant pair of yellow stars 22 28.8 0 -1 12 120 Aquarius 94 Aquarii 5.3 7.3 12.7 pale rose & emerald 23 19.1 -13 28 32 152 Aquarius M72 globular cluster 20 53.5 -12 32 31 151 Aquarius M73 Y-shaped asterism of 4 stars 20 59 -12 38 16 117 Aquarius NGC7606 Galaxy 23 19.1 -8 29 32 149 Aquarius NGC7009 Saturn Neb planetary nebula, large & bright pale green oval 21 4.2 -11 21.8 38 135
    [Show full text]
  • Curriculum Vitae - 24 March 2020
    Dr. Eric E. Mamajek Curriculum Vitae - 24 March 2020 Jet Propulsion Laboratory Phone: (818) 354-2153 4800 Oak Grove Drive FAX: (818) 393-4950 MS 321-162 [email protected] Pasadena, CA 91109-8099 https://science.jpl.nasa.gov/people/Mamajek/ Positions 2020- Discipline Program Manager - Exoplanets, Astro. & Physics Directorate, JPL/Caltech 2016- Deputy Program Chief Scientist, NASA Exoplanet Exploration Program, JPL/Caltech 2017- Professor of Physics & Astronomy (Research), University of Rochester 2016-2017 Visiting Professor, Physics & Astronomy, University of Rochester 2016 Professor, Physics & Astronomy, University of Rochester 2013-2016 Associate Professor, Physics & Astronomy, University of Rochester 2011-2012 Associate Astronomer, NOAO, Cerro Tololo Inter-American Observatory 2008-2013 Assistant Professor, Physics & Astronomy, University of Rochester (on leave 2011-2012) 2004-2008 Clay Postdoctoral Fellow, Harvard-Smithsonian Center for Astrophysics 2000-2004 Graduate Research Assistant, University of Arizona, Astronomy 1999-2000 Graduate Teaching Assistant, University of Arizona, Astronomy 1998-1999 J. William Fulbright Fellow, Australia, ADFA/UNSW School of Physics Languages English (native), Spanish (advanced) Education 2004 Ph.D. The University of Arizona, Astronomy 2001 M.S. The University of Arizona, Astronomy 2000 M.Sc. The University of New South Wales, ADFA, Physics 1998 B.S. The Pennsylvania State University, Astronomy & Astrophysics, Physics 1993 H.S. Bethel Park High School Research Interests Formation and Evolution
    [Show full text]
  • Exercise E1: Finding Your Way Around the Sky
    E – Star Finding Exercise E1: Finding Your Way Around the Sky Student name: ________________________ Class: ____________ Date: _____________ Check the box with the correct answer. Question 1: What is the orientation of the Big Dipper asterism in winter? a. It appears upside down. b. It sits with its handle downwards. c. It appears to sit upright, resting upon its bowl. d. The Big Dipper is not visible in the winter. Question 2: Polaris is part of which constellation? (Hint: Select Constellations from the Settings view to display IAU Boundaries and Show Names). a. Cepheus b. Draco c. Ursa Minor d. Ursa Major Question 3: What happens to the position of Polaris in your sky as time advances over a period of a year? a. It remains absolutely fixed, and does not change its position. b. The north celestial pole revolves about Polaris. c. It revolves in a very small circle around the north celestial pole. d. Its altitude changes by + and - 23.5 degrees throughout the year because of the tilt of the Earth's spin axis. Starry Night College Version 7 1 Question 4: What is the relationship between the altitude of Polaris and the latitude of the observer? a. There is no relationship between these two parameters. b. The altitude of Polaris is almost the same as the latitude of the observer. c. The altitude of Polaris is almost the equal to 90 degrees minus the latitude of the observer. d. The latitude equals the altitude of Polaris minus the altitude of the North celestial Pole. Question 5: What is the nearest star to the south celestial pole, as shown in the Main Window? (Hint: Use the Search facility to locate these stars and zoom in towards the SCP.
    [Show full text]
  • Binocular Challenge Here
    AHSP Binocular Observing Award Compiled by Phil Harrington www.philharrington.net • To qualify for the BOA pin, you must see 15 of the following 20 binocular targets. Check off each as you spot them. Seen # Object Const. Type* RA Dec Mag Size Nickname 1. M13 Her GC 16 41.7 +36 28 5.9 16' Great Hercules Globular 2. M57 Lyr PN 18 53.6 +33 02 9.7 86"x62" Ring Nebula 3. Collinder 399 Vul AS 19 25.4 +20 11 3.6 60' Coathanger/Brocchi’s Cluster 3.1 4. Albireo Cyg Dbl 19 30.7 +27 57 35” Color Contrasting Double 5.1 5. M27 Vul PN 19 59.6 +22 43 8.1 8’x6’ Dumbbell Nebula 6. NGC 6992 Cyg SNR 20 56.4 +31 43 - 60'x8 Veil Nebula (east) 7. NGC 7000 Cyg BN 20 58.8 +44 20 - 120'x100' North America Nebula 8. M15 Peg GC 21 30.0 +12 10 7.5 12’ Great Pegasus Cluster 9. M39 Cyg OC 21 32.2 +48 26 4.6 32' 10. Barnard 168 Cyg DN 21 53.2 +47 12 - 100'x10' West of Cocoon Nebula 11. IC 5146 Cyg BN/OC 21 53.5 +47 16 - 12'x12' Cocoon Nebula 12. M110 And Gx 00 40.4 +41 41 10 17’x10’ 13. M32 And Gx 00 42.8 +40 52 10 8’x6’ 14. M31 And Gx 00 42.8 +41 16 4.5 178’ Andromeda Galaxy 15. NGC 457 Cas OC 01 19.1 +58 20 6.4 13’ Owl Cluster/ET Cluster 16.
    [Show full text]
  • 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).
    [Show full text]
  • Abstract a Search for Extrasolar Planets Using Echoes Produced in Flare Events
    ABSTRACT A SEARCH FOR EXTRASOLAR PLANETS USING ECHOES PRODUCED IN FLARE EVENTS A detection technique for searching for extrasolar planets using stellar flare events is explored, including a discussion of potential benefits, potential problems, and limitations of the method. The detection technique analyzes the observed time versus intensity profile of a star’s energetic flare to determine possible existence of a nearby planet. When measuring the pulse of light produced by a flare, the detection of an echo may indicate the presence of a nearby reflective surface. The flare, acting much like the pulse in a radar system, would give information about the location and relative size of the planet. This method of detection has the potential to give science a new tool with which to further humankind’s understanding of planetary systems. Randal Eugene Clark May 2009 A SEARCH FOR EXTRASOLAR PLANETS USING ECHOES PRODUCED IN FLARE EVENTS by Randal Eugene Clark A thesis submitted in partial fulfillment of the requirements for the degree of Master of Science in Physics in the College of Science and Mathematics California State University, Fresno May 2009 © 2009 Randal Eugene Clark APPROVED For the Department of Physics: We, the undersigned, certify that the thesis of the following student meets the required standards of scholarship, format, and style of the university and the student's graduate degree program for the awarding of the master's degree. Randal Eugene Clark Thesis Author Fred Ringwald (Chair) Physics Karl Runde Physics Ray Hall Physics For the University Graduate Committee: Dean, Division of Graduate Studies AUTHORIZATION FOR REPRODUCTION OF MASTER’S THESIS X I grant permission for the reproduction of this thesis in part or in its entirety without further authorization from me, on the condition that the person or agency requesting reproduction absorbs the cost and provides proper acknowledgment of authorship.
    [Show full text]
  • Star Clusters
    Star Clusters Culpeper Astronomy Club (CAC) Meeting May 21, 2018 Overview • Introductions • Main Topic: Star Clusters - Open and Globular • Constellations: Bootes, Canes Venatici, Coma Berenices • Observing Session - TBD Observing Session – 29 April 18 • Kicked off at about 6:30 p.m • Ended at about 1:30 a.m • Set up several telescopes • Three refractor’s (RAS -7”, f/12) • 11” CPC 1100 SCT (Dennis) • 12” Meade SCT • Targets included: • Venus • Moon • Several double stars • Several deep sky objects • Jupiter • Checked out Saturn and Mars at after arriving home – 2:30 a.m. Loaner Telescopes Jupiter near Opposition • Taken on 13 May 2018 by Jerry Sykes (Opposition 8 May) • Taken with a 120mm refractor, 3x barlow and ASI224mc video camera • First time using his ASI224mc camera • Took several videos through breaks in the clouds • Shot 21,700 frames in a little over two minutes. • Used 29% of 21,700 frames • Captured using Sharpcap • Stacked in AS!3 • Processed in Registax6 Stellar Evolution - The Birth • Stars are born within the clouds of dust and gas scattered throughout most galaxies (Orion Nebula) • Swirling cloud gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction • As cloud collapses, material at the center heats up and begins gathering dust and gas (Protostar) • Spinning clouds may break up into two or three blobs resulting in paired or groups of multiple stars • Not all of this material ends up as part of a star — the remaining dust can become planets, asteroids,
    [Show full text]
  • 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
    [Show full text]
  • Celestial Gymnastics # 02
    PLANETARIUM EDUCATIONTM (Class Test) 9A Celestial Gymnastics # 02 www.leoplanetaria.com 9A Celestial Gymnastics 02 Max. Duration: 00min Max. Marks: 00 Date:____/____/______ TM Name: _______________________________ Class: ______ Sec: ________ Roll No:______ TM Planetarium Education www.leoplanetaria.com Tick (þ) mark the correct answer or fill in the blank. 1. The obvious choice reference of a central circle on a rotating ball’s surface as a starting or zero reference point of its latitudes is (A) North pole (B) South pole (C) Equator (D) Prime meridian 2. Which of the following point on the surface of a rotating ball when viewed from space is called its North Pole? (A) (B) 3. Which of the following diagram from a vantage point from where you have a bird’s eye view of the solar system is correct? (A) (B) 4. From where on the Earth over a period of one year you can see the entire celestial sphere – you would miss no star, no planet or any other object of the sky. (A) North pole (B) South pole (C) Equator (D) Prime meridian 5. Which constellation helps you find the pole star of the southern hemisphere of the Earth? (A) Crux (B) Ursa Major (C) Orion (D) Ursa Minor 6. The height of the pole star in our skies as we move from equator towards the poles... (A) Increases (B) Decreases (C) Remains unchanged 7. Prime Meridian passes through... (A) Allahabad (B) London (C) New York (D) Paris 8. Who laid the laws of motion for celestial bodies in space? (A) Kepler (B) Newton (C) Galileo (D) Copernicus Pg 1/3 C Leo Planetaria Astronomy Education Pvt.
    [Show full text]