Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa

Total Page:16

File Type:pdf, Size:1020Kb

Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966- Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. Launius . .1 Introduction . .11 1958 . .17 1) Able 1 / “Pioneer 0” . .17 2) no name / [Luna] . .17 3) Able 2 / “Pioneer 0” . .18 4) no name / [Luna] . .18 5) Pioneer 2 . .18 6) no name / [Luna] . .19 7) Pioneer 3 . .19 1959 . .21 8) Cosmic Rocket . .21 9) Pioneer 4 . .22 10) no name / [Luna] . .22 11) Second Cosmic Rocket . .23 12) Automatic Interplanetary Station . .23 13) Able IVB / “Pioneer” . .23 1960 . .25 14) Pioneer 5 . .25 15) no name / [Luna] . .25 16) no name / [Luna] . .26 17) Able VA / “Pioneer” . .26 18) no name / [Mars] . .26 19) no name / [Mars] . .27 20) Able VB / “Pioneer” . .27 1961 . .29 21) Tyazhelyy Sputnik / [Venera] . .29 22) Venera . .29 23) Ranger 1 . .31 24) Ranger 2 . .31 1962 . .33 25) Ranger 3 . .33 26) Ranger 4 . .33 27) Mariner 1 . .34 28) no name / [Venera] . .34 29) Mariner 2 . .34 30) no name / [Venera] . .35 31) no name / [Venera] . .35 32) Ranger 5 . .35 33) no name / [Mars] . .36 34) Mars 1 . .36 35) no name / [Mars] . .37 Table of Contents i 1963 . .39 36) no name / [Luna] . .39 37) no name / [Luna] . .39 38) Luna 4 . .40 39) Kosmos 21 / [Zond] . .40 1964 . .41 40) Ranger 6 . .41 41) no name / [Zond] . .41 42) no name / [Luna] . .42 43) Kosmos 27 / [Zond] . .42 44) Zond 1 . .42 45) no name / [Luna] . .43 46) Ranger 7 . .43 47) Mariner 3 . .43 48) Mariner 4 . .44 49) Zond 2 . ..
Recommended publications
  • Master Table of All Deep Space, Lunar, and Planetary Probes, 1958–2000 Official Name Spacecraft / 1958 “Pioneer” Mass[Luna] No
    Deep Space Chronicle: Master Table of All Deep Space, Lunar, and Planetary Probes, 1958–2000 Official Spacecraft / Mass Launch Date / Launch Place / Launch Vehicle / Nation / Design & Objective Outcome* Name No. Time Pad No. Organization Operation 1958 “Pioneer” Able 1 38 kg 08-17-58 / 12:18 ETR / 17A Thor-Able I / 127 U.S. AFBMD lunar orbit U [Luna] Ye-1 / 1 c. 360 kg 09-23-58 / 09:03:23 NIIP-5 / 1 Luna / B1-3 USSR OKB-1 lunar impact U Pioneer Able 2 38.3 kg 10-11-58 / 08:42:13 ETR / 17A Thor-Able I / 130 U.S. NASA / AFBMD lunar orbit U [Luna] Ye-1 / 2 c. 360 kg 10-11-58 / 23:41:58 NIIP-5 / 1 Luna / B1-4 USSR OKB-1 lunar impact U Pioneer 2 Able 3 39.6 kg 11-08-58 / 07:30 ETR / 17A Thor-Able I / 129 U.S. NASA / AFBMD lunar orbit U [Luna] Ye-1 / 3 c. 360 kg 12-04-58 / 18:18:44 NIIP-5 / 1 Luna / B1-5 USSR OKB-1 lunar impact U Pioneer 3 - 5.87 kg 12-06-58 / 05:44:52 ETR / 5 Juno II / AM-11 U.S. NASA / ABMA lunar flyby U 1959 Luna 1 Ye-1 / 4 361.3 kg 01-02-59 / 16:41:21 NIIP-5 / 1 Luna / B1-6 USSR OKB-1 lunar impact P Master Table of All Deep Space, Lunar, andPlanetary Probes1958–2000 ofAllDeepSpace,Lunar, Master Table Pioneer 4 - 6.1 kg 03-03-59 / 05:10:45 ETR / 5 Juno II / AM-14 U.S.
    [Show full text]
  • Solar-Wind Proton Access Deep Into the Near-Moon Wake M
    GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L16103, doi:10.1029/2009GL039444, 2009 Click Here for Full Article Solar-wind proton access deep into the near-Moon wake M. N. Nishino,1 M. Fujimoto,1 K. Maezawa,1 Y. Saito,1 S. Yokota,1 K. Asamura,1 T. Tanaka,1 H. Tsunakawa,2 M. Matsushima,2 F. Takahashi,2 T. Terasawa,2 H. Shibuya,3 and H. Shimizu4 Received 3 June 2009; revised 22 July 2009; accepted 24 July 2009; published 28 August 2009. [1] We study solar wind (SW) entry deep into the near- wake were not known because there were no observation Moon wake using SELENE (KAGUYA) data. It has been data. Recently, a Japanese lunar orbiter SELENE known that SW protons flowing around the Moon access (KAGUYA) performed comprehensive measurements of the central region of the distant lunar wake, while their the plasma and electromagnetic environment around the intrusion deep into the near-Moon wake has never been Moon; in particular, entry of SW protons into the near- expected. We show that SW protons sneak into the deepest Moon wake was found [Nishino et al., 2009]. The SW lunar wake (anti-subsolar region at 100 km altitude), and protons are accelerated by the bipolar electric field around that the entry yields strong asymmetry of the near-Moon the wake boundary and come into the near-Moon wake by wake environment. Particle trajectory calculations their Larmor motion in the direction perpendicular to the demonstrate that these SW protons are once scattered at IMF. This entry mechanism, which we call ‘Type-I entry’, the lunar dayside surface, picked-up by the SW motional lets the SW protons come fairly deep into the wake (solar electric field, and finally sneak into the deepest wake.
    [Show full text]
  • University of Iowa Instruments in Space
    University of Iowa Instruments in Space A-D13-089-5 Wind Van Allen Probes Cluster Mercury Earth Venus Mars Express HaloSat MMS Geotail Mars Voyager 2 Neptune Uranus Juno Pluto Jupiter Saturn Voyager 1 Spaceflight instruments designed and built at the University of Iowa in the Department of Physics & Astronomy (1958-2019) Explorer 1 1958 Feb. 1 OGO 4 1967 July 28 Juno * 2011 Aug. 5 Launch Date Launch Date Launch Date Spacecraft Spacecraft Spacecraft Explorer 3 (U1T9)58 Mar. 26 Injun 5 1(U9T68) Aug. 8 (UT) ExpEloxrpelro r1e r 4 1915985 8F eJbu.l y1 26 OEGxOpl o4rer 41 (IMP-5) 19697 Juunlye 2 281 Juno * 2011 Aug. 5 Explorer 2 (launch failure) 1958 Mar. 5 OGO 5 1968 Mar. 4 Van Allen Probe A * 2012 Aug. 30 ExpPloiorenre 3er 1 1915985 8M Oarc. t2. 611 InEjuxnp lo5rer 45 (SSS) 197618 NAouvg.. 186 Van Allen Probe B * 2012 Aug. 30 ExpPloiorenre 4er 2 1915985 8Ju Nlyo 2v.6 8 EUxpKlo 4r e(rA 4ri1el -(4IM) P-5) 197619 DJuenc.e 1 211 Magnetospheric Multiscale Mission / 1 * 2015 Mar. 12 ExpPloiorenre 5e r 3 (launch failure) 1915985 8A uDge.c 2. 46 EPxpiolonreeerr 4130 (IMP- 6) 19721 Maarr.. 313 HMEaRgCnIe CtousbpeShaetr i(cF oMxu-1ltDis scaatelell itMe)i ssion / 2 * 2021081 J5a nM. a1r2. 12 PionPeioenr e1er 4 1915985 9O cMt.a 1r.1 3 EExpxlpolorerer r4 457 ( S(IMSSP)-7) 19721 SNeopvt.. 1263 HMaalogSnaett oCsupbhee Sriact eMlluitlet i*scale Mission / 3 * 2021081 M5a My a2r1. 12 Pioneer 2 1958 Nov. 8 UK 4 (Ariel-4) 1971 Dec. 11 Magnetospheric Multiscale Mission / 4 * 2015 Mar.
    [Show full text]
  • Mars Express Orbiter Radio Science
    MaRS: Mars Express Orbiter Radio Science M. Pätzold1, F.M. Neubauer1, L. Carone1, A. Hagermann1, C. Stanzel1, B. Häusler2, S. Remus2, J. Selle2, D. Hagl2, D.P. Hinson3, R.A. Simpson3, G.L. Tyler3, S.W. Asmar4, W.I. Axford5, T. Hagfors5, J.-P. Barriot6, J.-C. Cerisier7, T. Imamura8, K.-I. Oyama8, P. Janle9, G. Kirchengast10 & V. Dehant11 1Institut für Geophysik und Meteorologie, Universität zu Köln, D-50923 Köln, Germany Email: [email protected] 2Institut für Raumfahrttechnik, Universität der Bundeswehr München, D-85577 Neubiberg, Germany 3Space, Telecommunication and Radio Science Laboratory, Dept. of Electrical Engineering, Stanford University, Stanford, CA 95305, USA 4Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91009, USA 5Max-Planck-Instuitut für Aeronomie, D-37189 Katlenburg-Lindau, Germany 6Observatoire Midi Pyrenees, F-31401 Toulouse, France 7Centre d’etude des Environnements Terrestre et Planetaires (CETP), F-94107 Saint-Maur, France 8Institute of Space & Astronautical Science (ISAS), Sagamihara, Japan 9Institut für Geowissenschaften, Abteilung Geophysik, Universität zu Kiel, D-24118 Kiel, Germany 10Institut für Meteorologie und Geophysik, Karl-Franzens-Universität Graz, A-8010 Graz, Austria 11Observatoire Royal de Belgique, B-1180 Bruxelles, Belgium The Mars Express Orbiter Radio Science (MaRS) experiment will employ radio occultation to (i) sound the neutral martian atmosphere to derive vertical density, pressure and temperature profiles as functions of height to resolutions better than 100 m, (ii) sound
    [Show full text]
  • Information Summaries
    TIROS 8 12/21/63 Delta-22 TIROS-H (A-53) 17B S National Aeronautics and TIROS 9 1/22/65 Delta-28 TIROS-I (A-54) 17A S Space Administration TIROS Operational 2TIROS 10 7/1/65 Delta-32 OT-1 17B S John F. Kennedy Space Center 2ESSA 1 2/3/66 Delta-36 OT-3 (TOS) 17A S Information Summaries 2 2 ESSA 2 2/28/66 Delta-37 OT-2 (TOS) 17B S 2ESSA 3 10/2/66 2Delta-41 TOS-A 1SLC-2E S PMS 031 (KSC) OSO (Orbiting Solar Observatories) Lunar and Planetary 2ESSA 4 1/26/67 2Delta-45 TOS-B 1SLC-2E S June 1999 OSO 1 3/7/62 Delta-8 OSO-A (S-16) 17A S 2ESSA 5 4/20/67 2Delta-48 TOS-C 1SLC-2E S OSO 2 2/3/65 Delta-29 OSO-B2 (S-17) 17B S Mission Launch Launch Payload Launch 2ESSA 6 11/10/67 2Delta-54 TOS-D 1SLC-2E S OSO 8/25/65 Delta-33 OSO-C 17B U Name Date Vehicle Code Pad Results 2ESSA 7 8/16/68 2Delta-58 TOS-E 1SLC-2E S OSO 3 3/8/67 Delta-46 OSO-E1 17A S 2ESSA 8 12/15/68 2Delta-62 TOS-F 1SLC-2E S OSO 4 10/18/67 Delta-53 OSO-D 17B S PIONEER (Lunar) 2ESSA 9 2/26/69 2Delta-67 TOS-G 17B S OSO 5 1/22/69 Delta-64 OSO-F 17B S Pioneer 1 10/11/58 Thor-Able-1 –– 17A U Major NASA 2 1 OSO 6/PAC 8/9/69 Delta-72 OSO-G/PAC 17A S Pioneer 2 11/8/58 Thor-Able-2 –– 17A U IMPROVED TIROS OPERATIONAL 2 1 OSO 7/TETR 3 9/29/71 Delta-85 OSO-H/TETR-D 17A S Pioneer 3 12/6/58 Juno II AM-11 –– 5 U 3ITOS 1/OSCAR 5 1/23/70 2Delta-76 1TIROS-M/OSCAR 1SLC-2W S 2 OSO 8 6/21/75 Delta-112 OSO-1 17B S Pioneer 4 3/3/59 Juno II AM-14 –– 5 S 3NOAA 1 12/11/70 2Delta-81 ITOS-A 1SLC-2W S Launches Pioneer 11/26/59 Atlas-Able-1 –– 14 U 3ITOS 10/21/71 2Delta-86 ITOS-B 1SLC-2E U OGO (Orbiting Geophysical
    [Show full text]
  • Lunar Ionosphere Exploration Method Using Auroral Kilometric Radiation
    Earth Planets Space, 63, 47–56, 2011 Lunar ionosphere exploration method using auroral kilometric radiation Yoshitaka Goto1, Takamasa Fujimoto1, Yoshiya Kasahara1, Atsushi Kumamoto2, and Takayuki Ono2 1Kanazawa University, Kanazawa, Japan 2Tohoku University, Sendai, Japan (Received June 3, 2009; Revised November 10, 2010; Accepted January 14, 2011; Online published February 21, 2011) The evidence of a lunar ionosphere provided by radio occultation experiments performed by the Soviet spacecraft Luna 19 and 22 has been controversial for the past three decades because the observed large density is difficult to explain theoretically without magnetic shielding from the solar wind. The KAGUYA mission provided an opportunity to investigate the lunar ionosphere with another method. The natural plasma wave receiver (NPW) and waveform capture (WFC) instruments, which are subsystems of the lunar radar sounder (LRS) on board the lunar orbiter KAGUYA, frequently observe auroral kilometric radiation (AKR) propagating from the Earth. The dynamic spectra of the AKR sometimes exhibit a clear interference pattern that is caused by phase differences between direct waves and waves reflected on a lunar surface or a lunar ionosphere if it exists. It was hypothesized that the electron density profiles above the lunar surface could be evaluated by comparing the observed interference pattern with the theoretical interference patterns constructed from the profiles with ray tracing. This method provides a new approach to examining the lunar ionosphere that does not involve the conventional radio occultation technique. Key words: KAGUYA, lunar ionosphere, auroral kilometric radiation. 1. Introduction 2001; Kurata et al., 2005). The dense plasma layers may The lunar atmosphere is extremely tenuous compared to be maintained by these strong fields.
    [Show full text]
  • The Mathematics of the Chinese, Indian, Islamic and Gregorian Calendars
    Heavenly Mathematics: The Mathematics of the Chinese, Indian, Islamic and Gregorian Calendars Helmer Aslaksen Department of Mathematics National University of Singapore [email protected] www.math.nus.edu.sg/aslaksen/ www.chinesecalendar.net 1 Public Holidays There are 11 public holidays in Singapore. Three of them are secular. 1. New Year’s Day 2. Labour Day 3. National Day The remaining eight cultural, racial or reli- gious holidays consist of two Chinese, two Muslim, two Indian and two Christian. 2 Cultural, Racial or Religious Holidays 1. Chinese New Year and day after 2. Good Friday 3. Vesak Day 4. Deepavali 5. Christmas Day 6. Hari Raya Puasa 7. Hari Raya Haji Listed in order, except for the Muslim hol- idays, which can occur anytime during the year. Christmas Day falls on a fixed date, but all the others move. 3 A Quick Course in Astronomy The Earth revolves counterclockwise around the Sun in an elliptical orbit. The Earth ro- tates counterclockwise around an axis that is tilted 23.5 degrees. March equinox June December solstice solstice September equinox E E N S N S W W June equi Dec June equi Dec sol sol sol sol Beijing Singapore In the northern hemisphere, the day will be longest at the June solstice and shortest at the December solstice. At the two equinoxes day and night will be equally long. The equi- noxes and solstices are called the seasonal markers. 4 The Year The tropical year (or solar year) is the time from one March equinox to the next. The mean value is 365.2422 days.
    [Show full text]
  • Misiones Espaciales Misiones Que Año Nación Lanzador Síntesis De La Misión Recorrido Lo Visitaron
    Una vez finalizada la Segunda Guerra Mundial, Estados Unidos y la Unión Soviética se enfrentaron ideológica y políticamente. El campo de batalla de los dos bloques fue llamado Guerra fría. Las dos super potencias se embarcaron en una carrera por la conquista del espacio en un despliegue de poderío científico, militar y tecnológico. En un comienzo los mayores éxitos fueron de la URSS pero fue EE UU el que logró llevar seres humanos a la Luna. Luego de ese suceso, pasaron varios años hasta que otros países lograron el sueño de llegar a nuestro satélite. LMiUNsiones espacAiales En la actual carrera espacial ingresan nuevos proyectos financiados de manera privada. Las misiones que tuvieron éxito en llegar a la Luna se pueden dividir en: las que sobrevolaron, las que orbitaron, las que descendieron con robots y las que lograron llevar humanos Sobrevuelos/Orbitadores: Luna | Ranger | Zond| Lunar Orbiter | Explorer | Clementine | Lunar prospector | Smart | Kaguya Selene|Chang`e| Chandrayaan| Lunar reconnaissance|Grail| Ladee Landers y Rovers: Luna 9| Surveyour|Luna13|Luna 16/20/24| Luna 17|Lunakhod|Yutu Misiones tripuladas: Apollo 8/10/11/12/14/15/16/17 Fuente: http://mars.jpl.nasa.gov/programmissions/missions/ Planetario de Buenos AiresPlanetario de la Ciudad de Buenos Aires Galileo Galilei - Av. Sarmiento y B. Roldán - Tel. 4772-9265 / 4771-6629 - e-mail: [email protected] 1/6 Misiones espaciales Misiones que año Nación Lanzador Síntesis de la misión Recorrido lo visitaron Objetivo: Impactar Sobrevoló la Luna. Luego ingresó en órbita al Sol R-7 Logros : Fue el primer vehículo en escapar de la gravedad Enero Unión terrestre.
    [Show full text]
  • Geochronology Database for Central Colorado
    Geochronology Database for Central Colorado Data Series 489 U.S. Department of the Interior U.S. Geological Survey Geochronology Database for Central Colorado By T.L. Klein, K.V. Evans, and E.H. DeWitt Data Series 489 U.S. Department of the Interior U.S. Geological Survey U.S. Department of the Interior KEN SALAZAR, Secretary U.S. Geological Survey Marcia K. McNutt, Director U.S. Geological Survey, Reston, Virginia: 2010 For more information on the USGS—the Federal source for science about the Earth, its natural and living resources, natural hazards, and the environment, visit http://www.usgs.gov or call 1-888-ASK-USGS For an overview of USGS information products, including maps, imagery, and publications, visit http://www.usgs.gov/pubprod To order this and other USGS information products, visit http://store.usgs.gov Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. Although this report is in the public domain, permission must be secured from the individual copyright owners to reproduce any copyrighted materials contained within this report. Suggested citation: T.L. Klein, K.V. Evans, and E.H. DeWitt, 2009, Geochronology database for central Colorado: U.S. Geological Survey Data Series 489, 13 p. iii Contents Abstract ...........................................................................................................................................................1 Introduction.....................................................................................................................................................1
    [Show full text]
  • Radial Variation of the Interplanetary Magnetic Field Between 0.3 AU and 1.0 AU
    |00000575|| J. Geophys. 42, 591 - 598, 1977 Journal of Geophysics Radial Variation of the Interplanetary Magnetic Field between 0.3 AU and 1.0 AU Observations by the Helios-I Spacecraft G. Musmann, F.M. Neubauer and E. Lammers Institut for Geophysik and Meteorologie, Technische Universitiit Braunschweig, Mendelssohnstr. lA, D-3300 Braunschweig, Federal Republic of Germany Abstract. We have investigated the radial dependence of the radial and azimuthal components and the magnitude of the interplanetary magnetic field obtained by the Technical University of Braunschweig magnetometer experiment on-board of Helios-1 from December 10, 1974 to first perihelion on March 15, 1975. Absolute values of daily averages of each quantity have been employed. The regression analysis based on power laws leads to 2.55 y x r- 2 · 0 , 2.26 y x r- i.o and F = 5.53 y x r- i. 6 with standard deviations of 2.5 y, 2.0 y and 3.2 y for the radial and azimuthal components and magnitude, respectively. Here r is the radial distance from the sun in astronomical units. The results are compared with results obtained for Mariners 4, 5 and 10 and Pioneers 6 and 10. The differences are probably due to different epochs in the solar cycle and the different statistical techniques used. Key words: Interplanetary magnetic field - Helios-1 results. Introduction The study of the vanat10n of the components and magnitude of the in­ terplanetary magnetic field with heliocentric distance is very intersting at the present time. The mission of Mariner 10 to the inner solar system to a heliocentric distance of 0.46 AU and the missions of Pioneer 10 and Pioneer 11 to the outer solar system to heliocentric distances beyond 5 AU have provided new data over a wide range of heliocentric distance.
    [Show full text]
  • The Calendars of India
    The Calendars of India By Vinod K. Mishra, Ph.D. 1 Preface. 4 1. Introduction 5 2. Basic Astronomy behind the Calendars 8 2.1 Different Kinds of Days 8 2.2 Different Kinds of Months 9 2.2.1 Synodic Month 9 2.2.2 Sidereal Month 11 2.2.3 Anomalistic Month 12 2.2.4 Draconic Month 13 2.2.5 Tropical Month 15 2.2.6 Other Lunar Periodicities 15 2.3 Different Kinds of Years 16 2.3.1 Lunar Year 17 2.3.2 Tropical Year 18 2.3.3 Siderial Year 19 2.3.4 Anomalistic Year 19 2.4 Precession of Equinoxes 19 2.5 Nutation 21 2.6 Planetary Motions 22 3. Types of Calendars 22 3.1 Lunar Calendar: Structure 23 3.2 Lunar Calendar: Example 24 3.3 Solar Calendar: Structure 26 3.4 Solar Calendar: Examples 27 3.4.1 Julian Calendar 27 3.4.2 Gregorian Calendar 28 3.4.3 Pre-Islamic Egyptian Calendar 30 3.4.4 Iranian Calendar 31 3.5 Lunisolar calendars: Structure 32 3.5.1 Method of Cycles 32 3.5.2 Improvements over Metonic Cycle 34 3.5.3 A Mathematical Model for Intercalation 34 3.5.3 Intercalation in India 35 3.6 Lunisolar Calendars: Examples 36 3.6.1 Chinese Lunisolar Year 36 3.6.2 Pre-Christian Greek Lunisolar Year 37 3.6.3 Jewish Lunisolar Year 38 3.7 Non-Astronomical Calendars 38 4. Indian Calendars 42 4.1 Traditional (Siderial Solar) 42 4.2 National Reformed (Tropical Solar) 49 4.3 The Nānakshāhī Calendar (Tropical Solar) 51 4.5 Traditional Lunisolar Year 52 4.5 Traditional Lunisolar Year (vaisnava) 58 5.
    [Show full text]
  • Arxiv:1912.04482V1 [Physics.Space-Ph] 10 Dec 2019
    manuscript submitted to Radio Science Measuring the Earth's Synchrotron Emission from Radiation Belts with a Lunar Near Side Radio Array Alexander Hegedus1, Quentin Nenon2, Antoine Brunet3, Justin Kasper1, Ang´elicaSicard3, Baptiste Cecconi4, Robert MacDowall5, Daniel Baker6 1University of Michigan, Department of Climate and Space Sciences and Engineering, Ann Arbor, Michigan, USA 2Space Sciences Laboratory, University of California, Berkeley, CA, USA 3ONERA / DPHY, Universit´ede Toulouse, F-31055 Toulouse France 4LESIA, Observatoire de Paris, Universit PSL, CNRS, Sorbonne Universit, Univ. de Paris, Meudon, France 5NASA Goddard Space Flight Center, Greenbelt, MD, USA 6University of Colorado Boulder, Laboratory for Atmospheric and Space Physics, Boulder, Colorado, USA Key Points: • Synchrotron emission between 500-1000 kHz has a total flux density of 1.4-2 Jy at lunar distances • A 10 km radio array with 16000 elements could detect the emission in 12-24 hours with moderate noise • Changing electron density can make detections 10x faster at lunar night, 10x slower at lunar noon arXiv:1912.04482v1 [physics.space-ph] 10 Dec 2019 Corresponding author: Alexander Hegedus, [email protected] {1{ manuscript submitted to Radio Science Abstract The high kinetic energy electrons that populate the Earth's radiation belts emit synchrotron emissions because of their interaction with the planetary magnetic field. A lunar near side array would be uniquely positioned to image this emission and provide a near real time measure of how the Earth's radiation belts are responding to the current solar in- put. The Salammb^ocode is a physical model of the dynamics of the three-dimensional phase-space electron densities in the radiation belts, allowing the prediction of 1 keV to 100 MeV electron distributions trapped in the belts.
    [Show full text]