Initiation of a Lightning Search Using the Lightning and Airglow Camera
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Observation of the Airglow from the ISS by the IMAP Mission *Y
2013/3/13(ANGWIN workshop, Tachikawa) Observation of the airglow from the ISS by the IMAP mission *Y. Akiya [1], A. Saito [1], T. Sakanoi [2], Y. Hozumi [1], A. Yamazaki [3], Y. Otsuka [4] [1] Graduation School of Science, Kyoto University , [2] PPARC, Tohoku University, [3] ISAS/JAXA, [4] STE Laboratory, Nagoya University ----- Outline ----- Introduction of the IMAP mission Visible and near-infrared spectrographic imager Samples of airglow observation by VISI Summary “ISS-IMAP” mission Ionosphere, Mesosphere, Upper atmosphere and Plasmasphere Imagers of the ISS-IMAP mapping mission from the mission International Space Station (ISS) Observational imagers were installed on the Exposure Facility of Japanese Experimental Module: August 9th, 2012. Initial checkout: August and September, 2012 Nominal observations: October, 2012 - [Pictures: Courtesy of JAXA/NASA] [this issue]. According to characteristics of airglow emissions, wavelength range from 630 to 762 nm. Typical total intensity of such as intensity, emission height, background continuum, etc., we airglow is 100 1000 R as listed in Table 1, and 10 % variation of selected the airglow emissions which will be measured with VISI, the total intensity must be detected in order to investigate the and determined the requirements for instrumental design. The airglow variation pattern. In addition, short exposure cycle less targets and requirements are summarized in Table 1. than several seconds is necessary to measure small-scale airglow Table 1. Scientific Targets of VISI signatures (see Table 1) considering the orbital speed of ISS (~8 km/s). Airglow Required Region Scientific Typical A sectional view of VISI and its specifications are given in (waele- spatial (height) target intensity Figure 4 and Table 2, respectively. -
New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period
Hayabusa2 Extended Mission: New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period M. Hirabayashi1, Y. Mimasu2, N. Sakatani3, S. Watanabe4, Y. Tsuda2, T. Saiki2, S. Kikuchi2, T. Kouyama5, M. Yoshikawa2, S. Tanaka2, S. Nakazawa2, Y. Takei2, F. Terui2, H. Takeuchi2, A. Fujii2, T. Iwata2, K. Tsumura6, S. Matsuura7, Y. Shimaki2, S. Urakawa8, Y. Ishibashi9, S. Hasegawa2, M. Ishiguro10, D. Kuroda11, S. Okumura8, S. Sugita12, T. Okada2, S. Kameda3, S. Kamata13, A. Higuchi14, H. Senshu15, H. Noda16, K. Matsumoto16, R. Suetsugu17, T. Hirai15, K. Kitazato18, D. Farnocchia19, S.P. Naidu19, D.J. Tholen20, C.W. Hergenrother21, R.J. Whiteley22, N. A. Moskovitz23, P.A. Abell24, and the Hayabusa2 extended mission study group. 1Auburn University, Auburn, AL, USA ([email protected]) 2Japan Aerospace Exploration Agency, Kanagawa, Japan 3Rikkyo University, Tokyo, Japan 4Nagoya University, Aichi, Japan 5National Institute of Advanced Industrial Science and Technology, Tokyo, Japan 6Tokyo City University, Tokyo, Japan 7Kwansei Gakuin University, Hyogo, Japan 8Japan Spaceguard Association, Okayama, Japan 9Hosei University, Tokyo, Japan 10Seoul National University, Seoul, South Korea 11Kyoto University, Kyoto, Japan 12University of Tokyo, Tokyo, Japan 13Hokkaido University, Hokkaido, Japan 14University of Occupational and Environmental Health, Fukuoka, Japan 15Chiba Institute of Technology, Chiba, Japan 16National Astronomical Observatory of Japan, Iwate, Japan 17National Institute of Technology, Oshima College, Yamaguchi, Japan 18University of Aizu, Fukushima, Japan 19Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA 20University of Hawai’i, Manoa, HI, USA 21University of Arizona, Tucson, AZ, USA 22Asgard Research, Denver, CO, USA 23Lowell Observatory, Flagstaff, AZ, USA 24NASA Johnson Space Center, Houston, TX, USA 1 Highlights 1. -
View Conducted by Its Standing Review Board (SRB)
Science Committee Report Dr. Wes Huntress, Chair 1 Science Committee Members Wes Huntress, Chair Byron Tapley, (Vice Chair) University of Texas-Austin, Chair of Earth Science Alan Boss, Carnegie Institution, Chair of Astrophysics Ron Greeley, Arizona State University, Chair of Planetary Science Gene Levy, Rice University , Chair of Planetary Protection Roy Torbert, University of New Hampshire, Chair of Heliophysics Jack Burns, University of Colorado Noel Hinners, Independent Consultant *Judith Lean, Naval Research Laboratory Michael Turner, University of Chicago Charlie Kennel, Chair of Space Studies Board (ex officio member) * = resigned July 16, 2010 2 Agenda • Science Results • Programmatic Status • Findings & Recommendations 3 Unusual Thermosphere Collapse • Deep drop in Thermospheric (50 – 400 km) density • Deeper than expected from solar cycle & CO2 4 Aeronomy of Ice in the Mesosphere (AIM) unlocking the secrets of Noctilucent Clouds (NLCs) Form 50 miles above surface in polar summer vs ~ 6 miles for “norm79al” clouds. NLCs getting brighter; occurring more often. Why? Linked to global change? AIM NLC Image June 27, 2009 - AIM measured the relationship between cloud properties and temperature - Quantified for the first time, the dramatic response to small changes, 10 deg C, in temperature - T sensitivity critical for study of global change effects on mesosphere Response to Gulf Oil Spill UAVSAR 23 June 2010 MODIS 31 May 2010 ASTER 24 May 2010 Visible Visible/IR false color Satellite instruments: continually monitoring the extent of -
Hubble Space Telescope Primer for Cycle 25
January 2017 Hubble Space Telescope Primer for Cycle 25 An Introduction to the HST for Phase I Proposers 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration How to Get Started For information about submitting a HST observing proposal, please begin at the Cycle 25 Announcement webpage at: http://www.stsci.edu/hst/proposing/docs/cycle25announce Procedures for submitting a Phase I proposal are available at: http://apst.stsci.edu/apt/external/help/roadmap1.html Technical documentation about the instruments are available in their respective handbooks, available at: http://www.stsci.edu/hst/HST_overview/documents Where to Get Help Contact the STScI Help Desk by sending a message to [email protected]. Voice mail may be left by calling 1-800-544-8125 (within the US only) or 410-338-1082. The HST Primer for Cycle 25 was edited by Susan Rose, Senior Technical Editor and contributions from many others at STScI, in particular John Debes, Ronald Downes, Linda Dressel, Andrew Fox, Norman Grogin, Katie Kaleida, Matt Lallo, Cristina Oliveira, Charles Proffitt, Tony Roman, Paule Sonnentrucker, Denise Taylor and Leonardo Ubeda. Send comments or corrections to: Hubble Space Telescope Division Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 E-mail:[email protected] CHAPTER 1: Introduction In this chapter... 1.1 About this Document / 7 1.2 What’s New This Cycle / 7 1.3 Resources, Documentation and Tools / 8 1.4 STScI Help Desk / 12 1.1 About this Document The Hubble Space Telescope Primer for Cycle 25 is a companion document to the HST Call for Proposals1. -
Probes to the Inferior Planets – a New Dawn for Neo and Ieo Detection Technology Demonstration from Heliocentric Orbits Interior to the Earth’S?
PROBES TO THE INFERIOR PLANETS – A NEW DAWN FOR NEO AND IEO DETECTION TECHNOLOGY DEMONSTRATION FROM HELIOCENTRIC ORBITS INTERIOR TO THE EARTH’S? 2011 IAA Planetary Defense Conference 09-12 May 2011 Bucharest, Romania Jan Thimo Grundmann(1), Stefano Mottola(2), Maximilian Drentschew(6), Martin Drobczyk(1), Ralph Kahle(3), Volker Maiwald(4), Dominik Quantius(4), Paul Zabel(4), Tim van Zoest(5) (1)DLR German Aerospace Center - Institute of Space Systems - Department of Satellite Systems Robert-Hooke-Straße 7, 28359 Bremen, Germany Email: [email protected], [email protected] (2)DLR German Aerospace Center - Institute of Planetary Research - Department Asteroids and Comets Rutherfordstraße 2, 12489 Berlin, Germany Email: [email protected] (3)DLR German Aerospace Center - Space Operations and Astronaut Training - Space Flight Technology Dept. 82234 Oberpfaffenhofen-Wesseling, Germany Email: [email protected] (4)DLR German Aerospace Center - Institute of Space Systems - Dept. System Analysis Space Segments (SARA) Robert-Hooke-Straße 7, 28359 Bremen, Germany Email: [email protected], [email protected], [email protected] (5)DLR German Aerospace Center - Institute of Space Systems - Department of Exploration Systems Robert-Hooke-Straße 7, 28359 Bremen, Germany Email: [email protected] (6)ZFT Zentrum für Telematik Allesgrundweg 12, 97218 Gerbrunn, Germany Email: [email protected] ABSTRACT With the launch of MESSENGER and VENUS EXPRESS, a new wave of exploration of the inner solar system has begun. Noting the growing number of probes to the inner solar system, it is proposed to connect the expertise of the respective spacecraft teams and the NEO and IEO survey community to best utilize the extended cruise phases and to provide additional data return in support of pure science as well as planetary defence. -
[OI] 5577 in the Airglow and the Aurora
Journal of Resea rch of the National Bureau of Sta ndards- D. Radio Propagation Vol. 63D, No.1, July-August 1959 Origin of [OlJ 5577 in the Airglow and the Aurora Franklin E. Roach, James W. McCaulley, and Edward Marovich (January 30, 1959) The distribution of 5577 zenith intensities at stations in the subauroral zone iB found to be unimodal with no discontinuity at the visual threshold. This is interpreted as evi dence that 5577 airglow and 5577 aurora may have a common origin. 1. Introduction origin hypothesis, their critical characteristic being the lack of any discontinuity. It i cu tomary to refer to [01] 5577 as airglow if In figure 2, a replot of the histogram of St. Amand it is invisible and as aurora if it is visible. Thus, and Ashburn is shown with a regroupillg of the data the physiological visual threshold (at approximately to correspond to class intervals of 50 R rather than the 10 R that they used. They put an approxi 1,000 myleighs 1 for extended objects) has been assumed to have a physical significance in the upper mately normal curve through the plot on the basis atmosphere with different mechanisms operative of which they were able to state that an intensity above and below the threshold. The purpose of correspondulg to a just visible aurora should occur this paper is to inquil'e into the existence of a only "once or twice in geologic time." Because physical criterion to distinguish between 5577 auroras do occur occasionally, though rarely, in southern California, the implication is that an aurora airglow and 5577 aurora. -
Achievements of Hayabusa2: Unveiling the World of Asteroid by Interplanetary Round Trip Technology
Achievements of Hayabusa2: Unveiling the World of Asteroid by Interplanetary Round Trip Technology Yuichi Tsuda Project Manager, Hayabusa2 Japan Aerospace ExplorationAgency 58th COPUOS, April 23, 2021 Lunar and Planetary Science Missions of Japan 1980 1990 2000 2010 2020 Future Plan Moon 2007 Kaguya 1990 Hiten SLIM Lunar-A × Venus 2010 Akatsuki 2018 Mio 1998 Nozomi × Planets Mercury (Mars) 2010 IKAROS Venus MMX Phobos/Mars 1985 Suisei 2014 Hayabusa2 Small Bodies Asteroid Ryugu 2003 Hayabusa 1985 Sakigake Asteroid Itokawa Destiny+ Comet Halley Comet Pheton 2 Hayabusa2 Mission ✓ Sample return mission to a C-type asteroid “Ryugu” ✓ 5.2 billion km interplanetary journey. Launch Earth Gravity Assist Ryugu Arrival MINERVA-II-1 Deployment Dec.3, 2014 Sep.21, 2018 Dec.3, 2015 Jun.27, 2018 MASCOT Deployment Oct.3, 2018 Ryugu Departure Nov.13.2019 Kinetic Impact Earth Return Second Dec.6, 2020 Apr.5, 2019 Target Markers Orbiting Touchdown Sep.16, 2019 Jul,11, 2019 First Touchdown Feb.22, 2019 MINERVA-II-2 Orbiting MD [D VIp srvlxp #534<# Oct.2, 2019 Hayabusa2 Spacecraft Overview Deployable Xband Xband Camera (DCAM3) HGA LGA Xband Solar Array MGA Kaba nd Ion Engine HGA Panel RCS thrusters ×12 ONC‐T, ONC‐W1 Star Trackers Near Infrared DLR MASCOT Spectrometer (NIRS3) Lander Thermal Infrared +Z Imager (TIR) Reentry Capsule +X MINERVA‐II Small Carry‐on +Z LIDAR ONC‐W2 +Y Rovers Impactor (SCI) +X Sampler Horn Target +Y Markers ×5 Launch Mass: 609kg Ion Engine: Total ΔV=3.2km/s, Thrust=5-28mN (variable), Specific Impulse=2800- 3000sec. (4 thrusters, mounted on two-axis gimbal) Chemical RCS: Bi-prop. -
+ New Horizons
Media Contacts NASA Headquarters Policy/Program Management Dwayne Brown New Horizons Nuclear Safety (202) 358-1726 [email protected] The Johns Hopkins University Mission Management Applied Physics Laboratory Spacecraft Operations Michael Buckley (240) 228-7536 or (443) 778-7536 [email protected] Southwest Research Institute Principal Investigator Institution Maria Martinez (210) 522-3305 [email protected] NASA Kennedy Space Center Launch Operations George Diller (321) 867-2468 [email protected] Lockheed Martin Space Systems Launch Vehicle Julie Andrews (321) 853-1567 [email protected] International Launch Services Launch Vehicle Fran Slimmer (571) 633-7462 [email protected] NEW HORIZONS Table of Contents Media Services Information ................................................................................................ 2 Quick Facts .............................................................................................................................. 3 Pluto at a Glance ...................................................................................................................... 5 Why Pluto and the Kuiper Belt? The Science of New Horizons ............................... 7 NASA’s New Frontiers Program ........................................................................................14 The Spacecraft ........................................................................................................................15 Science Payload ...............................................................................................................16 -
Highlights in Space 2010
International Astronautical Federation Committee on Space Research International Institute of Space Law 94 bis, Avenue de Suffren c/o CNES 94 bis, Avenue de Suffren UNITED NATIONS 75015 Paris, France 2 place Maurice Quentin 75015 Paris, France Tel: +33 1 45 67 42 60 Fax: +33 1 42 73 21 20 Tel. + 33 1 44 76 75 10 E-mail: : [email protected] E-mail: [email protected] Fax. + 33 1 44 76 74 37 URL: www.iislweb.com OFFICE FOR OUTER SPACE AFFAIRS URL: www.iafastro.com E-mail: [email protected] URL : http://cosparhq.cnes.fr Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law The United Nations Office for Outer Space Affairs is responsible for promoting international cooperation in the peaceful uses of outer space and assisting developing countries in using space science and technology. United Nations Office for Outer Space Affairs P. O. Box 500, 1400 Vienna, Austria Tel: (+43-1) 26060-4950 Fax: (+43-1) 26060-5830 E-mail: [email protected] URL: www.unoosa.org United Nations publication Printed in Austria USD 15 Sales No. E.11.I.3 ISBN 978-92-1-101236-1 ST/SPACE/57 *1180239* V.11-80239—January 2011—775 UNITED NATIONS OFFICE FOR OUTER SPACE AFFAIRS UNITED NATIONS OFFICE AT VIENNA Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law Progress in space science, technology and applications, international cooperation and space law UNITED NATIONS New York, 2011 UniTEd NationS PUblication Sales no. -
REMOTE SENSING of SEISMIC ACTIVITY on VENUS USING a SMALL SPACECRAFT: INITIAL MODELING RESULTS, A. Komjathy1, A. Didion1, B. Sutin1, B
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 1731.pdf REMOTE SENSING OF SEISMIC ACTIVITY ON VENUS USING A SMALL SPACECRAFT: INITIAL MODELING RESULTS, A. Komjathy1, A. Didion1, B. Sutin1, B. Nakazono1, A. Karp1, M. Wallace1, G. Lan- toine1, S. Krishnamoorthy1, M. Rud1, J. Cutts, J. Makela2, M. Grawe2, P. Lognonné3, B. Kenda3, M. Drilleau3 and Jörn Helbert4 1Jet Propulsion Laboratory, California Institute of Technology, USA 2University of Illinois at Urbana-Champaign, USA 3Institut de Physique du Globe-Paris Sorbonne, France 4Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), Germany Introduction: The planetary evolution and struc- other at 4.3 µm (visible on the dayside). The signifi- ture of Venus remain uncertain more than half a centu- cant advantage of observing nightglow on Venus is ry after the first visit by a robotic spacecraft. To under- that it is much brighter on Venus than on Earth [2] and stand how Venus evolved it is necessary to detect the that airglow lifetime (~4,000 sec) is significantly long- signs of seismic activity. Due to the adverse surface er than the period of seismic waves (10-30 sec). This conditions on Venus, with extremely high temperature makes it very attractive for directly detecting surface and pressure, it is infeasible with current technology, waves on Venus. This is in sharp contrast with Earth even using flagship missions, to place seismometers on where the lifetime of airglow is about one order of the surface for an extended period of time. Due to dy- magnitude smaller (~110 sec) than, e.g., the tsunami namic coupling between the solid planet and the at- waves we routinely observe on Earth with 630 nm air- mosphere, the waves generated by quakes propagate glow instruments [4]. -
Sample of Paper for 30Th ISTS & 6Th NAST
Orbit Determination for Long-term Prediction of Solar Power Sail Demonstrator IKAROS By ShoTaniguchi1), Takafumi Ohnishi1), Osamu Mori 2), Hideki Kato2), Hiroshi Takeuchi2), Atsushi Tomiki2), Yuya Mimasu2), Naoko Ogawa2), Jun Matsumoto2), Taichi ITO2), Tsutomu Ichikawa2), MakotoYoshikawa2), Shota Kikuchi3) , and Yosuke Kawabata3) 1) Technical computing solutions unit, science solutions div, Fujitsu Limited, Tokyo, Japan 2) Institute of Space and Astronautical Science, JAXA, Sagamihara, Japan 3) Department of Aeronautics and Astronautics, The University of Tokyo, Tokyo, Japan (Received April 24st, 2017) The world’s first solar sail IKAROS (Interplanetary Kite-craft Accelerated by Radiation of the Sun) was launched along with the Venus Climate Orbiter Akatsuki in May 2010. IKAROS was full successful of missions that have been planned for first half year. After the Venus flyby in Dec 2010, it was carried out an extended mission. IKAROS has succeeded many additional engineering and scientific missions. We are obtained many orbit determination skill1) in nominal and extended phase. However, the IKAROS was almost run out the fuel in Dec 2011, so attitude and spin rate was out of control .As a result, lost communication with the ground station due to the power shortage on December 24, 2011. After this operation IKAROS began to repeat the hibernation of the 10-month period by substantially fixed attitude in inertial coordinate while maintaining the spin rate between 5rpm and 6rpm without fuel. End of a hibernation, it is necessary to difficult orbit determination and 10 months or more of the long-term trajectory prediction for antenna tracking at USUDA deep space tracking station. In order to perform the orbit determination of long-term arc, an optical model2) of the solar sail back surface was constructed. -
Nighttime Photochemical Model and Night Airglow on Venus
Planetary and Space Science 85 (2013) 78–88 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Nighttime photochemical model and night airglow on Venus Vladimir A. Krasnopolsky n a Department of Physics, Catholic University of America, Washington, DC 20064, USA b Moscow Institute of Physics and Technology, Dolgoprudnyy 141700 Russia article info abstract Article history: The photochemical model for the Venus nighttime atmosphere and night airglow (Krasnopolsky, 2010, Received 23 December 2012 Icarus 207, 17–27) has been revised to account for the SPICAV detection of the nighttime ozone layer and Received in revised form more detailed spectroscopy and morphology of the OH nightglow. Nighttime chemistry on Venus is 28 April 2013 induced by fluxes of O, N, H, and Cl with mean hemispheric values of 3 Â 1012,1.2Â 109,1010, and Accepted 31 May 2013 − − 1010 cm 2 s 1, respectively. These fluxes are proportional to column abundances of these species in the Available online 18 June 2013 daytime atmosphere above 90 km, and this favors their validity. The model includes 86 reactions of 29 Keywords: species. The calculated abundances of Cl2, ClO, and ClNO3 exceed a ppb level at 80–90 km, and Venus perspectives of their detection are briefly discussed. Properties of the ozone layer in the model agree Photochemistry with those observed by SPICAV. An alternative model without the flux of Cl agrees with the observed O Night airglow 3 peak altitude and density but predicts an increase of ozone to 4 Â 108 cm−3 at 80 km.