UNDERSTANDING SPACE WEATHER Part III: the Sun’S Domain
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Global Ionosphere-Thermosphere-Mesosphere (ITM) Mapping Across Temporal and Spatial Scales a White Paper for the NRC Decadal
Global Ionosphere-Thermosphere-Mesosphere (ITM) Mapping Across Temporal and Spatial Scales A White Paper for the NRC Decadal Survey of Solar and Space Physics Andrew Stephan, Scott Budzien, Ken Dymond, and Damien Chua NRL Space Science Division Overview In order to fulfill the pressing need for accurate near-Earth space weather forecasts, it is essential that future measurements include both temporal and spatial aspects of the evolution of the ionosphere and thermosphere. A combination of high altitude global images and low Earth orbit altitude profiles from simple, in-the-medium sensors is an optimal scenario for creating continuous, routine space weather maps for both scientific and operational interests. The method presented here adapts the vast knowledge gained using ultraviolet airglow into a suggestion for a next-generation, near-Earth space weather mapping network. Why the Ionosphere, Thermosphere, and Mesosphere? The ionosphere-thermosphere-mesosphere (ITM) region of the terrestrial atmosphere is a complex and dynamic environment influenced by solar radiation, energy transfer, winds, waves, tides, electric and magnetic fields, and plasma processes. Recent measurements showing how coupling to other regions also influences dynamics in the ITM [e.g. Immel et al., 2006; Luhr, et al, 2007; Hagan et al., 2007] has exposed the need for a full, three- dimensional characterization of this region. Yet the true level of complexity in the ITM system remains undiscovered primarily because the fundamental components of this region are undersampled on the temporal and spatial scales that are necessary to expose these details. The solar and space physics research community has been driven over the past decade toward answering scientific questions that have a high level of practical application and relevance. -
Doc.10100.Space Weather Manual FINAL DRAFT Version
Doc 10100 Manual on Space Weather Information in Support of International Air Navigation Approved by the Secretary General and published under his authority First Edition – 2018 International Civil Aviation Organization TABLE OF CONTENTS Page Chapter 1. Introduction ..................................................................................................................................... 1-1 1.1 General ............................................................................................................................................... 1-1 1.2 Space weather indicators .................................................................................................................... 1-1 1.3 The hazards ........................................................................................................................................ 1-2 1.4 Space weather mitigation aspects ....................................................................................................... 1-3 1.5 Coordinating the response to a space weather event ......................................................................... 1-3 Chapter 2. Space Weather Phenomena and Aviation Operations ................................................................. 2-1 2.1 General ............................................................................................................................................... 2-1 2.2 Geomagnetic storms .......................................................................................................................... -
In-Flight PSF Calibration of the Nustar Hard X-Ray Optics
In-flight PSF calibration of the NuSTAR hard X-ray optics Hongjun Ana, Kristin K. Madsenb, Niels J. Westergaardc, Steven E. Boggsd, Finn E. Christensenc, William W. Craigd,e, Charles J. Haileyf, Fiona A. Harrisonb, Daniel K. Sterng, William W. Zhangh aDepartment of Physics, McGill University, Montreal, Quebec, H3A 2T8, Canada; bCahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA; cDTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark; dSpace Sciences Laboratory, University of California, Berkeley, CA 94720, USA; eLawrence Livermore National Laboratory, Livermore, CA 94550, USA; fColumbia Astrophysics Laboratory, Columbia University, New York NY 10027, USA; gJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA; hGoddard Space Flight Center, Greenbelt, MD 20771, USA ABSTRACT We present results of the point spread function (PSF) calibration of the hard X-ray optics of the Nuclear Spectroscopic Telescope Array (NuSTAR). Immediately post-launch, NuSTAR has observed bright point sources such as Cyg X-1, Vela X-1, and Her X-1 for the PSF calibration. We use the point source observations taken at several off-axis angles together with a ray-trace model to characterize the in-orbit angular response, and find that the ray-trace model alone does not fit the observed event distributions and applying empirical corrections to the ray-trace model improves the fit significantly. We describe the corrections applied to the ray-trace model and show that the uncertainties in the enclosed energy fraction (EEF) of the new PSF model is ∼<3% for extraction ′′ apertures of R ∼> 60 with no significant energy dependence. -
Space UK Earth’S Surface Water
Issue #49 IN THIS ISSUE: Staring at the Sun MYSTERIOUS Helpline from Space Weightless in the Clouds MERCURY Contents News Cornwall Calling Space Weather Watcher Mapping the Route to Mars Honour for UK Astronaut New Satellite Tracks Pollution UK-France Space Deal In Pictures The Sun Features Mysterious Mercury Zero-G Science Helpline from Space Education Resources UK Space History Skylark Made in the UK Earth-i Info News Cornwall Calling The first Moon landing Cornwall Calling Credit: NASA Cornwall could soon be Antennas at Goonhilly beamed communicating with the Moon and images of the 1969 Moon landing Mars, following the announcement and, shortly after it was built in that the world’s first commercial deep 1985, the 32-metre Goonhilly-6 space communication base will be at antenna carried the historic Live Aid the Goonhilly Earth Station. concert broadcast to TV viewers An £8.4 million investment will see a around the world. two-year upgrade of the Goonhilly-6 A Space Industry Bill, announced antenna so it can communicate as part of the Queen’s speech in One of the large dishes at Goonhilly with future robotic and crewed 2017, will introduce new powers missions to the Moon and Mars. The to allow rocket and spaceplane Credit: Goonhilly Cornwall and Isles of Scilly Local launches from UK soil. Goonhilly is Enterprise Partnership’s Growth Deal also offering spacecraft tracking and the European Space Agency and communications facilities as (ESA) – which the UK Space Agency part of the Spaceport Cornwall contributes to – funded the contract, funding bid. which will allow Goonhilly to support “We see huge opportunities for ESA’s worldwide network of spacecraft the developing space sector in monitoring ground stations. -
Observations of Solar Wind Penetration Into the Earth's Magnetosphere: the Plasma Mantle
ENNIO R. SANCHEZ, CHING-I. MENG, and PATRICK T. NEWELL OBSERVATIONS OF SOLAR WIND PENETRATION INTO THE EARTH'S MAGNETOSPHERE: THE PLASMA MANTLE The large database provided by the continuous coverage of the Defense Meteorological Satellite Pro gram polar orbiting satellites constitutes an important source of information on particle precipitation in the ionosphere. This information can be used to monitor and map the Earth's magnetosphere (the cavity around the Earth that forms as the stream of particles and magnetic field ejected from the Sun, known as the solar wind, encounters the Earth's magnetic field) and for a large variety of statistical studies of its morphology and dynamics. The boundary between the magnetosphere and the solar wind is pre sumably open in some places and at some times, thus allowing the direct entry of solar-wind plasma into the magnetosphere through a boundary layer known as the plasma mantle. The preliminary results of a statistical study of the plasma-mantle precipitation in the ionosphere are presented. The first quan titative mapping of the ionospheric region where the plasma-mantle particles precipitate is obtained. INTRODUCTION Polar orbiting satellites are very useful platforms for studying the properties of the environment surrounding the Earth at distances well above the ionosphere. This article focuses on a description of the enormous poten tial of those platforms, especially when they are com bined with other means of measurement, such as ground-based stations and other satellites. We describe in some detail the first results of the kind of study for which the polar orbiting satellites are ideal instruments. -
Structure and Energy Transport of the Solar Convection Zone A
Structure and Energy Transport of the Solar Convection Zone A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI'I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN ASTRONOMY December 2004 By James D. Armstrong Dissertation Committee: Jeffery R. Kuhn, Chairperson Joshua E. Barnes Rolf-Peter Kudritzki Jing Li Haosheng Lin Michelle Teng © Copyright December 2004 by James Armstrong All Rights Reserved iii Acknowledgements The Ph.D. process is not a path that is taken alone. I greatly appreciate the support of my committee. In particular, Jeff Kuhn has been a friend as well as a mentor during this time. The author would also like to thank Frank Moss of the University of Missouri St. Louis. His advice has been quite helpful in making difficult decisions. Mark Rast, Haosheng Lin, and others at the HAO have assisted in obtaining data for this work. Jesper Schou provided the helioseismic rotation data. Jorgen Christiensen-Salsgaard provided the solar model. This work has been supported by NASA and the SOHOjMDI project (grant number NAG5-3077). Finally, the author would like to thank Makani for many interesting discussions. iv Abstract The solar irradiance cycle has been observed for over 30 years. This cycle has been shown to correlate with the solar magnetic cycle. Understanding the solar irradiance cycle can have broad impact on our society. The measured change in solar irradiance over the solar cycle, on order of0.1%is small, but a decrease of this size, ifmaintained over several solar cycles, would be sufficient to cause a global ice age on the earth. -
Solar Radiation
5 Solar Radiation In this chapter we discuss the aspects of solar radiation, which are important for solar en- ergy. After defining the most important radiometric properties in Section 5.2, we discuss blackbody radiation in Section 5.3 and the wave-particle duality in Section 5.4. Equipped with these instruments, we than investigate the different solar spectra in Section 5.5. How- ever, prior to these discussions we give a short introduction about the Sun. 5.1 The Sun The Sun is the central star of our solar system. It consists mainly of hydrogen and helium. Some basic facts are summarised in Table 5.1 and its structure is sketched in Fig. 5.1. The mass of the Sun is so large that it contributes 99.68% of the total mass of the solar system. In the center of the Sun the pressure-temperature conditions are such that nuclear fusion can Table 5.1: Some facts on the Sun Mean distance from the Earth 149 600 000 km (the astronomic unit, AU) Diameter 1392000km(109 × that of the Earth) Volume 1300000 × that of the Earth Mass 1.993 ×10 27 kg (332 000 times that of the Earth) Density(atitscenter) >10 5 kg m −3 (over 100 times that of water) Pressure (at its center) over 1 billion atmospheres Temperature (at its center) about 15 000 000 K Temperature (at the surface) 6 000 K Energy radiation 3.8 ×10 26 W TheEarthreceives 1.7 ×10 18 W 35 36 Solar Energy Internal structure: core Subsurface ows radiative zone convection zone Photosphere Sun spots Prominence Flare Coronal hole Chromosphere Corona Figure 5.1: The layer structure of the Sun (adapted from a figure obtained from NASA [ 28 ]). -
Nustar Observatory Guide
NuSTAR Guest Observer Program NuSTAR Observatory Guide Version 3.2 (June 2016) NuSTAR Science Operations Center, California Institute of Technology, Pasadena, CA NASA Goddard Spaceflight Center, Greenbelt, MD nustar.caltech.edu heasarc.gsfc.nasa.gov/docs/nustar/index.html i Revision History Revision Date Editor Comments D1,2,3 2014-08-01 NuSTAR SOC Initial draft 1.0 2014-08-15 NuSTAR GOF Release for AO-1 Addition of more information about CZT 2.0 2014-10-30 NuSTAR SOC detectors in section 3. 3.0 2015-09-24 NuSTAR SOC Update to section 4 for release of AO-2 Update for NuSTARDAS v1.6.0 release 3.1 2016-05-10 NuSTAR SOC (nusplitsc, Section 5) 3.2 2016-06-15 NuSTAR SOC Adjustment to section 9 ii Table of Contents Revision History ......................................................................................................................................................... ii 1. INTRODUCTION ................................................................................................................................................... 1 1.1 NuSTAR Program Organization ..................................................................................................................................................................................... 1 2. The NuSTAR observatory .................................................................................................................................... 2 2.1 NuSTAR Performance ........................................................................................................................................................................................................ -
Episode 2: Bodies in Orbit
Episode 2: Bodies in Orbit This transcript is based on the second episode of Moonstruck, a podcast about humans in space, produced by Dra!House Media and featuring analysis from the Center for Strategic and International Studies’ Aerospace Security Project. Listen to the full episode on iTunes, Spotify, or on our website. BY Thomas González Roberts // PUBLISHED April 4, 2018 AS A DOCENT at the Smithsonian National Air & Space But before humans could use the bathroom in space, a Museum I get a lot of questions from visitors about the lot of questions needed to be answered. Understanding grittiest details of spaceflight. While part of me wants to how human bodies respond to the environment of outer believe that everyone is looking for a thoughtful Kennedy space took years of research. It was a dark, controversial quote to drive home an analysis of the complicated period in the history of spaceflight. This is Moonstruck, a relationship between nationalism and space travel, some podcast about humans in space. I’m Thomas González people are less interested in my stories and more Roberts. interested in other, equally scholarly topics: In the late 1940s, American scientists began to focus on Kids: I have a question. What if you need to go to the two important challenges of spaceflight: solar radiation bathroom while you're in a spacesuit? Is there a special and weightlessness.1 diaper? Aren't you like still wearing the diaper when you are wearing a spacesuit? Let'sThomas start González with radiation. Roberts is the host and executive producer of Moonstruck, and a space policy Alright, alright, I get it. -
Chapter 16 the Sun and Stars
Chapter 16 The Sun and Stars Stargazing is an awe-inspiring way to enjoy the night sky, but humans can learn only so much about stars from our position on Earth. The Hubble Space Telescope is a school-bus-size telescope that orbits Earth every 97 minutes at an altitude of 353 miles and a speed of about 17,500 miles per hour. The Hubble Space Telescope (HST) transmits images and data from space to computers on Earth. In fact, HST sends enough data back to Earth each week to fill 3,600 feet of books on a shelf. Scientists store the data on special disks. In January 2006, HST captured images of the Orion Nebula, a huge area where stars are being formed. HST’s detailed images revealed over 3,000 stars that were never seen before. Information from the Hubble will help scientists understand more about how stars form. In this chapter, you will learn all about the star of our solar system, the sun, and about the characteristics of other stars. 1. Why do stars shine? 2. What kinds of stars are there? 3. How are stars formed, and do any other stars have planets? 16.1 The Sun and the Stars What are stars? Where did they come from? How long do they last? During most of the star - an enormous hot ball of gas day, we see only one star, the sun, which is 150 million kilometers away. On a clear held together by gravity which night, about 6,000 stars can be seen without a telescope. -
Building the Coolest X-Ray Satellite
National Aeronautics and Space Administration Building the Coolest X-ray Satellite 朱雀 Suzaku A Video Guide for Teachers Grades 9-12 Probing the Structure & Evolution of the Cosmos http://suzaku-epo.gsfc.nasa.gov/ www.nasa.gov The Suzaku Learning Center Presents “Building the Coolest X-ray Satellite” Video Guide for Teachers Written by Dr. James Lochner USRA & NASA/GSFC Greenbelt, MD Ms. Sara Mitchell Mr. Patrick Keeney SP Systems & NASA/GSFC Coudersport High School Greenbelt, MD Coudersport, PA This booklet is designed to be used with the “Building the Coolest X-ray Satellite” DVD, available from the Suzaku Learning Center. http://suzaku-epo.gsfc.nasa.gov/ Table of Contents I. Introduction 1. What is Astro-E2 (Suzaku)?....................................................................................... 2 2. “Building the Coolest X-ray Satellite” ....................................................................... 2 3. How to Use This Guide.............................................................................................. 2 4. Contents of the DVD ................................................................................................. 3 5. Post-Launch Information ........................................................................................... 3 6. Pre-requisites............................................................................................................. 4 7. Standards Met by Video and Activities ...................................................................... 4 II. Video Chapter 1 -
THEMIS Telescope Images Analysed for Space Weather Traces
EPSC Abstracts Vol. 14, EPSC2020-1022, 2020 https://doi.org/10.5194/epsc2020-1022 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. THEMIS telescope images analysed for space weather traces Melinda Dósa1, Valeria Mangano2, Zsofia Bebesi1, Stefano Massetti2, Anna Milillo2, and Anna Görgei3 1Wigner Research Centre for Physics, Space Physics and Space Technology, Budapest, Hungary ([email protected]) 2INAF/IAPS, Istituto Nazionale di Astrofisica, Roma, Italy 3Eötvös Loránd University, Institute of Physics The THEMIS solar telescope operating on Tenerife (Canary islands) has observed Mercury’s Na exosphere along several campaigns since 2007. A dataset of images taken between 2009 and 2013 are analysed here in relation with propagated solar wind data. A small subset of the images shows a low level of correlation between Na-emission and solar wind dynamic pressure. The amount of data at present is not sufficient to make a clear statement on whether the correlation is a coincidence or can be explained by other factors (position of Mercury and Earth, solar activity, etc.). Nevertheless, the authors present a comprehensive study taking into account all possible factors. Sodium plays a special role in Mercury’s exosphere: due to its strong resonance line it has been observed and monitored by Earth-based telescopes for decades. Different and highly variable patterns of Na-emission have been identified, the most common and recurrent being the high latitude double-peak pattern [1]. It is clear that the exosphere is linked to the surface and influenced by the interstellar medium and the solar wind deviated by the magnetosphere, but the role and weight of the single processes are still under discussion [2].