SPACE WEATHER INTERPRETING THE WIND. Petra Vanlommel & Luciano Rodriguez
|
|
|
- Bonnie Charles
- 10 years ago
- Views:
Transcription
1 SPACE WEATHER INTERPRETING THE WIND Petra Vanlommel & Luciano Rodriguez
2 THE SUN LOSES ENERGY Radiation Mass Particles
3 THE SUN LOSES ENERGY PHYSICAL REPHRASING Total Solar Irradiance Solar Wind Fast Particles
4 SPACE WEATHER Flares Plasma wolken Snelle zonnewind Proton storm
5 SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
6 SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
7 SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
8 TIME TO ARRIVE ON EARTH Plasma wolken 8 minutes Flares Days Proton Hour storm Snelle zonnewind
9 FORECAST Flare Flares probability Perturbations Plasma wolken of the Geomagnetic Snelle zonnewind field Proton Probability storm
10 RELAX AND WATCH
11 OUR PROTECTION
12 Total Solar Irradiance Solar Wind Fast Particles
13
14 GEOMAGNETIC STORMS 4x 100x 200x 600x 1700x
15 CONSEQUENCES GIC Satellite operations, e.g. GNSS, drag, surface charging Radio communication Electrical power plants Aurora Malmö Blackout - Oct 30, 2004 About customer were without electricity in Malmö, Sweden for minutes First known power grid blackout due to GIC in Europe An overcurrent relay was too sensitive to the third harmonic of 50 hz. It has been replaced by a less sensitive relay later.
16 GLOBAL SOLAR DIPOLE Snelle wind Open magneetveld lijnen Snelle wind Gesloten veldlijnen Heliosferisch stroomvlak Trage wind Trage wind Snelle wind
17 LOCAL MAGNETIC FIELDS
18 LOCAL MAGNETIC FIELDS
19 SOLAR WIND
20 SLOW VERSUS FAST High: ~10 Low: ~10 4 K, ~1eV Variable km/s Density, cm -3 Temperature Behavior Low: ~3 High: ~10 5 K, ~10eV Stationary
21
22 SOLAR WIND - IN SITU
23 COORDINATE SYSTEM
24 IMF POLARITY for 400 km/s ϕ ~ 135 for 400 km/s ϕ ~ 315
25 EXTREME FAST ϕ = 90
26 EXTREME FAST ϕ = 0 ϕ = 360
27 RADIAL
28 RADIAL
29 RADIAL
30 RADIAL
31 VARIATIONS Non-eruptive Eruptive Coronal Hole Coronal Mass Ejection Sector Boundary Crossing
32 SECTOR BOUNDARY CROSSING
33 HELIOSPHERIC CURRENT SHEET Snelle wind Open magneetveld lijnen Snelle wind Gesloten veldlijnen Heliosferisch stroomvlak Trage wind Trage wind Snelle wind
34 BALLERINA SKIRT
35 MAGNETIC SECTORS Cravens, 1997
36 SEPT 10 - IN SITU: PHI
37 SEPT 10 - IN SITU - DENSITY
38 SEPT 10 - IN SITU - BZ
39 GEO EFFECTIVENESS
40 CORONAL HOLE
41 WHEN SLOW AND FAST MEET
42 Top View
43
44
45
46
47 IN SITU - CH IN A SCHEME
48 CORONAL HOLE Co-rotating structure Shock is present, usually behind 1AU Radial! No extra mass-flux
49 IN SITU
50 IN REAL LIFE
51 CME A new, discrete, bright white light feature in the coronograph field-of-view with a predominantly, radial outward velocity.
52 TRANSIENT - EXTRA MASS
53 STRUCTURE 1.Shock, if ICME is fast enough 2.Shocked sheath plasma compressed - heated - strong B - varying direction of B 3.Driver gas, i.e. ICME cool - steady strong B - large scale smooth field rotation - decreasing speed
54 PATH
55
56
57
58
59
60 Shock Short sheath High B Smooth rotation in Bz Decreasing speed
61 Shock Sheath High B Smooth rotation in Phi Decreasing speed Low T
62 THE WIND YESTERDAY
63 SOLAR SOURCE
64 CONTACT SIDC: sidc.be STCE News letter: stce.be
65 INTERESTING stce.be/esww10
66 MI : SPACE WEATHER FOR ENGINEERS Focus on HF communication, Trans-ionospheric propagation, effects on GNSS signal precision Nov 12-15, 2013, Leuven, Belgium
67
Space Weather: An Introduction C. L. Waters. Centre for Space Physics University of Newcastle, Australia
Space Weather: An Introduction C. L. Waters Centre for Space Physics University of Newcastle, Australia 1 Outline Space weather: Conditions on the Sun and in the solar wind, magnetosphere, ionosphere and
Met Office Space Weather Operations and R&D
Met Office Space Weather Operations and R&D David Jackson Mark Gibbs, Suzy Bingham, Francois Bocquet, Edmund Henley, Sophie Murray WMO / ISES Meeting, August 9-10 2014, Moscow, Russia Met Office Motivation?
Solar Storms and Northern lights - how to predict Space Weather and the Aurora
Solar Storms and Northern lights - how to predict Space Weather and the Aurora Pål Brekke Norwegian Space Centre/UNIS Pål Brekke torsdag 12. mars 15 Fleet of satellites watching the Sun Stereo SDO SOHO
Space Weather: Forecasting & Impacts on Critical Infrastructure
Space Weather: Forecasting & Impacts on Critical Infrastructure Dr. Genene Fisher Senior Advisor for Space Weather National Weather Service AMS Washington Forum 12 April 2012 Outline Solar Activity Update
INTRODUCTION TO SOLAR WEATHER & HF PROPAGATION. Lewis Thompson W5IFQ September 27, 2011
INTRODUCTION TO SOLAR WEATHER & HF PROPAGATION Lewis Thompson W5IFQ September 27, 2011 PRESENTATION Ionospheric propagation NVIS Long-Range Frequency Selection (Critical Frequency & MUF) Propagation modeling
The solar wind (in 90 minutes) Mathew Owens
The solar wind (in 90 minutes) Mathew Owens 5 th Sept 2013 STFC Advanced Summer School [email protected] Overview There s simply too much to cover in 90 minutes Hope to touch on: Formation of the
Activities of the Japanese Space Weather Forecast Center at Communications Research Laboratory
J. RADIAT. RES., 43: SUPPL., S53 S57 (2002) Activities of the Japanese Space Weather Forecast Center at Communications Research Laboratory SHINICHI WATARI 1 * and FUMIHIKO TOMITA 1 Space weather / ISES/SEP
Space Weather Forecasts for Civil Aviation & Spaceflight. Bill Murtagh NOAA Space Environment Center Boulder, Colorado
Space Weather Forecasts for Civil Aviation & Spaceflight Bill Murtagh NOAA Space Environment Center Boulder, Colorado Space Weather, Aviation, and Spaceflight: Opportunities for Space Weather Research
Space Weather Prediction Research and Services for China Manned Space Mission
Space Weather Prediction Research and Services for China Manned Space Mission Siqing Liu National Space Science Center, CAS Center for Space Science and Applied Research, CAS Outline I. General information
Solar Forcing of Electron and Ion Auroral Inputs
Solar Forcing of Electron and Ion Auroral Inputs Barbara A. Emery (NCAR), Ian G. Richardson (GSFC), David S. Evans (NOAA), Frederick J. Rich (LL/MIT), Gordon Wilson (AFRL), Sarah Gibson (NCAR), Giuliana
EASA Safety Information Bulletin
EASA Safety Information Bulletin SIB No.: 2012-09 Issued: 23 May 2012 Subject: Effects of Space Weather on Aviation Ref. Publication: 1. EU OPS 1.390 Cosmic Radiation; 2. SIB 2012-10 Single Event Effects
COMESEP Project : Space Weather Impact Forecasting
COMESEP Project : Space Weather Impact Forecasting Crosby, N.B. 1, Veronig, A. 2, Robbrecht, E. 3, Vrsnak, B. 4, Vennerstrom, S. 5, Malandraki, O. 6, Dalla, S. 7, Rodriguez, L. 3, Srivastava, N. 8, Hesse,
U.S. DEPARTMENT OF COMMERCE
Space Weather Space Weather Storms from the Sun Storms from the Sun U.S. DEPARTMENT OF COMMERCE National Oceanic and Atmospheric Administration National Weather Service U.S. Department of Commerce National
The Effect of Space Weather Phenomena on Precise GNSS Applications
FUGRO SATELLITE POSITIONING Doc. Ref.: A12321850TCBRC1 The Effect of Space Weather Phenomena on Precise GNSS Applications December 2014 PUBLIC Table of contents The Effect of Space Weather Phenomena on
The Solar Wind. Chapter 5. 5.1 Introduction. 5.2 Description
Chapter 5 The Solar Wind 5.1 Introduction The solar wind is a flow of ionized solar plasma and an associated remnant of the solar magnetic field that pervades interplanetary space. It is a result of the
Solar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
The Extreme Solar Storms of October to November 2003
S.P. Plunkett S.P. Plunkett Space Science Division The Extreme Solar Storms of October to November 2003 AN OVERVIEW OF SOLAR ACTIVITY AND SPACE WEATHER In recent decades, humans have come to rely on space
Coronal Heating Problem
Mani Chandra Arnab Dhabal Raziman T V PHY690C Course Project Indian Institute of Technology Kanpur Outline 1 2 3 Source of the energy Mechanism of energy dissipation Proposed mechanisms Regions of the
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114,, doi:10.1029/2008ja013631, 2009 Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured
Solar Wind: Theory. Parker s solar wind theory
Solar Wind: Theory The supersonic outflow of electrically charged particles, mainly electrons and protons from the solar CORONA, is called the SOLAR WIND. The solar wind was described theoretically by
EMİNE CEREN KALAFATOĞLU EYİGÜLER
EMİNE CEREN KALAFATOĞLU EYİGÜLER SPACE ENVIRONMENT UZB411E 2015-2016 FALL ROOM: 322 / THIRD FLOOR UPPER ATMOSPHERE AND SPACE WEATHER LAB OFFICE HOURS: EVERY TUESDAY AND WEDNESDAY BETWEEN 15-17 FOR OTHER
Simultaneous Heliospheric Imager and Interplanetary Scintillation observations of CMEs and CIRs
Simultaneous Heliospheric Imager and Interplanetary Scintillation observations of CMEs and CIRs Gareth D. Dorrian ([email protected]) 1, Andy R. Breen 1, Jackie A. Davies 2, Alexis P. Rouillard 3, Mario
Counting Sunspots. Parent Prompts: Are there years with lots of sunspots? Are there years with very few sunspots?
Counting are magnetic storms on the Sun these dark areas are a little cooler than the rest of the Sun s atmosphere. They can be easily seen when the Sun s image is projected onto a white surface, using
How To Understand Space Weather
GOES Data and Products in the Space Weather Prediction Center and National Geophysical Data Center Mary Shouldis Satellite Data Product Development Team Lead NGDC/University of Colorado/CIRES Putting Science
Using spacecraft measurements ahead of Earth in the Parker spiral to improve terrestrial space weather forecasts
SPACE WEATHER, VOL. 9,, doi:10.1029/2010sw000627, 2011 Using spacecraft measurements ahead of Earth in the Parker spiral to improve terrestrial space weather forecasts D. L. Turner 1,2 and X. Li 1,2 Received
Coronal expansion and solar wind
Coronal expansion and solar wind The solar corona over the solar cycle Coronal and interplanetary temperatures Coronal expansion and solar wind acceleration Origin of solar wind in magnetic network Multi-fluid
Group Leader: Group Members:
THE SOLAR SYSTEM PROJECT: TOPIC: THE SUN Required Project Content for an Oral/Poster Presentation on THE SUN - What it s made of - Age and how it formed (provide pictures or diagrams) - What is an AU?
Space Weather Measurements. Mary Kicza Assistant Administrator NOAA Satellite & Info. Service (NESDIS) Space Weather Enterprise Forum
Continuity of Critical Space Weather Measurements Mary Kicza Assistant Administrator NOAA Satellite & Info. Service (NESDIS) Space Weather Enterprise Forum May 19, 2009 NOAA Space Weather Requirements
Heating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
Understanding HF propagation
Understanding HF propagation Jari Perkiömäki, OH6BG 12 July 2012 Sappee, Pälkäne, Finland (translated and revised English presentation) HF conditions and contests in a nutshell 1. Learn the basics! The
Space Weather Research and Forecasting in CRL, Japan
Space Weather Research and Forecasting in CRL, Japan Maki Akioka Hiraiso Solar Observatory Communications Research Laboratory Contact [email protected] 1 Contents of Presentation 1.Space Weather Observation
METIS Coronagraph on Solar Orbiter and Solar Probe Synergies. INAF - Osservatorio Astronomico di Torino (Italy) & the METIS Team
METIS Coronagraph on Solar Orbiter and Solar Probe Synergies Silvano Fineschi INAF - Osservatorio Astronomico di Torino (Italy) & the METIS Team 3rd METIS Scientific and Technical Meeting Napoli 17 th
The Sun: Our nearest star
The Sun: Our nearest star Property Surface T Central T Luminosity Mass Lifetime (ms) Value 5500K 15x10 6 K 2 x 10 33 ergs 4 x 10 33 grams 10 billion years Solar Structure Build a model and find the central
Astronomical applications of the over-the-horizon radar NOSTRADAMUS
Astronomical applications of the over-the-horizon radar NOSTRADAMUS J-F. Degurse 1,2, J-Ph. Molinié 1, V. Rannou 1,S. Marcos 2 1 ONERA, Département Electromagnétisme et Radar 2 L2S Supéléc, CNRS UMR 8506,
Space Weather Preparedness Strategy
Space Weather Preparedness Strategy July 2015 OFFICIAL Page i 1. Executive Summary... 1 2. Space weather preparedness... 4 2.1 An overview... 4 2.2 What is the purpose of the document and who does it apply
CSSAR Space Science Cooperation
CSSAR Space Science Cooperation WANG Shuzhi Center for Space Science and Applied Research Chinese Academy of Science(CSSAR) Table of Contents Brief History of CSSAR International Cooperation CAS Strategic
The Earth's Atmosphere. Layers of the Earth's Atmosphere
The Earth's Atmosphere The atmosphere surrounds Earth and protects us by blocking out dangerous rays from the sun. The atmosphere is a mixture of gases that becomes thinner until it gradually reaches space.
UNDERSTANDING SOLAR METRICS DATA
AM 5-610 UNDERSTANDING SOLAR METRICS DATA MAKING SENSE OF THE SOLAR METRICS September 2015 Version 0 DISTRIBUTION RESTRICTION: Approved for public release. Distribution is unlimited \ DEPARTMENT OF THE
SPATIAL DISTRIBUTION OF NORTHERN HEMISPHERE WINTER TEMPERATURES OVER THE SOLAR CYCLE DURING THE LAST 130 YEARS
SPATIAL DISTRIBUTION OF NORTHERN HEMISPHERE WINTER TEMPERATURES OVER THE SOLAR CYCLE DURING THE LAST 130 YEARS Kalevi Mursula, Ville Maliniemi, Timo Asikainen ReSoLVE Centre of Excellence Department of
The Sun and Solar Energy
I The Sun and Solar Energy One of the most important forces behind global change on Earth is over 90 million miles distant from the planet. The Sun is the ultimate, original source of the energy that drives
Solar Energetic Particles: A Relay Race to Earth By Andrea Karelitz
Karelitz 1 Solar Energetic Particles: A Relay Race to Earth By Andrea Karelitz Things move fast. If you re feeling daring, take a trip to Brazil and speed down the fastest water slide in the world at 65
FROM RESEARCH TO OPERATIONS EUROPEAN AND INTERNATIONAL SPACE WEATHER PROJECTS
Volker Bothmer University of Göttingen Institute for Astrophysics Germany 24 th October 2011 IV EU-Russian Open Days Russian Institute for Science and Culture, Vienna, Brahmsplatz 8 Topic: Solar-Terrestrial
JPL ANOMALY ISSUES. Henry B. Garrett Jet Propulsion Laboratory California Institute of Technology Pasadena, CA, 91109
JPL ANOMALY ISSUES Henry B. Garrett Pasadena, CA, 91109 Space Weather Anomaly Concerns for JPL Robotic Mission AGENDA Overview of Space Weather Anomalies on JPL Missions Space Weather Products used by
Solar Activity and Earth's Climate
Rasmus E. Benestad Solar Activity and Earth's Climate Second Edition Published in association with Springer Praxis ids Publishing Publisl PRAXI Chichester, UK Contents Preface to the second edition Preface
Online Solar Databases at NGDC RSTN Solar Radio Databases
Abstract for LWS (Living with a Star) Science Workshop Connecting our Dynamic Sun to the Heliosphere and Geospace, Boulder, Colorado March 23-26, 2004 Online Solar Databases at NGDC RSTN Solar Radio Databases
Multiple Choice Identify the choice that best completes the statement or answers the question.
Test 2 f14 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Carbon cycles through the Earth system. During photosynthesis, carbon is a. released from wood
The sun and the solar corona
The sun and the solar corona Introduction The Sun of our solar system is a typical star of intermediate size and luminosity. Its radius is about 696000 km, and it rotates with a period that increases with
A Plan of Action Under LTSP III
A Plan of Action Under LTSP III William Liu and Robert Rankin Department of Physics, University of Alberta David Boteler Geomagnetic Laboratory, Geological Survey of Canada Submitted to the Canadian Space
Introduction to Astronomy. Lecture 4: Our star, the Sun
Introduction to Astronomy Lecture 4: Our star, the Sun 1 Sun Facts Age = 4.6 x 10 9 years Mean Radius = 7.0x10 5 km = 1.1x10 2 R = 1R Volume = 1.4x10 18 km 3 = 1.3x10 6 R = 1V Mass = 2x10 30 kg = 3.3x10
NOAA Space Weather Prediction Testbed and TESTMEX - NASA
NOAA Space Weather Prediction Testbed: Overview and Updates Rodney Viereck Director, Space Weather Prediction Testbed, NOAA Space Weather Prediction Center Outline: Overview The Transition Process Accomplishments
Ensuring the Preparedness of Users: NOAA Satellites GOES R, JPSS Laura K. Furgione
Ensuring the Preparedness of Users: NOAA Satellites GOES R, JPSS Laura K. Furgione U.S. Permanent Representative with the WMO Deputy Director, NOAA s s National Weather Service WMO Executive Council 65
WELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
2. The map below shows high-pressure and low-pressure weather systems in the United States.
1. Which weather instrument has most improved the accuracy of weather forecasts over the past 40 years? 1) thermometer 3) weather satellite 2) sling psychrometer 4) weather balloon 6. Wind velocity is
Proton temperature and Plasma Volatility
The microstate of the solar wind Radial gradients of kinetic temperatures Velocity distribution functions Ion composition and suprathermal electrons Coulomb collisions in the solar wind Waves and plasma
2-1-5 Space Radiation Effect on Satellites
2-1-5 Space Radiation Effect on Satellites Solar activity and space environment is considered as fundamental and important factors for space system design and operation. Space and solar radiation is widely
Unit 2 Lesson 1 Introduction to Energy. Copyright Houghton Mifflin Harcourt Publishing Company
Get Energized! What are two types of energy? Energy is the ability to cause change. Energy takes many different forms and causes many different effects. There are two general types of energy: kinetic energy
Temperature anisotropy in the solar wind
Introduction Observations Simulations Summary in the solar wind Petr Hellinger Institute of Atmospheric Physics & Astronomical Institute AS CR, Prague, Czech Republic Kinetic Instabilities, Plasma Turbulence
Electromagnetic Pulse: Effects on the U.S. Power Grid
Executive Summary The nation s power grid is vulnerable to the effects of an electromagnetic pulse (EMP), a sudden burst of electromagnetic radiation resulting from a natural or man-made event. EMP events
Solar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation
Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics
Name Period 4 th Six Weeks Notes 2015 Weather
Name Period 4 th Six Weeks Notes 2015 Weather Radiation Convection Currents Winds Jet Streams Energy from the Sun reaches Earth as electromagnetic waves This energy fuels all life on Earth including the
Ionospheric Research with the LOFAR Telescope
Ionospheric Research with the LOFAR Telescope Leszek P. Błaszkiewicz Faculty of Mathematics and Computer Science, UWM Olsztyn LOFAR - The LOw Frequency ARray The LOFAR interferometer consist of a large
8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
Ay 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable
Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater
2. Orbits. FER-Zagreb, Satellite communication systems 2011/12
2. Orbits Topics Orbit types Kepler and Newton laws Coverage area Influence of Earth 1 Orbit types According to inclination angle Equatorial Polar Inclinational orbit According to shape Circular orbit
Diagnostics. Electric probes. Instituto de Plasmas e Fusão Nuclear Instituto Superior Técnico Lisbon, Portugal http://www.ipfn.ist.utl.
Diagnostics Electric probes Instituto de Plasmas e Fusão Nuclear Instituto Superior Técnico Lisbon, Portugal http://www.ipfn.ist.utl.pt Langmuir probes Simplest diagnostic (1920) conductor immerse into
Physics 30 Worksheet #10 : Magnetism From Electricity
Physics 30 Worksheet #10 : Magnetism From Electricity 1. Draw the magnetic field surrounding the wire showing electron current below. x 2. Draw the magnetic field surrounding the wire showing electron
The heliosphere-interstellar medium interaction: One shock or two?
1 The heliosphere-interstellar medium interaction: One shock or two? John D. Richardson M.I.T. Abstract. The issue of whether a shock forms in the interstellar medium as it approaches the heliopause has
What's a magnet? How do you make a magnet? Can you unmake a magnet?
Many people know that the earth has a magnetic field, but few are aware that this field is shrinking. This decrease has been measured over a period of 150 years, and the rate of the decrease shows that
Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
Meeting the Grand Challenge of Protecting an Astronaut s Health: Electrostatic Active Space Radiation Shielding for Deep Space Missions
Meeting the Grand Challenge of Protecting an Astronaut s Health: Electrostatic Active Space Radiation Shielding for Deep Space Missions Ram Tripathi NASA Langley Research Center NIAC 2012 Spring Symposium,
California Standards Grades 9 12 Boardworks 2009 Science Contents Standards Mapping
California Standards Grades 912 Boardworks 2009 Science Contents Standards Mapping Earth Sciences Earth s Place in the Universe 1. Astronomy and planetary exploration reveal the solar system s structure,
ESA Space Weather Initiatives
ESA Space Weather Initiatives The Multi-functional Nature of the Aerospace Domain: a European Approach 22-24 October 2014 Firenze, Italy Juha-Pekka Luntama Space Weather Manager ESA SSA Programme Office
Overview of the IR channels and their applications
Ján Kaňák Slovak Hydrometeorological Institute [email protected] Overview of the IR channels and their applications EUMeTrain, 14 June 2011 Ján Kaňák, SHMÚ 1 Basics in satellite Infrared image interpretation
Neutron Stars. How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967.
Neutron Stars How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967. Using a radio telescope she noticed regular pulses of radio
Lesson 6: Earth and the Moon
Lesson 6: Earth and the Moon Reading Assignment Chapter 7.1: Overall Structure of Planet Earth Chapter 7.3: Earth s Interior More Precisely 7-2: Radioactive Dating Chapter 7.5: Earth s Magnetosphere Chapter
The Solar Wind Interaction with the Earth s Magnetosphere: A Tutorial. C. T. Russell
The Solar Wind Interaction with the Earth s Magnetosphere: A Tutorial C. T. Russell Department of Earth and Space Sciences and Institute of Geophysics and Space Physics University of California Los Angeles
7613-1 - Page 1. Weather Unit Exam Pre-Test Questions
Weather Unit Exam Pre-Test Questions 7613-1 - Page 1 Name: 1) Equal quantities of water are placed in four uncovered containers with different shapes and left on a table at room temperature. From which
Graduate Certificate Program in Energy Conversion & Transport Offered by the Department of Mechanical and Aerospace Engineering
Graduate Certificate Program in Energy Conversion & Transport Offered by the Department of Mechanical and Aerospace Engineering Intended Audience: Main Campus Students Distance (online students) Both Purpose:
Solar Energetic Protons
Solar Energetic Protons The Sun is an effective particle accelerator. Solar Energetic Particles (SEPs) are an important hazard to spacecraft systems and constrain human activities in space. Primary radiation
SPACE WEATHER SUPPORT FOR COMMUNICATIONS. Overview
SPACE WEATHER SUPPORT FOR COMMUNICATIONS Overview Ionospheric variability (space weather) significantly impacts ground and space-based communications. In essence, the electrically charged particles of
SINP SPACE MONITORING DATA CENTER PORTAL
SINP SPACE MONITORING DATA CENTER PORTAL Parunakian D.A. 1, Kalegaev V.V. 2, Bobrovnikov S.Yu. 2, Barinova W.O. 2 1 Moscow State University Skobeltsyn Institute of Nuclear Physics 119991, Russia, e-mail:
Prediction performance of space weather forecast centers following the extreme events of October and November 2003
performance of space weather forecast centers following the extreme events of October and November 2003 Cary Oler Solar Terrestrial Dispatch, Stirling, Alberta, Canada SPACE WEATHER, VOL. 2,, doi:10.1029/2004sw000076,
Towards an Enhanced Telluric Compensation Methodology
Towards an Enhanced Telluric Compensation Methodology Chijioke Ukiwe & Shamus M c Donnell Hunter M c Donnell Pipelines Services Inc. Presented at AUCSC 2011 by Gord Parker, C.E.T., CP2 Edmonton, Alberta,
Kinetic physics of the solar wind
"What science do we need to do in the next six years to prepare for Solar Orbiter and Solar Probe Plus?" Kinetic physics of the solar wind Eckart Marsch Max-Planck-Institut für Sonnensystemforschung Complementary