An isolated substorm is caused by a brief (30-60 min) pulse of southward IMF.
|
|
- Laurel Hoover
- 5 years ago
- Views:
Transcription
1 ESS 200C Lecture 18
2 An isolated substorm is caused by a brief (30-60 min) pulse of southward IMF. Magnetospheric storms are large, prolonged disturbances of the magnetosphere caused by large, prolonged V x B z in solar wind. Many storms follow coronal mass ejections (CMEs; during solar max). Solar Wind has increased magnetic field (flux rope) and high speeds Bipolar signature in Bz depends on solar cycle (+/- versus -/+) Storms can be caused by high speed streams (during solar min). Recur with solar rotation period, 27 days, due to coronal hole recurrence CME or fast wind generate interplanetary shock as overtaking slow wind Impulse from the interplanetary disturbance impulsively compresses the magnetosphere. The sudden compression rapidly increases the magnetopause current and brings it closer to Earth increasing the H- component on the ground. The sudden commencement can be seen in midlatitude magnetograms. The rise time is a few minutes and corresponds to the propagation time of MHD waves from the magnetopause to the point of observations. The compressive phase of the storm lasts 2 to 8 hours. When not followed by the other phases of the storm this part is called a sudden impulse
3 The ring current causes decreases in the horizontal component of the magnetic field at the Earth s surface. The disturbance storm time (Dst) index measures these differences. Sudden Commencement Main Phase Recovery Phase
4 Extended periods (several hours) of southward IMF lead to the main phase of the magnetic storm. Southward IMF leads to magnetic reconnection. Northward IMF has only minimal dayside reconnection. The increased dayside reconnection increases the penetration of the solar wind into the magnetosphere. The enhanced duskward electric field increases the number of particles injected into the ring current. Stronger electric fields lead to earthward expansion of the ring current region. Heavy ionospheric particles also are added to ring current.
5 RC The ring current will grow and D st will decrease ( = ) and eˆ z B0 3 Wmag approach a saturation level when particle sources and losses balance. Ion Losses: charge exchange, scattering into the loss cone and outward diffusion + magnetopause loss Electron Losses: pitch angle scattering into loss cone ΔB r 2 W The period during which the ring current increases is the main phase.
6 As the southward component of the IMF weakens or disappears, the ring current starts to decay. This is the recovery phase of the storm. The recovery phase has several steps. The reduction of the southward IMF causes the reconnection rate to decrease. The reduction of the southward IMF results in a decreasing electric field which leads to a reduction in the injection of new particles into the ring current. The convection boundary moves outward.
7 The ionosphere fills the depleted flux tubes within this expanded boundary with cold ionospheric particles. The interaction between the two plasma populations (hot ring current and cold ionospheric) causes plasma waves which scatter the ring current particles into the loss cone. This causes a loss of ion ring current particles. Another loss mechanism for ring current particles is charge exchange. Charge exchange occurs between energetic ring-current ions and cold(er) hydrogen atoms of the extended exosphere. The result is energetic neutral atoms and cold ions. Detectors which can detect the energetic neutral atoms are have been developed. They enable us to image the ring current in three dimensions. The result of the last two processes is a gradual decrease of the ring current over several days. Energetic Ring Current Ion Thermal Ion + + Thermal Neutral Atom Energetic Neutral Atom (leaves the system)
8 Images in Extreme UltraViolet (EUV) (30.4nm line) of the He + resonant absorption and scattering of sunlight provides a global snapshot of the plasmaspheric He + density. This is produced by photoionization of exospheric He, which provides an image of the exospheric density. This image is taken from the EUV instrument on the IMAGE satellite (Sandel et al., 2000).
9 Charge exchange of energetic ions with exospheric neutrals produces ENA images which image the charged particle density of the ring current in the energy range of the neutrals. This image is taken from the High Energy Neutral Atom instrument on the IMAGE satellite, imaging the Oxygen between keV, the peak contributors to the energy density of the storm time ring current (Mitchell et al., 2000).
10 During quiet times the solar wind provides ~65% of the ring current energy density and the ionosphere only ~35%. (H + dominant). During small and moderate storms the ionospheric contribution becomes ~50% (H + dominant). During intense storms (D st <-150 nt) the ionospheric contribution increases to ~70%. (O + dominant). The O + dominance during intense storms is greater during solar maximum. Increased solar EUV irradiation causes increases ionospheric and atmospheric scale heights which favors the escape of O +. Increased heating of neutral atmosphere and increased ionization rates.
11 Ring current injection can be explained primarily in terms of inward transport of plasma sheet and pre-existing ringcurrent particles. None of the models currently includes the ionosphere. Diffusion has been used successfully to study the injection of radiation belt particles during a storm (see figure at the right). However, the diffusion calculations don t seem to work for the lower energies of the ring current.
12 New Radiation Belt formed by October 2003 Magnetic Storm
13 During magnetic storms precipitation of auroral particles expands toward lower latitudes. Intense red and greenline auroral emissions are found at the equatorward most part of the expanded auroral oval.
14 Examples of magnetic storms: On September 24, 1998 a strong interplanetary shock reached the Wind spacecraft 185R E upstream of the Earth. When this hit the Earth the pressure at the nose of the magnetosphere went from 2nPa to 15nPa. The x-component of velocity was -900 km/s The IMF initially was horizontal but after 2 hours it turned southward and a strong storm began.
15 Bz GSM (nt) Dst Vx (km/s)
16
17 THEMIS recently discovered that (+/-) North-then-South polarity of CMEs results in 20 times more solar wind plasma penetrating Earth's magnetosphere ahead of a storm This causes a cold-dense plasma sheet prior to the storm Results in intense storm time ring current compared to (-/+) CMEs Boundary Layer under Northward IMF Boundary Layer under Southward IMF
18 Solar variability effects human activities in three ways. Space travelers can be exposed to potentially lethal radiation especially when carrying out activities outside of the spacecraft. Technology both in space and on the ground can be damaged especially during some magnetic storms. Satellites are damaged by energetic ions and electrons. High frequency communications used by airplanes (30-300MHz) can be disrupted. The Wide Area Augmentation System that uses Global Positioning Satellites to aid aircraft navigation can be disrupted by events that effect the GPS satellites and make precise approaches impossible. The power grid can be disrupted by induced currents during storms. There may be a relationship between terrestrial climate and solar activity.
19 When high energy particles encounter atoms or molecules within the human body, ionization may occur. Ionization can occur when the particle is stopped by an atom or molecule. The resulting radiation can ionize nearby atoms or molecules. Bremsstrahlung can also ionize atoms or molecules. A rad (Radiation Absorbed Dose) is the amount of ionizing radiation corresponding to 0.01 Joule absorbed by one kilogram of material. The SI unit for radiation is 1gray (1Gy) which is equal to 1J/kg = 1m 2 /s 2 The rad unit is independent of the type of radiation. ~100 rads will cause radiation sickness (1Gy = 100 rads). 1 Gy has a high probability of killing a cell by producing a lesion in its DNA. 1 rad from x-rays is less harmful than 1 rad from high energy protons. The relative biological effectiveness (RBE) of radiation is normalized to 200 kev x-rays to produce the equivalent biological effectiveness for the radiation being considered. For 200keV X- or γ-rays RBE=1. The SI unit is Sievert (1SV) but the rem is used (Radiation Equivalent in Man). 1 rem = 0.01SV. The biological damage is measured in rem (rem=dose(rad)x RBE). Electrons, protons, neutrons and alpha particles are the most damaging because they penetrate deeply into human tissue. The energy deposition in matter is quantified by the Linear Energy Transfer (LET). This energy deposition LET is equal to the radiation energy loss per unit distance, except when bremsstrahlung is emitted (travels far from particle track). For biological applications LET is measured in kev/μm For electronics applications LET is measured in MeV cm 2 /mg; i.e., energy per distance divided by mass density.
20 The average person in the US gets ~170mr per year from radioactive elements around us, cosmic rays, food and water. Astronauts must worry about a number of sources. Solar energetic particle events (SEPs) Relativistic electron events (REE) Passages through the south Atlantic anomaly Radiation belts. Astronauts can receive several times the average annual dose in one short mission. At higher apogees astronauts can get hundreds of milli rads. The dose is lower at low latitudes than above 50 o. Doses are higher for extra-vehicular activities since space suits have little shielding. Protons >10 MeV penetrate typical suits. Spacecraft exteriors have several grams per cm 2 of aluminum shielding and can stop higher energy particles.
21
22 Spacecraft charging is a variation of the electrostatic potential of the spacecraft surface with respect to the surrounding plasma. The resulting discharges can: Cause spurious electronic switching Break down thermal coatings (kapton, blanket layers, Dag). Degrade amplifiers and solar cells Degrade optical sensors. Photoionization frees electrons from the spacecraft and it develops a positive charge. Electrons may form a negative cloud near the spacecraft. If the entire surface was a homogeneous conductor this would not be a problem but this isn t the case. Differential charging of the sunlit surface with respect to the dark surface, and poor conductance paths result in kilovolt potentials. Electrons with energies of a few kev can penetrate the skin of the spacecraft and charge that portion of the spacecraft negatively. Differential charging relative to the rest of the spacecraft develops. In shadow, the entire spacecraft becomes negatively charged.
23 Surface Charging: SCATHA Satellite Observations. SCATHA (Reagan et al., 1981)
24
25 Electrons with energies between 2 and 10 MeV have enough energy to get deep into satellite surfaces and results in component malfunction Excess charge spreads out evenly on conducting surfaces but the charge accumulates on dielectric surfaces resulting in potential differences between different parts of the satellite. Eventually static discharges occur. This can happen on electron circuitry. Plot shows count rate of 3 MeV electrons versus time. Arrows show times when the spacecraft star tracker had anomalies.
26 High Energy Electrons: Deep-Dialectric Charging 1. Electrons bury themselves in the insulator 4. Electrons build up faster than they leak off 2. Electrons slowly leak out of the insulator 5. Discharge (electrical spark) that damages or destroys the material 3. Influx of electrons increases to levels higher than the leakage rate
27
28 Single Event Effects (SEEs) Apply to both ground (cell phones, computers) and space Are the result of individual penetrating ion hits causing ionization that can temporarily or permanently damage a component Single Event Upsets or soft errors bit flips can result in I/O error Caused by:» Galactic cosmic rays» Solar Energetic Particles» Radiation Belts Result in:» Damage to stored data» Damage to software» Cause processor to write over critical data tables.» Create faulty commands. Single Event Latchups result in shortcircuit of power rails, and over-current, possibly permanently damaging component.
29 Background caused by Solar Energetic Particles
30 Other Hazards from Space Weather: Spacecraft operating below a few thousand kilometers encounter a significant number of atmospheric particles during each orbit. Any mechanism that heats the atmosphere will produce density increases above the level heated. Geomagnetic storms Changes in solar extreme ultraviolet (EUV) radiation. Heating during magnetic storms Strong field-aligned currents and enhanced electrojets contribute to atmospheric heating. Most of the heating is in the auroral zone so polar orbiting satellites experience the greatest effects. Enhanced drag can cause satellites to reenter the atmosphere. Enhanced drag at perigee will cause the orbit to become more circular and increase the interval with drag. Even a single density increase will alter all future orbits.
31 At auroral latitudes currents induced by magnetospheric activity can interfere with the transmission of electrical power. One major blackout was caused by this in Quebec. Numerous studies have suggested that solar events can effect terrestrial atmospheric weather. The Maunder minimum was a little ice age. There is some evidence that penetrating particles can influence cloud formation. These ideas are highly controversial. Precipitating high energy electrons may contribute to ozone depletion.
32 Area affected by blackout. Transformers destroyed by induced currents. Transformer winding failure Transformer exit lead overheating
33
Even if not soon to. humans will still be in Space (ISS)
ESS 7 Lectures 22 and 23 May 28 and June 2, 2010 Humans in Space Even if not soon to the Moon or Mars, humans will still be in Space (ISS) NASA Feb 19 2010 Radiation Doses and Risks When high energy particles
More informationbestbuy.com Mgccl.com
ESS 7 Lectures 18, 19 and 20 May 17, 19 and 21, 2010 Technology and Space Weather bestbuy.com Mgccl.com www.goes.noaa.gov Space Weather Effects on Satellite Lifetimes: Atmospheric Drag A satellite would
More informationHow is Earth s Radiation Belt Variability Controlled by Solar Wind Changes
How is Earth s Radiation Belt Variability Controlled by Solar Wind Changes Richard M. Thorne Department of Atmospheric and Oceanic Sciences, UCLA Electron (left) and Proton (right) Radiation Belt Models
More informationSpace Weather and Satellite System Interaction
Space Engineering International Course, Kyutech, 4 th Quarter Semester 2017 Space Weather and Satellite System Interaction Lecture 2: Space Weather Concept, Reporting and Forecasting Assoc. Prof. Ir. Dr.
More informationDYNAMICS OF THE EARTH S MAGNETOSPHERE
DYNAMICS OF THE EARTH S MAGNETOSPHERE PROF JIM WILD j.wild@lancaster.ac.uk @jim_wild With thanks to: Stan Cowley, Rob Fear & Steve Milan OUTLINE So far: Dungey cycle - the stirring of the magnetosphere
More informationChapter 8 Geospace 1
Chapter 8 Geospace 1 Previously Sources of the Earth's magnetic field. 2 Content Basic concepts The Sun and solar wind Near-Earth space About other planets 3 Basic concepts 4 Plasma The molecules of an
More informationGeomagnetic Disturbance Report Reeve Observatory
Event type: Various geomagnetic disturbances including coronal hole high-speed stream, coronal mass ejection, sudden impulse and reverse shock effects Background: This background section defines the various
More informationMagnetic Reconnection
Magnetic Reconnection? On small scale-lengths (i.e. at sharp gradients), a diffusion region (physics unknown) can form where the magnetic field can diffuse through the plasma (i.e. a breakdown of the frozenin
More informationGeomagnetic storms. Measurement and forecasting
Geomagnetic storms. Measurement and forecasting Anna Gustavsson 17 October 2006 Project of the Space Physics Course 2006 Umeå University 1 Introduction Effects of magnetic storms on technology Geomagnetic
More informationINTERPLANETARY ASPECTS OF SPACE WEATHER
INTERPLANETARY ASPECTS OF SPACE WEATHER Richard G. Marsden Research & Scientific Support Dept. of ESA, ESTEC, P.O. Box 299, 2200 AG Noordwijk, NL, Email: Richard.Marsden@esa.int ABSTRACT/RESUME Interplanetary
More informationThe Structure of the Magnetosphere
The Structure of the Magnetosphere The earth s magnetic field would resemble a simple magnetic dipole, much like a big bar magnet, except that the solar wind distorts its shape. As illustrated below, the
More informationIn-Situ vs. Remote Sensing
In-Situ vs. Remote Sensing J. L. Burch Southwest Research Institute San Antonio, TX USA Forum on the Future of Magnetospheric Research International Space Science Institute Bern, Switzerland March 24-25,
More informationTime Series of Images of the Auroral Substorm
ESS 7 Lecture 13 October 27, 2010 Substorms Time Series of Images of the Auroral Substorm This set of images in the ultra-violet from the Polar satellite shows changes that occur during an auroral substorm.
More informationThe Dynamic Magnetosphere. Ioannis A. Daglis. National Observatory of Athens, Greece
310/1749-42 ICTP-COST-USNSWP-CAWSES-INAF-INFN International Advanced School on Space Weather 2-19 May 2006 The Dynamic Magnetosphere: Reaction to and Consequences of Solar Wind Variations Yannis DAGLIS
More informationHigh energy particles from the Sun. Arto Sandroos Sun-Earth connections
High energy particles from the Sun Arto Sandroos Sun-Earth connections 25.1.2006 Background In addition to the solar wind, there are also particles with higher energies emerging from the Sun. First observations
More informationESS 200C Aurorae. Lecture 15
ESS 200C Aurorae Lecture 15 The record of auroral observations dates back thousands of years to Greek and Chinese documents. The name aurora borealis (latin for northern dawn) was coined in 1621 by P.
More informationThe Solar wind - magnetosphere - ionosphere interaction
The Solar wind - magnetosphere - ionosphere interaction Research seminar on Sun-Earth connections Eija Tanskanen Friday January 27, 2006 12-14 a.m., D115 Outline 1. Basics of the Earth s magnetosphere
More informationcos 6 λ m sin 2 λ m Mirror Point latitude Equatorial Pitch Angle Figure 5.1: Mirror point latitude as function of equatorial pitch angle.
Chapter 5 The Inner Magnetosphere 5.1 Trapped Particles The motion of trapped particles in the inner magnetosphere is a combination of gyro motion, bounce motion, and gradient and curvature drifts. In
More informationTHE SOLAR WIND & SOLAR VARIABILITY
The Sun-Earth System: CONTENTS AN OVERVIEW The Stars Around Us 1 Our Dependence on the Sun 3 The Sun s Inconstancy 3 Intruders from Afar 5 What Gets By 5 Voyages of Discovery in an Age of Exploration 6
More informationCollege Physics B - PHY2054C
College - PHY2054C Physics - Radioactivity 11/24/2014 My Office Hours: Tuesday 10:00 AM - Noon 206 Keen Building Review Question 1 Isotopes of an element A have the same number of protons and electrons,
More informationResponse of the Earth s magnetosphere and ionosphere to the small-scale magnetic flux rope in solar wind by the MHD simulation
Response of the Earth s magnetosphere and ionosphere to the small-scale magnetic flux rope in solar wind by the MHD simulation Kyung Sun Park 1, Dae-Young Lee 1, Myeong Joon Kim 1, Rok Soon Kim 2, Kyungsuk
More informationIntroduction to Space Weather
Introduction to Space Weather We may have been taught that there is a friendly, peaceful nonhostile relationship between the Sun and the Earth and that the Sun provides a constant stream of energy and
More informationSPACECRAFT CHARGING: OBSERVATIONS AND RELATIONSHIP TO SATELLITE ANOMALIES
SPACECRAFT CHARGING: OBSERVATIONS AND RELATIONSHIP TO SATELLITE ANOMALIES J. F. Fennell, H. C. Koons, J. L. Roeder, and J. B. Blake The Aerospace Corporation, Los Angeles, CA, 90009, USA (Phone:+1 310
More informationWHAT IS IONIZING RADIATION
WHAT IS IONIZING RADIATION Margarita Saraví National Atomic Energy Commission - Argentina Workshop on Ionizing Radiation SIM Buenos Aires 10 November 2011 What is ionizing radiation? What is ionizing radiation?
More informationThis project has received funding from the European Union s Horizon 2020 research and innovation programme under the Marie-Sklodowska-Curie grant
This project has received funding from the European Union s Horizon 2020 research and innovation programme under the Marie-Sklodowska-Curie grant agreement number 721624. Space weather and the variable
More informationNuclear Spectroscopy: Radioactivity and Half Life
Particle and Spectroscopy: and Half Life 02/08/2018 My Office Hours: Thursday 1:00-3:00 PM 212 Keen Building Outline 1 2 3 4 5 Some nuclei are unstable and decay spontaneously into two or more particles.
More informationThe Magnetic Sun. CESAR s Booklet
The Magnetic Sun CESAR s Booklet 1 Introduction to planetary magnetospheres and the interplanetary medium Most of the planets in our Solar system are enclosed by huge magnetic structures, named magnetospheres
More informationSpace Physics: Recent Advances and Near-term Challenge. Chi Wang. National Space Science Center, CAS
Space Physics: Recent Advances and Near-term Challenge Chi Wang National Space Science Center, CAS Feb.25, 2014 Contents Significant advances from the past decade Key scientific challenges Future missions
More informationSpace Weather. ~ Affects of solar activities onto Earth. Cause-Effect Time Intervals range from immediate (precisely, 8 minutes) to several days.
Space Weather ~ Affects of solar activities onto Earth Cause-Effect Time Intervals range from immediate (precisely, 8 minutes) to several days. days Two difficulties arise for forecasting (modelling):
More informationPlanned talk schedule. Substorm models. Reading: Chapter 9 - SW-Magnetospheric Coupling from Russell book (posted)
Reading: Chapter 9 - SW-Magnetospheric Coupling from Russell book (posted) Today: Example of dynamics/time variation Review of intro to auroral substorms Substorm models How do we know a substorm is occurring?
More informationSpecification of electron radiation environment at GEO and MEO for surface charging estimates
Specification of electron radiation environment at GEO and MEO for surface charging estimates Natalia Ganushkina (University of Michigan/FMI) Collaborators: S. Dubyagin (FMI), J.-C. Matéo Vélez, A. Sicard
More informationSpace Physics. An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres. May-Britt Kallenrode. Springer
May-Britt Kallenrode Space Physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres With 170 Figures, 9 Tables, Numerous Exercises and Problems Springer Contents 1. Introduction
More informationsample What happens when we are exposed to radiation? 1.1 Natural radiation Cosmic radiation
1.1 Natural radiation 3 1 What happens when we are exposed to radiation? 1.1 Natural radiation For as long as humans have walked the earth, we have continually been exposed to naturally-occurring radiation.
More informationEarth s Magnetosphere
Earth s Magnetosphere General Description of the Magnetosphere Shape Pressure Balance The Earth s Magnetic Field The Geodynamo, Magnetic Reversals, Discovery Current Systems Chapman Ferraro Cross Tail
More informationAtmospheric Structure
Atmospheric Structure The gaseous area surrounding the planet is divided into several concentric strata or layers. About 99% of the total atmospheric mass is concentrated in the first 20 miles (32 km)
More informationSTUDY ON RELATIONSHIP OF MAGNETOSPHERIC SUBSTORM AND MAGNETIC STORM
Prosiding Seminar Nasional Penelitian, Pendidikan dan Penerapan MIPA Fakultas MIPA, Universitas Negeri Yogyakarta, 16 Mei 2009 STUDY ON RELATIONSHIP OF MAGNETOSPHERIC SUBSTORM AND MAGNETIC STORM L. Muhammad
More informationBIRA-IASB, 30th October 2006
Satellite Anomalies and Launch Failures: Space Weather Connection by Natalia Romanova (runatka@mail.ru) Belgian Institute for Space Aeronomy Institute of the Physics of the Earth, Moscow, Russia BIRA-IASB,
More informationAndrew Keen, Inari, Finland 18 Feb º C spaceweather.com
ESS 7 Lecture 17 May 14, 2010 The Aurora Aurora Amazing Light Show Andrew Keen, Inari, Finland 18 Feb 2010-31º C spaceweather.com Athabasca Aurora Oct 3 2003 Courtesy Mikko Syrjäsuo There is a Long Record
More informationLow energy electrons in the inner Earth s magnetosphere
Low energy electrons in the inner Earth s magnetosphere Natalia Ganushkina (1, 2) (1) University of Michigan, Ann Arbor MI, USA (2) Finnish Meteorological Institute, Helsinki, Finland The research leading
More informationSubstorms at Mercury: Old Questions and New Insights. Daniel N. Baker Laboratory for Atmospheric and Space Physics (LASP)
Substorms at Mercury: Old Questions and New Insights Daniel N. Baker Laboratory for Atmospheric and Space Physics (LASP) Outline of Presentation Introduction Substorms in the Earth s Magnetosphere Prior
More informationRemote sensing of magnetospheric processes: Lesson 1: Configura7on of the magnetosphere
Remote sensing of magnetospheric processes: Lesson 1: Configura7on of the magnetosphere AGF-351 Optical methods in auroral physics research UNIS, 24.-25.11.2011 Anita Aikio Dept. Physics University of
More informationUppsala universitet Institutionen för astronomi och rymdfysik Anders Eriksson
Tentamen för Rymdfysik I 2006-08-15 Uppsala universitet Institutionen för astronomi och rymdfysik Anders Eriksson Please write your name on all papers, and on the first page your address, e-mail and phone
More informationOutline. Radiation Interactions. Spurs, Blobs and Short Tracks. Introduction. Radiation Interactions 1
Outline Radiation Interactions Introduction Interaction of Heavy Charged Particles Interaction of Fast Electrons Interaction of Gamma Rays Interactions of Neutrons Radiation Exposure & Dose Sources of
More informationLET! (de / dx) 1 Gy= 1 J/kG 1Gy=100 rad. m(kg) dose rate
Basics of Radiation Dosimetry for the Physicist http://en.wikipedia.org/wiki/ionizing_radiation I. Ionizing radiation consists of subatomic particles or electromagnetic waves that ionize electrons along
More informationSubstorm-associated effects in the variations of low energy electron fluxes in the inner magnetosphere: Does the substorm s strength matter?
Substorm-associated effects in the variations of low energy electron fluxes in the inner magnetosphere: Does the substorm s strength matter? N. Ganushkina (1, 2), S. Dubyagin (1), I. Sillanpää (1), D.
More informationThe Auroral Zone: Potential Structures in Field and Density Gradients
The Auroral Zone: Potential Structures in Field and Density Gradients David Schriver May 8, 2007 Global Kinetic Modeling: week 10 Foreshock (week 3) Auroral zone (week 7) (week 8) Radiation Belt (week
More informationChapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He
Our sole source of light and heat in the solar system A common star: a glowing ball of plasma held together by its own gravity and powered by nuclear fusion at its center. Nuclear fusion: Combining of
More informationSolar-Wind/Magnetosphere Coupling
Solar-Wind/Magnetosphere Coupling Joe Borovsky Space Science Institute --- University of Michigan 1. Get a feeling for how the coupling works 2. Get an understanding of how reconnection works 3. Look at
More informationPROBLEM 1 (15 points) In a Cartesian coordinate system, assume the magnetic flux density
PROBLEM 1 (15 points) In a Cartesian coordinate system, assume the magnetic flux density varies as ( ) where is a constant, is the unit vector in x direction. a) Sketch the magnetic flux density and the
More informationThe Sun sends the Earth:
The Sun sends the Earth: Solar Radiation - peak wavelength.visible light - Travels at the speed of light..takes 8 minutes to reach Earth Solar Wind, Solar flares, and Coronal Mass Ejections of Plasma (ionized
More informationLow energy electron radiation environment for extreme events
Low energy electron radiation environment for extreme events Natalia Ganushkina (1, 2) and Stepan Dubyagin (1) Special thanks to Jean-Charles Matéo-Vélez (3) (1) Finnish Meteorological Institute, Helsinki,
More informationIonospheric Tomography II: Ionospheric Tomography II: Applications to space weather and the high-latitude ionosphere
Ionospheric Tomography II: Ionospheric Tomography II: Applications to space weather and the high-latitude ionosphere Why tomography at high latitudes? Why tomography at high latitudes? Magnetic field railway
More informationCosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time.
Cosmic Rays 1. Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked' away in time, and this could never be prevented, no matter how good the
More informationAuroral Disturbances During the January 10, 1997 Magnetic Storm
Auroral Disturbances During the January 10, 1997 Magnetic Storm L. R. Lyons and E. Zesta J. C. Samson G. D. Reeves Department of Atmospheric Sciences Department of Physics NIS-2 Mail Stop D436 University
More informationSolar-terrestrial relation and space weather. Mateja Dumbović Hvar Observatory, University of Zagreb Croatia
Solar-terrestrial relation and space weather Mateja Dumbović Hvar Observatory, University of Zagreb Croatia Planets Comets Solar wind Interplanetary magnetic field Cosmic rays Satellites Astronauts HELIOSPHERE
More informationA NEW MODEL FOR REALISTIC 3-D SIMULATIONS OF SOLAR ENERGETIC PARTICLE EVENTS
A NEW MODEL FOR REALISTIC 3-D SIMULATIONS OF SOLAR ENERGETIC PARTICLE EVENTS Nicolas Wijsen KU Leuven In collaboration with: A. Aran (University of Barcelona) S. Poedts (KU Leuven) J. Pomoell (University
More information! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun. The Sun & Solar Activity
! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun The Sun & Solar Activity The Sun in Perspective Planck s Law for Black Body Radiation ν = c / λ
More informationUnderstanding Solar Indices
Understanding Solar Indices By Ken Larson KJ6RZ Long distance HF radio communications is made possible by a region of charged particles in the Earth s upper atmosphere, 30 to 200 miles above the Earth
More informationIntroduction to the Sun and the Sun-Earth System
Introduction to the Sun and the Sun-Earth System Robert Fear 1,2 R.C.Fear@soton.ac.uk 1 Space Environment Physics group University of Southampton 2 Radio & Space Plasma Physics group University of Leicester
More informationDifferences between CME associated and CH associated RED events during 2005
Bull. Astr. Soc. India (2007) 35, 539 547 Differences between CME associated and CH associated RED events during 2005 Radharani Alyana 1, Girija Rajaram 1, Jatin Rathod 1, A. Chandrasekhar Reddy 1, D.
More informationDIN EN : (E)
DIN EN 16603-10-04:2015-05 (E) Space engineering - Space environment; English version EN 16603-10-04:2015 Foreword... 12 Introduction... 13 1 Scope... 14 2 Normative references... 15 3 Terms, definitions
More informationMagnetospheric Currents at Quiet Times
Magnetospheric Currents at Quiet Times Robert L. McPherron Institute of Geophysics and Planetary Physics University of California Los Angeles Los Angeles, CA 90095-1567 e-mail: rmcpherron@igpp.ucla.edu
More informationSPACE WEATHER: STORMS FROM THE SUN
GIFT 2013 - Natural Hazards Vienna, Austria, 10 April 2013 SPACE WEATHER: STORMS FROM THE SUN Norma B. Crosby Belgian Institute for Space Aeronomy Ringlaan-3-Avenue Circulaire, B-1180 Brussels, Belgium
More informationProject report. Spacecraft Charging and Mitigation Methods. By Muhammad Azam. Abstract
Umeå University October 7, 2009 Department of physics Space physics 7.5 ECTS. Project report Spacecraft Charging and Mitigation Methods By Muhammad Azam Muhammad.azam1@yahoo.com Supervisor Kjell Rönnmark
More informationGLOSSARY OF BASIC RADIATION PROTECTION TERMINOLOGY
GLOSSARY OF BASIC RADIATION PROTECTION TERMINOLOGY ABSORBED DOSE: The amount of energy absorbed, as a result of radiation passing through a material, per unit mass of material. Measured in rads (1 rad
More informationRationale for a European Space Weather Programme
Rationale for a European Space Weather Programme Hannu Koskinen Finnish Meteorological Institute ESWS Final Presentation ESTEC, 6 December, 2001 Scope WP 300 of ESWS: Establishment of detailed rationale
More informationSpace Weather. S. Abe and A. Ikeda [1] ICSWSE [2] KNCT
Space Weather S. Abe and A. Ikeda [1] ICSWSE [2] KNCT Outline Overview of Space Weather I. Space disasters II. Space weather III. Sun IV. Solar wind (interplanetary space) V. Magnetosphere VI. Recent Space
More informationEffect of Solar Flare X-Rays on digisonde fmin values. S. C. Tripathi H. Haralambous
Effect of Solar Flare X-Rays on digisonde fmin values S. C. Tripathi H. Haralambous SOLAR FLARE Solar flares occur when the sun's magnetic field twists up and reconnects, blasting energy outward and superheating
More informationMAE 5595: Space Environments and Spacecraft Interactions. Lesson 4: Introduction
MAE 5595: Space Environments and Spacecraft Interactions Lesson 4: Introduction Ambient Environment Neutral Environment Low pressure environment (150km ~ 3x10-9 atm) Ambient neutral gas (LEO atomic oxygen)
More informationMAGNETISM QUIZ MAGNETISM
MAGNETISM QUIZ MAGNETISM 1. What force steers particles in a supercollider? A. Centrifugal B. Electric C. Magnetic D. Gravity 2. What can we learn from the paths of charged particles after a supercollider
More informationThe Sun ASTR /17/2014
The Sun ASTR 101 11/17/2014 1 Radius: 700,000 km (110 R ) Mass: 2.0 10 30 kg (330,000 M ) Density: 1400 kg/m 3 Rotation: Differential, about 25 days at equator, 30 days at poles. Surface temperature: 5800
More informationSolar Terrestrial Influences on Climate during Geomagnetic Reversals
Solar Terrestrial Influences on Climate during Geomagnetic Reversals Glatzmaier, G.A., and P. Olson (2005), Probing the Geodynamo, Scientific American Special Edition, 15(2), 28. Robert L. McPherron Institute
More information1 Introduction. Cambridge University Press Physics of Space Plasma Activity Karl Schindler Excerpt More information
1 Introduction Space plasma phenomena have attracted particular interest since the beginning of the exploration of space about half a century ago. Already a first set of pioneering observations (e.g.,
More informationRadiation Terminology
Radiation Terminology This section discusses the terms and concepts which are necessary for a meaningful discussion of radiation, its sources, and its risks. USNRC Technical Training Center 5-1 0703 Energy
More informationTwo types of geomagnetic storms and relationship between Dst and AE indexes
Two types of geomagnetic storms and relationship between Dst and AE indexes Lyudmila P. Shadrina 1, * 1 Academy of sciences of Sakha (Yakutia) Republic, Yakutsk, Russia Abstract. The study of the relationship
More informationSolar Flare Durations
Solar Flare Durations Whitham D. Reeve 1. Introduction Scientific investigation of solar flares is an ongoing pursuit by researchers around the world. Flares are described by their intensity, duration
More informationRadiation and Radioactivity. PHYS 0219 Radiation and Radioactivity
Radiation and Radioactivity 1 Radiation and Radioactivity This experiment has four parts: 1. Counting Statistics 2. Gamma (g) Ray Absorption Half-length and shielding 3. 137 Ba Decay Half-life 4. Dosimetry
More informationNASA Future Magnetospheric Missions. J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC
NASA Future Magnetospheric Missions J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC Future Magnetospheric Missions Strategic Missions Radiation Belt Storm Probes (LWS/2011) Magnetospheric
More informationINCREASED LEVEL OF UV AND X-RAY RADIATION
INCREASED LEVEL OF UV AND X-RAY RADIATION By Senem ÜNAL Page 1 WHAT IS UV AND X-RAY? The sun radiates energy in a wide range of wavelengths, most of which are invisible to human eyes. The shorter the wavelength,
More informationChapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds Pearson Education, Inc.
Chapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds 10.1 Atmospheric Basics Our goals for learning: What is an atmosphere? How does the greenhouse effect warm a planet? Why do atmospheric
More informationCHAPTER 2 DATA. 2.1 Data Used
CHAPTER DATA For the analysis, it is required to use geomagnetic indices, which are representatives of geomagnetic activity, and Interplanetary Magnetic Field (IMF) data in addition to f F,which is used
More informationLong term data for Heliospheric science Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt, MD 20771, USA
Long term data for Heliospheric science Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt, MD 20771, USA IAU340 1-day School, Saturday 24th February 2018 Jaipur India CMEs & their Consequences
More informationDavid versus Goliath 1
David versus Goliath 1 or A Comparison of the Magnetospheres between Jupiter and Earth 1 David and Goliath is a story from the Bible that is about a normal man (David) who meets a giant (Goliath) Tomas
More informationTracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus
Tracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus In June 2015, the Sun emitted several M-Class flares over a 2-day period. These flares were concurrent with
More informationGeomagnetic Disturbances (GMDs) History and Prediction
Geomagnetic Disturbances (GMDs) History and Prediction J. Patrick Donohoe, Ph.D., P.E. Dept. of Electrical and Computer Engineering Mississippi State University Box 9571 Miss. State, MS 39762 donohoe@ece.msstate.edu
More informationSolar Particle Events in Aviation and Space. Günther Reitz Insitute of Aerospace Medicine German Aerospace Center, DLR, Cologne, Germany
Solar Particle Events in Aviation and Space Günther Reitz Insitute of Aerospace Medicine German Aerospace Center, DLR, Cologne, Germany Radiation Field in the Heliosphere LEO orbit Fluxes of primary space
More informationSun Earth Connection Missions
Sun Earth Connection Missions ACE Advanced Composition Explorer The Earth is constantly bombarded with a stream of accelerated particles arriving not only from the Sun, but also from interstellar and galactic
More informationThe Cosmic Perspective Planetary Atmospheres: Earth and the Other Terrestrial Worlds
Chapter 10 Lecture The Cosmic Perspective Seventh Edition Planetary Atmospheres: Earth and the Other Terrestrial Worlds Planetary Atmospheres: Earth and the Other Terrestrial Worlds 10.1 Atmospheric Basics
More informationSpace Radiation Mitigation for Fox-1
AMSAT Space Symposium 2012 Space Radiation Mitigation for Fox-1 Alan Biddle WA4SCA Tony Monteiro AA2TX Space Radiation Components Type Source Composition Trapped Particles in Van Allen Belts Galactic Cosmic
More informationSolar and Interplanetary Disturbances causing Moderate Geomagnetic Storms
J. Astrophys. Astr. (2008) 29, 263 267 Solar and Interplanetary Disturbances causing Moderate Geomagnetic Storms Santosh Kumar, M. P. Yadav & Amita Raizada Department of P.G. Studies and Research in Physics
More informationSpace weather. Introduction to lectures by Dr John S. Reid. Image courtesy:
Space weather Introduction to lectures by Dr John S. Reid Image courtesy: http://www.astro-photography.com/ss9393.htm Sunspot 9393 First pass from late March to early April, 2001 See: Storms from the Sun
More informationBASIC OF RADIATION; ORIGIN AND UNITS
INAYA MEDICAL COLLEGE (IMC) RAD 243 - LECTURE 2 BASIC OF RADIATION; ORIGIN AND UNITS DR. MOHAMMED MOSTAFA EMAM LECTURES & CLASS ACTIVITIES https://inayacollegedrmohammedemam.wordpress.com/ Password: drmohammedemam
More informationIntroduction to the Sun-Earth system Steve Milan
Introduction to the Sun-Earth system Steve Milan steve.milan@ion.le.ac.uk The solar-terrestrial system Corona is so hot that the Sun s gravity cannot hold it down it flows outwards as the solar wind A
More informationPS-21 First Spring Institute say : Teaching Physical Science. Radioactivity
PS-21 First Spring Institute say 2012-2013: Teaching Physical Science Radioactivity What Is Radioactivity? Radioactivity is the release of tiny, highenergy particles or gamma rays from the nucleus of an
More informationRadiation Safety Talk. UC Santa Cruz Physics 133 Winter 2018
Radiation Safety Talk UC Santa Cruz Physics 133 Winter 2018 Outline Types of radiation Sources of radiation Dose limits and risks ALARA principle Safety procedures Types of radiation Radiation is energy
More informationSolar Activity Space Debris
The Hazards To Space Systems Solar Activity Space Debris The Threat From The Sun Major solar events, (Solar Flares and Coronal Mass Ejections) have the potential to generate significant effects on satellites,
More informationThe Physics of Space Plasmas
The Physics of Space Plasmas Magnetic Storms and Substorms William J. Burke 14 November 2012 University of Massachusetts, Lowell Lecture 9 Course term-paper topics Geomagnetic Storms: (continued ) Volland-Stern
More information12 Moderator And Moderator System
12 Moderator And Moderator System 12.1 Introduction Nuclear fuel produces heat by fission. In the fission process, fissile atoms split after absorbing slow neutrons. This releases fast neutrons and generates
More informationSolar Activity The Solar Wind
Solar Activity The Solar Wind The solar wind is a flow of particles away from the Sun. They pass Earth at speeds from 400 to 500 km/s. This wind sometimes gusts up to 1000 km/s. Leaves Sun at highest speeds
More informationElectron Acceleration and Loss in the Earth s Radiation Belts: The Contribution of Wave- particle Interactions
Electron Acceleration and Loss in the Earth s Radiation Belts: The Contribution of Wave- particle Interactions Richard B Horne British Antarctic Survey R.Horne@bas.ac.uk Outline Relevance Radiation belt
More information