The solar wind (in 90 minutes) Mathew Owens
|
|
- Charity Welch
- 8 years ago
- Views:
Transcription
1 The solar wind (in 90 minutes) Mathew Owens 5 th Sept 2013 STFC Advanced Summer School m.j.owens@reading.ac.uk
2 Overview There s simply too much to cover in 90 minutes Hope to touch on: Formation of the solar wind and the Heliosphere Parker Spiral Three-dimensional solar wind Structure: Corotating interaction regions and transients Solar wind variability over centuries/millenia Apologies to: Turbulence and fine-scale structure Space weather Magnetospheric and ionospheric physics Solar-climate studies 2
3 Sunspots evidence of photospheric structure
4 Eclipses evidence of a solar atmosphere STFC Summer School
5 Carrington - evidence for particles from the Sun 11:18am, 1 September 1859, Redhill Richard Carrington: observed a very bright flare on the Sun Next day: auroras down to very low latitudes (Cuba, Hawaii) Telegraph systems disrupted Evidence for particles from the Sun, travelling at ~2000 km/s to the Earth Corpuscular radiation STFC Summer School
6 Evidence of a constant wind - Comet tails evidence of a solar wind comets Biermann (1951): non-radial comet tails imply constant wind of few hundred km/s STFC Summer School
7 Temperature (K) Coronal temperatures K K K K Height above photosphere (km) K braiding of magnetic field by photospheric motions is central to coronal heating
8 Origin of the solar wind Magnetic carpet of loops Most closed, some extend far above solar surface Plasma flows out along field lines into space STFC Summer School
9 Solar wind source: corona Hot corona has much higher pressure than interstellar medium Thermal scale height greater than gravitational scale height Can t balance pressures with a static corona (Parker, 1957) Corona expands into space, forming the solar wind Note: in lower corona, plasma <<1: plasma follows field STFC Summer School
10 Parker s solution Parker(1958) was the first to propose a model of the solar wind assuming a steady flow of plasma independent of time, as opposed to a static corona. He began from the mass and momentum conservation equations, taking time derivatives as zero since considering a steady flow. u 0 u. u p j B F g Found a solution of the form u 2 2kBT 1 du 4 m u dr kbt mr GM r 2 S
11 Possible solutions of the Parker solar wind equation
12 First solar wind observations Mariner 2 in
13 The heliosphere The cavity in our local interstellar wind termination shock heliopause interstellar wind dominated by the solar wind and Sun s magnetic field heliosheath bow shock
14 MHD simulations of the heliosphere Solar wind is confined in a cavity in interstellar space called the heliosphere that surrounds all the planets of the solar system Density is enhanced behind bow shock in heliosheath Termination shock heliopause heliosheath interstellar wind bow shock
15 A stellarsphere Hubble observations of the heliosheath behind the bow shock where the heliosphere of LL Ori heliosphere meets its (dense) local interstellar wind in the Orion nebula heliosheath bow shock interstellar wind heliopause
16 A stellarsphere Gemini adaptive optics observations near the galactic centre bow shock fast-moving star galactic centre heliosheath
17 Frozen-in theorem: The convective limit THE INDUCTION EQUATION B/ t = (V B ) + 2 B /( o ) convective term MAGNETIC REYNOLDS NUMBER diffusive term R m = { (V B ) } / { 2 B /( o )} { (V B ) } V c B c / L c ; { 2 B /( o ) } {B c / L c 2 } {1/( o )} Thus R m o V c L c Region (mhos m -1 ) V c (m s -1 ) L c (m) R m Base of corona AU Thus R m o V c L c >> 1 so B/ t = (V B ) this is the convective limit & leads to the frozen-in flux theorem
18 Frozen-in theorem: The convective limit ( by definition of B ) Charged particle motions Magnetic Field B Lorentz Force B B
19 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 1 Field is frozen-in to the solar wind flow
20 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 2 Field is frozen-in to the solar wind flow
21 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 3 Field is frozen-in to the solar wind flow
22 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 4 Field is frozen-in to the solar wind flow
23 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 5 Field is frozen-in to the solar wind flow
24 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 6 Field is frozen-in to the solar wind flow
25 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 7 Field is frozen-in to the solar wind flow
26 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 8 Field is frozen-in to the solar wind flow
27 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 9 Field is frozen-in to the solar wind flow
28 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 10 Field is frozen-in to the solar wind flow
29 Parker spiral Solar wind flow is radial Sun Solar rotation and radial solar wind generates a Parker spiral field structure 11 Field is frozen-in to the solar wind flow
30 Interplanetary scintillation
31 Interplanetary scintillation Solar rotation and radial solar wind generates a Parker spiral field structure Co-rotates with the solar corona (every 27 days in Earth s frame)
32 X-ray observations of flare particles Tracked by Ulysses satellite, looking down on ecliptic plane from over solar pole, using X-rays generated by super-thermal flare electrons moving along the field lines through the thermal solar wind
33 Calculating the Parker Spiral t left Sun at time t V SW t left Sun at time t+ t r r r t tan = r t / (V SW t) = tan -1 (r /V SW ) Sun
34 Observations of the spiral angle Y X X V sw = km s -1 Y X X V sw = km s -1 Colour histograms: Observed distributions of for , divided into 9 V SW ranges giving equal numbers of samples (grey) range and (black) average predicted by frozen-in = tan -1 {V SW /(r )} Y V sw = km s -1 Y V sw = km s -1 Spiral unwinds for higher V sw - as predicted by thory
35 Observations of the spiral angle V sw = km s -1
36 Observations of the spiral angle V sw = km s -1
37 Observations of the spiral angle V sw = km s -1
38 Observations of the spiral angle V sw = km s -1
39 Parker spiral angle at 1 AU 39
40 Solar wind effect on the corona The heliospheric magnetic field is a result of the Sun s magnetic field being carried outward, frozen in to the solar wind. Within the corona, the magnetic field forces dominate the plasma forces. As the field strength decreases with distance, beyond the Alfvén radius at a few solar radii, the plasma flow becomes dominant, and the field lines are constrained to move with the solar wind. Model of Pneumann and Kopp (1971)
41 Modelling the corona 41
42 The coronal source surface 42
43 PFSS solutions Magnetic field polarity at coronal source surface 43
44 Ulysses
45 Three-dimensional structure of interplanetary magnetic field 45
46 Heliospheric Ulysses passages above the current maximum latitude sheet of the current sheet STFC Advanced Summer School
47 Ulysses fast latitude scans 1 st - near sunspot min 2 nd - near sunspot max
48 B R invariance with latitude Radial flow at r > 10R S with B r independent of latitude V SW N Sun S Slight non-radial flow at r > 10R S to equalise P t & thus B r B r tangential pressure, P t B r2 / 2 o (as << 1)
49 Open Solar Flux Flux threading the coronal source surface closed field line Unsigned Flux, F U = + /2 2 - /2 0 B R r 2 cos( ) d d r = heliocentric distance B R = radial field = solar latitude = solar longitude open field lines STFC Advanced Summer School m.j.owens@reading.ac.uk
50 Open solar flux 50
51 Solar wind speed Sunspot minimum FAST Solar Wind in coronal holes SLOW Solar Wind in equatorial streamer belt Red = inward field Blue = outward field
52 Close to solar minimum the flow pattern close to the Sun can be approximated as a band of slow wind at low latitudes, centred on the Sun s dipole equator, with fast wind at all higher latitudes. This pattern of fast and slow solar wind is occasionally disturbed by transient flows associated with coronal mass ejections. Pizzo (1991) STFC Advanced Summer School m.j.owens@reading.ac.uk
53 Solar cycle evolution of speed
54 Characteristics of slow and fast solar wind Property at 1 AU Slow wind Fast wind Speed (v) ~400 km/s ~750 km/s Number density (n) ~10 cm 3 ~3 cm 3 Flux (nv) ~ cm 2 s 1 ~ cm 2 s 1 Magnetic field (Br) ~3 nt ~3 nt Proton temperature (Tp) ~ K ~ K Electron temperature(te) ~ K (>Tp) ~ K (<Tp) Composition (He/H) ~1 30% ~5% STFC Advanced Summer School m.j.owens@reading.ac.uk
55 Ionisation states Heavy ions (oxygen, carbon, magnesium) occur in small quantities in solar wind Ionisation states determined by temperature of plasma when collisional, in corona When collisionless, ionisation stares don t change Freezing-in temperature temperature of solar wind when collisions stop Diagnostic of conditions in corona where solar wind originates Very different in fast and slow solar wind STFC Summer School
56 Loop opening
57 Imaging the solar wind 57
58 Interaction of fast and slow wind If fast and slow solar wind streams at same latitude, fast can overtake slow Interaction: compression, can drive shocks 58
59 V (km/s) V T, V N (km/s) n p (cm -3 ) T p (x10 5 K) B (nt) B, B P Total (npa) V T V N FS HCS SI RW Day of 1992 B B In situ observations 59
60 Transient events - CMEs 60
61 In situ observations 61
62 Interaction with magnetosphere 62
63 Generation of energetic particles
64 Suprathermal electrons Owens and Crooker, 2008
65 CMEs add magnetic flux to the heliosphere 65
66
67
68
69
70
71
72
73 Cosmic rays Sunspot Number Huancauyo Hawaii neutron monitor counts (>13GV) Climax neutron monitor counts (>3GV)
74 14 C & 10 Be: spallation products from O, N & Ar 14 C 1/2 = 5370 yr < q G > = 2 atoms cm -2 s -1 GALACTIC COSMIC RAYS STRATOSPHERE ( 2/3) 10 Be 1/2 = yr < q G > = atoms cm -2 s C+0 14 C0 ; 14 C0+0H 14 C0 2 + H TROPOSPHERE ( 1/3) OCEANS ( ~1 year) ( ~1 week) 10 Be + AEROSOL BIOMASS ICE SHEETS
75 HMF reconstructions 75
76 Solar Modulation Parameter, (MV) Millennial Variation composite (40-year means) from cosmogenic isotopes 14 C & 10 Be 1000 we are still within recent grand maximum Year AD
77 Open questions Where does slow solar wind come from? How is the corona heated and the solar wind accelerated? What is the structure of the heliopause? How do CMEs mediate the solar cycle? How does the Sun evolve over centennial and millennial timescales? 77
78 The Future Solar Orbiter ESA-led mission Close to the Sun (0.23 AU) Orbit inclination to ecliptic (30 degrees) Launch in 2017? Lots of UK involvement (magnetometer at Imperial,, electron detector at MSSL) 78
Solar cycle. Auringonpilkkusykli. 1844 Heinrich Schwabe: 11 year solar cycle. ~11 years
Sun Solar cycle Auringonpilkkusykli 1844 Heinrich Schwabe: 11 year solar cycle ~11 years Auringonpilkkusykli Solar cycle Butterfly diagram: Edward Maunder 1904 New cycle Spots appear at mid-latitudes Migration
More informationSolar 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
More informationCoronal 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
More informationSolar atmosphere. Solar activity and solar wind. Reading for this week: Chap. 6.2, 6.3, 6.5, 6.7 Homework #2 (posted on website) due Oct.
Solar activity and solar wind Solar atmosphere Reading for this week: Chap. 6.2, 6.3, 6.5, 6.7 Homework #2 (posted on website) due Oct. 17 Photosphere - visible surface of sun. Only ~100 km thick. Features
More informationSolar 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
More informationThe 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
More informationSPACE WEATHER INTERPRETING THE WIND. Petra Vanlommel & Luciano Rodriguez
SPACE WEATHER INTERPRETING THE WIND Petra Vanlommel & Luciano Rodriguez THE SUN LOSES ENERGY Radiation Mass Particles THE SUN LOSES ENERGY PHYSICAL REPHRASING Total Solar Irradiance Solar Wind Fast Particles
More informationGEOPHYSICS AND GEOCHEMISTRY - Vol.III - Solar Wind And Interplanetary Magnetic Field - Schwenn R. SOLAR WIND AND INTERPLANETARY MAGNETIC FIELD
SOLAR WIND AND INTERPLANETARY MAGNETIC FIELD Schwenn R. Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany Keywords: Sun, corona, solar wind, plasma, magnetic field, reconnection, coronal mass
More informationSolar Wind: Global Properties
Solar Wind: Global Properties The most fundamental problem in solar system research is still unsolved: how can the Sun with a surface temperature of only 5800 K heat up its atmosphere to more than a million
More informationSpace 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
More informationWELCOME 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
More informationBulk 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
More informationSimultaneous Heliospheric Imager and Interplanetary Scintillation observations of CMEs and CIRs
Simultaneous Heliospheric Imager and Interplanetary Scintillation observations of CMEs and CIRs Gareth D. Dorrian (gdd05@aber.ac.uk) 1, Andy R. Breen 1, Jackie A. Davies 2, Alexis P. Rouillard 3, Mario
More informationThe 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
More informationCoronal 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
More informationProton 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
More informationSTUDY GUIDE: Earth Sun Moon
The Universe is thought to consist of trillions of galaxies. Our galaxy, the Milky Way, has billions of stars. One of those stars is our Sun. Our solar system consists of the Sun at the center, and all
More informationScience Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
More informationSolar 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
More informationName: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
More informationCSSAR 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
More informationChapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
More informationThe 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
More informationThe 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
More information8.1 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
More informationStudies on the ionospheric region during low solar activity in Brazil
Studies on the ionospheric region during low solar activity in Brazil Claudia M. N. Candido National Institute for Space Research - INPE Brazil 1 Plasma Bubbles-Spread-F OI 630.0-nm Peak at 250 km - F-layer
More informationJustin C. Kasper Harvard-Smithsonian Center for Astrophysics 2012 Heliophysics Summer School Boulder, CO
The Solar Wind Justin C. Kasper Harvard-Smithsonian Center for Astrophysics 2012 Heliophysics Summer School Boulder, CO Goals Origin of the solar wind Historical understanding of the solar wind Why study
More informationCalifornia 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,
More informationClass 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationSolar Wind and Interplanetary Magnetic Field: A Tutorial. C. T. Russell
Solar Wind and Interplanetary Magnetic Field: A Tutorial C. T. Russell Institute of Geophysics and Planetary Physics and Department of Earth and Space Sciences University of California, Los Angles California
More informationAcceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops
Acceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops L. A. Fisk 1, G. Gloeckler 1,2, T. H. Zurbuchen 1, J. Geiss 3, and N. A. Schwadron 4 1 Department
More informationLecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
More informationAcceleration of the solar wind as a result of the reconnection of open magnetic flux with coronal loops
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. A4, 1157, doi:10.1029/2002ja009284, 2003 Acceleration of the solar wind as a result of the reconnection of open magnetic flux with coronal loops L. A. Fisk
More informationSection 4: The Basics of Satellite Orbits
Section 4: The Basics of Satellite Orbits MOTION IN SPACE VS. MOTION IN THE ATMOSPHERE The motion of objects in the atmosphere differs in three important ways from the motion of objects in space. First,
More information2. 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
More informationLecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
More informationAy 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
More informationSpace Weather Research and Forecasting in CRL, Japan
Space Weather Research and Forecasting in CRL, Japan Maki Akioka Hiraiso Solar Observatory Communications Research Laboratory Contact akioka@crl.go.jp 1 Contents of Presentation 1.Space Weather Observation
More information1 Stellar winds and magnetic fields
1 Stellar winds and magnetic fields by Viggo Hansteen The solar wind is responsible for maintaining the heliosphere, and for being the driving agent in the magnetospheres of the planets but also for being
More informationL3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
More informationThe 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
More informationEarth-Sun Relationships. The Reasons for the Seasons
Earth-Sun Relationships The Reasons for the Seasons Solar Radiation The earth intercepts less than one two-billionth of the energy given off by the sun. However, the radiation is sufficient to provide
More informationThe 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
More informationSolar 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
More informationHeating & 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
More informationESCI 107/109 The Atmosphere Lesson 2 Solar and Terrestrial Radiation
ESCI 107/109 The Atmosphere Lesson 2 Solar and Terrestrial Radiation Reading: Meteorology Today, Chapters 2 and 3 EARTH-SUN GEOMETRY The Earth has an elliptical orbit around the sun The average Earth-Sun
More informationThe Limits of Our Solar System
The Limits of Our Solar System John D. Richardson Massachusetts Institute of Technology Nathan A. Schwadron Boston University Richardson and Schwadron: The Limits of Our Solar System 443 The heliosphere
More information2-1-5 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
More informationChapter 8 Formation of the Solar System. What theory best explains the features of our solar system? Close Encounter Hypothesis
Chapter 8 Formation of the Solar System What properties of our solar system must a formation theory explain? 1. Patterns of motion of the large bodies Orbit in same direction and plane 2. Existence of
More informationChapter Overview. Seasons. Earth s Seasons. Distribution of Solar Energy. Solar Energy on Earth. CHAPTER 6 Air-Sea Interaction
Chapter Overview CHAPTER 6 Air-Sea Interaction The atmosphere and the ocean are one independent system. Earth has seasons because of the tilt on its axis. There are three major wind belts in each hemisphere.
More informationSpace Weather Forecasting - Need and Importance
Coronal Magnetic Field Measurements: Space Weather Forecasting Needs D.N. Baker Laboratory for Atmospheric and Space Physics Department of Astrophysical and Planetary Sciences Department of Physics University
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationUsing 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
More informationTitan: The Solar System s Abiotic Petroleum Factory
Titan: The Solar System s Abiotic Petroleum Factory J. Hunter Waite, Ph.D. Institute Scientist Space Science & Engineering Division Southwest Research Institute Titan: The Solar System s Abiotic Petroleum
More informationThe 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
More informationChapter 8 Formation of the Solar System Agenda
Chapter 8 Formation of the Solar System Agenda Announce: Mercury Transit Part 2 of Projects due next Thursday Ch. 8 Formation of the Solar System Philip on The Physics of Star Trek Radiometric Dating Lab
More informationStatistical Study of Magnetic Reconnection in the Solar Wind
WDS'13 Proceedings of Contributed Papers, Part II, 7 12, 2013. ISBN 978-80-7378-251-1 MATFYZPRESS Statistical Study of Magnetic Reconnection in the Solar Wind J. Enžl, L. Přech, J. Šafránková, and Z. Němeček
More informationIntroduction 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
More informationLecture 19: Planet Formation I. Clues from the Solar System
Lecture 19: Planet Formation I. Clues from the Solar System 1 Outline The Solar System:! Terrestrial planets! Jovian planets! Asteroid belt, Kuiper belt, Oort cloud Condensation and growth of solid bodies
More informationSolar System Overview
Solar System Overview Planets: Four inner planets, Terrestrial planets Four outer planets, Jovian planets Asteroids: Minor planets (planetesimals) Meteroids: Chucks of rocks (smaller than asteroids) (Mercury,
More information1 A Solar System Is Born
CHAPTER 3 1 A Solar System Is Born SECTION Formation of the Solar System BEFORE YOU READ After you read this section, you should be able to answer these questions: What is a nebula? How did our solar system
More informationThe 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
More informationMultiple 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
More informationProgress Towards the Solar Dynamics Observatory
Progress Towards the Solar Dynamics Observatory Barbara J. Thompson SDO Project Scientist W. Dean Pesnell SDO Assistant Project Scientist Page 1 SDO OVERVIEW Mission Science Objectives The primary goal
More informationSPATIAL 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
More informationPresentation of problem T1 (9 points): The Maribo Meteorite
Presentation of problem T1 (9 points): The Maribo Meteorite Definitions Meteoroid. A small particle (typically smaller than 1 m) from a comet or an asteroid. Meteorite: A meteoroid that impacts the ground
More information5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
More informationRS platforms. Fabio Dell Acqua - Gruppo di Telerilevamento
RS platforms Platform vs. instrument Sensor Platform Instrument The remote sensor can be ideally represented as an instrument carried by a platform Platforms Remote Sensing: Ground-based air-borne space-borne
More informationUse the following image to answer the next question. 1. Which of the following rows identifies the electrical charge on A and B shown above?
Old Science 30 Physics Practice Test A on Fields and EMR Test Solutions on the Portal Site Use the following image to answer the next question 1. Which of the following rows identifies the electrical charge
More informationChapter 8 Welcome to the Solar System
Chapter 8 Welcome to the Solar System 8.1 The Search for Origins What properties of our solar system must a formation theory explain? What theory best explains the features of our solar system? What properties
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationInteraction of Energy and Matter Gravity Measurement: Using Doppler Shifts to Measure Mass Concentration TEACHER GUIDE
Interaction of Energy and Matter Gravity Measurement: Using Doppler Shifts to Measure Mass Concentration TEACHER GUIDE EMR and the Dawn Mission Electromagnetic radiation (EMR) will play a major role in
More informationPhysics 9e/Cutnell. correlated to the. College Board AP Physics 1 Course Objectives
Physics 9e/Cutnell correlated to the College Board AP Physics 1 Course Objectives Big Idea 1: Objects and systems have properties such as mass and charge. Systems may have internal structure. Enduring
More informationName Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
More informationEASA 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
More informationLARGE SCALE PROPERTIES OF THE INTERPLANETARY MAGNETIC FIELD
X-692-71-96 LARGE SCALE PROPERTIES OF THE INTERPLANETARY MAGNETIC FIELD KENNETH -. SCHATTEN '(A ~67 t4>(thru) 0 "(CODE) (NASA CR OR TMX OR AD NUMBER) (CATEGORY) MARCH 1971 GODDARD SPACE FLIGHT CENTER GREENBELT,
More informationGeneral Certificate of Education (A-level) January 2013 Physics A PHYA4 (Specification 2450) Unit 4: Fields and further mechanics Final Mark Scheme
Version 1.1 General Certificate of Education (A-level) January 013 Physics A PHYA4 (Specification 450) Unit 4: Fields and further mechanics Final Mark Scheme Mark schemes are prepared by the Principal
More informationPerspective and Scale Size in Our Solar System
Perspective and Scale Size in Our Solar System Notes Clue Session in Mary Gates RM 242 Mon 6:30 8:00 Read Lang Chpt. 1 Moodle Assignment due Thursdays at 6pm (first one due 1/17) Written Assignments due
More informationSolar System Fundamentals. What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System
Solar System Fundamentals What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System Properties of Planets What is a planet? Defined finally in August 2006!
More informationTHE SOLAR SYSTEM - EXERCISES 1
THE SOLAR SYSTEM - EXERCISES 1 THE SUN AND THE SOLAR SYSTEM Name the planets in their order from the sun. 1 2 3 4 5 6 7 8 The asteroid belt is between and Which planet has the most moons? About how many?
More informationCorso di Fisica Te T cnica Ambientale Solar Radiation
Solar Radiation Solar radiation i The Sun The Sun is the primary natural energy source for our planet. It has a diameter D = 1.39x10 6 km and a mass M = 1.989x10 30 kg and it is constituted by 1/3 of He
More informationAsteroids. Earth. Asteroids. Earth Distance from sun: 149,600,000 kilometers (92,960,000 miles) Diameter: 12,756 kilometers (7,926 miles) dotted line
Image taken by NASA Asteroids About 6,000 asteroids have been discovered; several hundred more are found each year. There are likely hundreds of thousands more that are too small to be seen from Earth.
More informationSeasonal & Daily Temperatures. Seasons & Sun's Distance. Solstice & Equinox. Seasons & Solar Intensity
Seasonal & Daily Temperatures Seasons & Sun's Distance The role of Earth's tilt, revolution, & rotation in causing spatial, seasonal, & daily temperature variations Please read Chapter 3 in Ahrens Figure
More informationSolar 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
More informationNonlinear processes in heliospheric plasma: models and observations
Mem. S.A.It. Vol. 74, 425 c SAIt 2003 Memorie della Nonlinear processes in heliospheric plasma: models and observations M. Velli 1, G. Einaudi 2, C. Chiuderi 1, P. L. Veltri 3, and the MM02242342 project
More informationSolar 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
More informationSummary: Four Major Features of our Solar System
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
More informationThe Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
More informationThe atmospheres of different planets
The atmospheres of different planets Thomas Baron October 13, 2006 1 Contents 1 Introduction 3 2 The atmosphere of the Earth 3 2.1 Description and Composition.................... 3 2.2 Discussion...............................
More informationBe Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
More informationExam # 1 Thu 10/06/2010 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti
Exam # 1 Thu 10/06/2010 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti INSTRUCTIONS: Please, use the `bubble sheet and a pencil # 2 to answer the exam questions, by marking
More information- 1 - Jennifer McClure. To: env.essay@physics.org. From: Jennifer McClure (j.m.mcclure@student.liverpool.ac.uk)
To: env.essay@physics.org Jennifer McClure From: Jennifer McClure (j.m.mcclure@student.liverpool.ac.uk) 1 st year Physics (F300), Department of Physics, University of Liverpool. - 1 - The Northern Lights;
More informationSunlight and its Properties. EE 495/695 Y. Baghzouz
Sunlight and its Properties EE 495/695 Y. Baghzouz The sun is a hot sphere of gas whose internal temperatures reach over 20 million deg. K. Nuclear fusion reaction at the sun's core converts hydrogen to
More informationUnit 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
More informationNuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
More informationArtificial Satellites Earth & Sky
Artificial Satellites Earth & Sky Name: Introduction In this lab, you will have the opportunity to find out when satellites may be visible from the RPI campus, and if any are visible during the activity,
More informationLecture 10 Formation of the Solar System January 6c, 2014
1 Lecture 10 Formation of the Solar System January 6c, 2014 2 Orbits of the Planets 3 Clues for the Formation of the SS All planets orbit in roughly the same plane about the Sun. All planets orbit in the
More informationThe Layout of the Solar System
The Layout of the Solar System Planets fall into two main categories Terrestrial (i.e. Earth-like) Jovian (i.e. Jupiter-like or gaseous) [~5000 kg/m 3 ] [~1300 kg/m 3 ] What is density? Average density
More informationSINP 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:
More informationHalliday, Resnick & Walker Chapter 13. Gravitation. Physics 1A PHYS1121 Professor Michael Burton
Halliday, Resnick & Walker Chapter 13 Gravitation Physics 1A PHYS1121 Professor Michael Burton II_A2: Planetary Orbits in the Solar System + Galaxy Interactions (You Tube) 21 seconds 13-1 Newton's Law
More information