Solar eruptive phenomena
|
|
- Audrey Blair
- 5 years ago
- Views:
Transcription
1 Solar eruptive phenomena Andrei Zhukov Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium 26/01/2018 1
2 Eruptive solar activity Solar activity exerts continous influence on the solar system, including the Earth. The phenomena of solar activity take place on a variety of time scales, from milliseconds to thousands of years. This presentation focuses on eruptive solar phenomena, i.e. the abrupt variations of activity taking place on short time scales (several minutes to several days). 26/01/2018 2
3 Why can solar activity be harmful to us? It is because we live in the atmosphere of a variable magnetic star! 26/01/2018 3
4 total eclipse Solar corona and solar wind 26/01/2018 4
5 total eclipse photosphere imaged in the visible light Solar corona and solar wind 26/01/2018 5
6 total eclipse corona imaged in the extreme ultraviolet (EUV) Solar corona and solar wind 26/01/2018 6
7 space-borne coronagraph total eclipse corona imaged in the extreme ultraviolet (EUV) Solar corona and solar wind 26/01/2018 7
8 eclipse + coronagraph space-borne coronagraph total eclipse corona imaged in the extreme ultraviolet (EUV) Solar corona and solar wind 26/01/2018 8
9 eclipse + coronagraph space-borne coronagraph total eclipse corona imaged in the extreme ultraviolet (EUV) Solar corona and solar wind Solar corona is the outer layer of the atmosphere of the Sun. The corona is magnetized and is in permanent expansion. Its expansion speed (usually between 400 et 800 km/s) is above the sound speed of the ambient medium (around 150 km/s). 26/01/2018 9
10 Our trips to the Moon (and to Mars in future) Apollo 16: April 1972 Apollo 17: 7-19 December 1972 (BBSO) 4 August 1972: a solar super-flare! 26/01/
11 (ESA, NASA) A story of a solar eruption 26/01/
12 (ESA, NASA) Three solar phenomena that can be geoeffective on short time scales Solar flares Their electromagnetic emission perturbs the terrestrial ionosphere. Coronal mass ejections (CMEs) Their magnetic field drives geomagnetic storms (with auroras as their most spectacular manifestation). Solar energetic particles mostly protons and electrons can be generated by both flares and CMEs, produce radiation storms. 26/01/
13 (NASA) Phenomenology: a solar flare K K K K K K K K 26/01/
14 (NASA) Phenomenology: a solar flare K K K K A flare is a local (inside a sunspot group) and sudden (on a time scale of minutes) increase of solar electromagnetic emission observed in different spectral domains K K K K 26/01/
15 (ESA, NASA) A series of flares observed during a half of a solar rotation (14 days) 26/01/
16 Energy and power of a solar eruption Energy Min Typ. Max Flare (J) World s production of energie during 7 days 20 years years Total energy consumption in Belgium during 4 years years 4 million years Volcanic eruptions million H-bombs (20 MT) million Power Min Typ. Max Flare (W) Total world power million 500 million Solar power at Earth Most energetic phenomena close to the Earth! 26/01/
17 η Carinae (NASA) Phenomenology: coronal mass ejections (CMEs) A CME is an ejection of plasma observed by a coronagraph. The CME speed is generally between 200 km/s (slower than the solar wind) and 2500 km/s (significantly faster than the solar wind). Plasma ejections are also observed in other stars, although they may correspond to different physical mechanisms. 26/01/ (ESA, NASA)
18 (ESA, NASA) CMEs are transparent (like the corona itself). The apparent differences in their morphology are often due to the projection effect: from one vantage point, a CME can be observed with a limited angular extent, from another vantage point, the same CME can be observed as a halo. Halo CMEs may propagate towards the observer, for example towards the Earth. 26/01/
19 (ESA, NASA, A. Zhukov) CME signatures in EUV Coronal dimmings EIT waves Post-eruptive arcades Limb signatures: loop opening, plasmoid rise, etc. Eruptive prominences (eruptive filaments) 30/09/
20 CME signatures in EUV In this movie, one can see different CME signatures observed in extreme ultraviolet (EUV): eruption of a filament (prominence), i.e. of relatively cold ( K) material that appears dark, post-eruptive arcade (a consequence of magnetic reconnection, see below), coronal dimmings (places of plasma evacuations during the CME lift-off), loop opening (a consequence of a magnetic instability). (ESA, NASA) 30/09/
21 (ESA, NASA) Another solar eruption In this movie, one can see: a flare, different CME signatures in the extreme ultraviolet (EUV): a post-eruptive arcade (a consequence of magnetic reconnection, see below), coronal dimmings (places of plasma evacuation during the CME lift-off), a CME, a solar energetic particle event. 26/01/
22 (NASA; N. Nitta) (ESA, NASA) EIT waves EIT waves were discovered using the EIT instrument developed by an international consortium and manufactured at the Centre Spatial de Liège. 30/09/
23 Physics of CMEs: magnetic flux ropes In a magnetic flux rope, the magnetic field is twisted. A magnetic flux rope (preexisting or formed during the eruption) is an essential ingredient of CME models. 26/01/
24 Physics of CMEs: catastrophic restructuring of the coronal magnetic field 26/01/
25 Physics of CMEs: catastrophic restructuring of the coronal magnetic field And without equations?.. 26/01/
26 Physics of CMEs: catastrophic restructuring of the coronal magnetic field (B. Kliem et al.) Catastrophe theory can be applied to CMEs. A catastrophe of the magnetic field can occur in two different ways: an instability, a loss of equilibrium. Torus instability 26/01/
27 Instability Physics of CMEs: catastrophic restructuring of the coronal magnetic field Loss of equilibrium (B. Kliem et al.) Catastrophe theory can be applied to CMEs. A catastrophe of the magnetic field can occur in two different ways: an instability, a loss of equilibrium. Torus instability 26/01/
28 (UKAEA) (T. Török, B. Kliem) Physics of CMEs: catastrophic restructuring of the coronal magnetic field There exist numerous types of magnetic instabilities in plasma. Another instability observed in the solar atmosphere: kink instability. This instability is also seen in the fusion research that uses magnetic confinement. 30/09/
29 (E. Priest) CME initiation in the low corona and link with flares 26/01/
30 (E. Priest) (U. Anzer & G. Pneumann) CME initiation in the low corona and link with flares 26/01/
31 (E. Priest) (U. Anzer & G. Pneumann) CME initiation in the low corona and link with flares 26/01/
32 (E. Priest) (U. Anzer & G. Pneumann) CME initiation in the low corona and link with flares Magnetic field lines of force are elongated and stretched due to the development of an instability. This may induce their reconnection. 26/01/
33 Physics: magnetic reconnection The reconnection of magnetic field lines leads to the conversion of free magnetic energy into: kinetic energy of bulk plasma motions (CME!), thermal energy of plasma leading to the increased radiation (flare!), energy of accelerated particles (that get thermalized and produce another component of the flare radiation). 30/09/
34 (NASA; H. Q. Song et al.) Physics: magnetic reconnection 30/09/
35 (NASA; H. Q. Song et al.) Physics: magnetic reconnection 30/09/
36 Energetic particle acceleration by magnetic reconnection and X-ray flares X-rays in a solar flare and in an X-ray tube originate in the same physical process. 26/01/
37 CME propagation towards the Earth Sun Earth The effect of a CME on the terrestrial environment depends mostly on the orientation of the CME magnetic field. 26/01/
38 (ESA, NASA) Phenomenology: solar energetic particle event A solar eruption can accelerate particles in several ways. The flare reconnection acceletrates the particles towards low altitudes (these particles produce the X-ray emission). The flare reconnection (?) also accelerates particles towards high altitudes. The shock wave driven by the CME plays a crucial role in the particle acceleration. 26/01/
39 (ESA, NASA) (NASA) (NSF, NASA; Nikolić et al.) Shock waves 26/01/
40 (R. Schwenn) Origin of transient shock waves in the heliosphere 26/01/
41 (R. Schwenn) Origin of transient shock waves in the heliosphere The transient shock waves in the heliosphere (i.e. those associated with solar eruptions) are produced by CMEs. 26/01/
42 (R. Treumann & C. Jaroschek) Acceleration of particles by the shock waves The energy of particles increases due to multiple reflections atthe waves and small-scale structures in the turbulent medium present at both sides of the propagating shock wave. 26/01/
43 (NASA) (NSF, NASA; Nikolić et al.) The same process of energetic particle acceleration takes place in the CME-driven shock waves and in supernova shock waves Solar cosmic rays Galactic cosmic rays 26/01/
44 (V. Bothmer) Phenomenologie: un evenement des particules energetiques 26/01/
45 (ESA, NASA) Solar eruptions: a summary 26/01/
46 Physics of solar eruptions: the old and the modern paradigms Old paradigm 26/01/2018 (J. Gosling) 46
47 What was the danger for the astronautes? Apollo 16: April 1972 Apollo 17: 7-19 December 1972 (BBSO) The danger was very real: a very high flux of energetic protons, mainly produced by the shock wave driven by the CME associated with the super-flare on 4 August 1972! 4 August 1972: a solar super-flare! 26/01/
48 Thank you for your attention! 26/01/
49 Further reading J. T. Gosling The Solar Flare Myth. J. Geophys. Res. 98, A11, (1993) R. Schwenn Space Weather: The Solar Perspective. Living Rev. Solar Phys., 3, 2 (2006) 26/01/
50 Backup slides 26/01/
51 CME propagation towards the Earth: a model 26/01/
An Introduction to Space Weather. J. Burkepile High Altitude Observatory / NCAR
An Introduction to Space Weather J. Burkepile High Altitude Observatory / NCAR What is Space Weather? Space Weather refers to conditions in interplanetary space, produced by the Sun, that can disrupt
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 informationModelling the Initiation of Solar Eruptions. Tibor Török. LESIA, Paris Observatory, France
Modelling the Initiation of Solar Eruptions Tibor Török LESIA, Paris Observatory, France What I will not talk about: global CME models Roussev et al., 2004 Manchester et al., 2004 Tóth et al., 2007 numerical
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 weather and solar-terrestrial relations
Space weather and solar-terrestrial relations 1 Hardi Peter Kiepenheuer-Institut für Sonnenphysik Freiburg solar eclipse, 11.8.1999, Wendy Carlos and John Kern with special thanks to Bernhard Kliem, AIP,
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 informationChapter 8 The Sun Our Star
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 8 The Sun
More information1-4-1A. Sun Structure
Sun Structure A cross section of the Sun reveals its various layers. The Core is the hottest part of the internal sun and is the location of nuclear fusion. The heat and energy produced in the core is
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 informationAstronomy Chapter 12 Review
Astronomy Chapter 12 Review Approximately how massive is the Sun as compared to the Earth? A. 100 times B. 300 times C. 3000 times D. 300,000 times E. One million times Approximately how massive is the
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 information1.3j describe how astronomers observe the Sun at different wavelengths
1.3j describe how astronomers observe the Sun at different wavelengths 1.3k demonstrate an understanding of the appearance of the Sun at different wavelengths of the electromagnetic spectrum, including
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 informationEFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER
Indian J.Sci.Res.3(2) : 121-125, 2012 EFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER a1 b c SHAM SINGH, DIVYA SHRIVASTAVA AND A.P. MISHRA Department of Physics, A.P.S.University, Rewa,M.P.,
More informationExploring the Solar Wind with Ultraviolet Light
Timbuktu Academy Seminar, Southern University and A&M College, November 19, 2003 Exploring the Solar Wind with Ultraviolet Light Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics, Cambridge,
More informationASPIICS: a Giant Solar Coronagraph onboard the PROBA-3 Mission
SOLI INVICTO ASPIICS: a Giant Solar Coronagraph onboard the PROBA-3 Mission Andrei Zhukov Principal Investigator of PROBA-3/ASPIICS Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium
More informationThe Sun Our Star. Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun
The Sun Our Star Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun General Properties Not a large star, but larger than most Spectral type G2 It
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 information1 A= one Angstrom = 1 10 cm
Our Star : The Sun )Chapter 10) The sun is hot fireball of gas. We observe its outer surface called the photosphere: We determine the temperature of the photosphere by measuring its spectrum: The peak
More informationThe General Properties of the Sun
Notes: The General Properties of the Sun The sun is an average star with average brightness. It only looks bright because it s so close. It contains 99% of the mass of the solar system. It is made of entirely
More information19:00-20:30 Welcome Reception at the Wäinö Aaltonen Museum of Art. 09:40-10:10 An Historical Perspective on Coronal Mass Ejections: 5$
6RODU(QHUJHWLF3ODVPDVDQG3DUWLFOHV 6FLHQWLILF3URJUDP 6XQGD\$XJXVW 19:00-20:30 Welcome Reception at the Wäinö Aaltonen Museum of Art 0RQGD\$XJXVW 09:00-09:10 Welcome: 3URIHVVRU.HLMR9LUWDQHQ, Rector of 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 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 informationSolar Dynamics Affecting Skywave Communications
Solar Dynamics Affecting Skywave Communications Ken Larson KJ6RZ October 2010 1 Page Subject 3 1.0 Introduction 3 2.0 Structure of the Sun 3 2.1 Core 3 2.2 Radiation Zone 4 2.3 Convection Zone 4 2.4 Photosphere
More informationLiving in a Star. Sarah Gibson (NCAR/HAO)
Living in a Star Sarah Gibson (NCAR/HAO) 3D real-time astronomy Solar eruption (CME) Earth s magnetosphere We are observing a stellar system from within What we see may impact us in near-real time Unescapably
More informationGuidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.
Guidepost The Sun is the source of light an warmth in our solar system, so it is a natural object to human curiosity. It is also the star most easily visible from Earth, and therefore the most studied.
More informationOutline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.
Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned. Next homework due Oct 24 th. I will not be here on Wednesday, but Paul Ricker will present the lecture! My Tuesday
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 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 informationSTCE Newsletter. 7 Dec Dec 2015
Published by the STCE - this issue : 18 Dec 2015. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
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 informationEvolution of Twisted Magnetic Flux Ropes Emerging into the Corona
Evolution of Twisted Magnetic Flux Ropes Emerging into the Corona Yuhong Fan High Altitude Observatory, National Center for Atmospheric Research Collaborators: Sarah Gibson (HAO/NCAR) Ward Manchester (Univ.
More informationLearning Objectives. wavelengths of light do we use to see each of them? mass ejections? Which are the most violent?
Our Beacon: The Sun Learning Objectives! What are the outer layers of the Sun, in order? What wavelengths of light do we use to see each of them?! Why does limb darkening tell us the inner Sun is hotter?!
More informationChapter 14 Lecture. The Cosmic Perspective Seventh Edition. Our Star Pearson Education, Inc.
Chapter 14 Lecture The Cosmic Perspective Seventh Edition Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is
More informationIn-Situ Signatures of Interplanetary Coronal Mass Ejections
In-Situ Signatures of Interplanetary Coronal Mass Ejections Ian G. Richardson, NASA/Goddard Space Flight Center and CRESST/Department of Astronomy, University of Maryland, College Park ~Two dozen in-situ
More information8.2 The Sun pg Stars emit electromagnetic radiation, which travels at the speed of light.
8.2 The Sun pg. 309 Key Concepts: 1. Careful observation of the night sky can offer clues about the motion of celestial objects. 2. Celestial objects in the Solar System have unique properties. 3. Some
More informationRadio Observations and Space Weather Research
Radio Observations and Space Weather Research Jasmina Magdalenić Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium What is space weather and why is it important? Eruptive processes:
More informationSpace Weather Effects of Coronal Mass Ejection
J. Astrophys. Astr. (2006) 27, 219 226 Space Weather Effects of Coronal Mass Ejection K. N. Iyer 1,, R. M. Jadav 1, A. K. Jadeja 1, P. K. Manoharan 2, Som Sharma 3 and Hari Om Vats 3 1 Department of Physics,
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 1 11 Jun 07 UA/NSO Summer School 1 If the sun didn't have a magnetic field, then it would be as boring a star as most astronomers think it is. -- Robert Leighton 11 Jun 07 UA/NSO
More informationThe Structure of the Sun. CESAR s Booklet
How stars work In order to have a stable star, the energy it emits must be the same as it can produce. There must be an equilibrium. The main source of energy of a star it is nuclear fusion, especially
More informationLogistics 2/14/17. Topics for Today and Thur. Helioseismology: Millions of sound waves available to probe solar interior. ASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Pleiades Star Cluster Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 9 Tues 14 Feb 2017 zeus.colorado.edu/astr1040-toomre Topics for Today and Thur Helioseismology:
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 informationThe importance of ground-based observations of the solar corona
The importance of ground-based observations of the solar corona J. Burkepile 1, S. Tomczyk 1, P. Nelson 1, A.G. dewijn 1, S. Sewell 1, D. Elmore 2, L. Sutherland 1, R. Summers 1, D. Kolinski 1, L. Sitongia
More informationOur sole source of light and heat in the solar system. A very common star: a glowing g ball of gas held together by its own gravity and powered
The Sun Visible Image of the Sun Our sole source of light and heat in the solar system A very common star: a glowing g ball of gas held together by its own gravity and powered by nuclear fusion at its
More informationThe Sun. Never look directly at the Sun, especially NOT through an unfiltered telescope!!
The Sun Introduction We will meet in class for a brief discussion and review of background material. We will then go outside for approximately 1 hour of telescope observing. The telescopes will already
More informationSTCE Newsletter. 28 Dec Jan 2016
Published by the STCE - this issue : 8 Jan 2016. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationWhy study plasma astrophysics?
Why study plasma astrophysics? Nick Murphy and Xuening Bai Harvard-Smithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics January 25, 2016 Today s plan Definition of a plasma Plasma astrophysics:
More informationSun s Properties. Overview: The Sun. Composition of the Sun. Sun s Properties. The outer layers. Photosphere: Surface. Nearest.
Overview: The Sun Properties of the Sun Sun s outer layers Photosphere Chromosphere Corona Solar Activity Sunspots & the sunspot cycle Flares, prominences, CMEs, aurora Sun s Interior The Sun as an energy
More informationRadiation Zone. AST 100 General Astronomy: Stars & Galaxies. 5. What s inside the Sun? From the Center Outwards. Meanderings of outbound photons
AST 100 General Astronomy: Stars & Galaxies 5. What s inside the Sun? From the Center Outwards Core: Hydrogen ANNOUNCEMENTS Midterm I on Tue, Sept. 29 it will cover class material up to today (included)
More informationThe Sun s Dynamic Atmosphere
Lecture 16 The Sun s Dynamic Atmosphere Jiong Qiu, MSU Physics Department Guiding Questions 1. What is the temperature and density structure of the Sun s atmosphere? Does the atmosphere cool off farther
More informationLogistics 2/13/18. Topics for Today and Thur+ Helioseismology: Millions of sound waves available to probe solar interior. ASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Pleiades Star Cluster Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 9 Tues 13 Feb 2018 zeus.colorado.edu/astr1040-toomre Topics for Today and Thur+ Helioseismology:
More informationThe kink instability of a coronal magnetic loop as a trigger mechanism for solar eruptions
The kink instability of a coronal magnetic loop as a trigger mechanism for solar eruptions T. Török 1 and B. Kliem 2 1 School of Mathematics and Statistics, University of St. Andrews St. Andrews, Fife
More informationMulti-wavelength VLA and Spacecraft Observations of Evolving Coronal Structures Outside Flares
Multi-Wavelength Investigations of Solar Activity Proceedings of IAU Symposium No. 223, 2004 A.V. Stepanov, E.E. Benevolenskaya & A.G. Kosovichev, eds. Multi-wavelength VLA and Spacecraft Observations
More informationTurbulent Origins of the Sun s Hot Corona and the Solar Wind
Turbulent Origins of the Sun s Hot Corona and the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics Turbulent Origins of the Sun s Hot Corona and the Solar Wind Outline: 1. Solar
More informationThe Sun. the main show in the solar system. 99.8% of the mass % of the energy. Homework due next time - will count best 5 of 6
The Sun the main show in the solar system 99.8% of the mass 99.9999...% of the energy 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Homework due next time - will count best 5 of 6 The
More informationOur sun is the star in our solar system, which lies within a galaxy (Milky Way) within the universe. A star is a large glowing ball of gas that
Our sun is the star in our solar system, which lies within a galaxy (Milky Way) within the universe. A star is a large glowing ball of gas that generates energy through nuclear fusion in its core. The
More informationThe Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:
The Sun Basic Properties Radius: Mass: 5 R Sun = 6.96 km 9 R M Sun 5 30 = 1.99 kg 3.33 M ρ Sun = 1.41g cm 3 Luminosity: L Sun = 3.86 26 W Effective Temperature: L Sun 2 4 = 4πRSunσTe Te 5770 K The Sun
More informationChapter 14 Lecture. Chapter 14: Our Star Pearson Education, Inc.
Chapter 14 Lecture Chapter 14: Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on FIRE?
More informationHelios in Greek and Sol in Roman
Helios in Greek and Sol in Roman Drove his chariot across the sky to provide daylight Returned each night in a huge golden cup on the river Oceanus His son Phaeton drove the chariot one day but lost control
More informationThe Sun. The Sun Is Just a Normal Star 11/5/2018. Phys1411 Introductory Astronomy. Topics. Star Party
Foundations of Astronomy 13e Seeds Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 8 The Sun Star Party This Friday November 9 weather permitting. See the flyer for updates in case of cancellations
More informationChapter 14 Our Star Pearson Education, Inc.
Chapter 14 Our Star Basic Types of Energy Kinetic (motion) Radiative (light) Potential (stored) Energy can change type, but cannot be created or destroyed. Thermal Energy: the collective kinetic energy
More informationChapter 14 Our Star A Closer Look at the Sun. Why was the Sun s energy source a major mystery?
Chapter 14 Our Star 14.1 A Closer Look at the Sun Our goals for learning Why was the Sun s energy source a major mystery? Why does the Sun shine? What is the Sun s structure? Why was the Sun s energy source
More informationCorrection to Homework
Today: Chapter 10 Reading Next Week: Homework Due March 12 Midterm Exam: March 19 Correction to Homework #1: Diameter of eye: 2.5 cm #10: See Ch. 11 Office Hours Monday. 11AM -2 PM Help Sessions Available:
More informationThere are two more types of solar wind! The ballerina Sun right before activity minimum. The ballerina dancing through the solar cycle
There are two more types of solar wind! 3. Low speed wind of "maximum" type Similar characteristics as (2), except for Lectures at the International Max-Planck-Research School Oktober 2002 by Rainer Schwenn,
More informationInitiation and Energy Release of Solar Coronal Mass Ejections (CMEs) & Relevant Solar Radio Bursts Yao Chen Institute of Space Sciences, Shandong
Initiation and Energy Release of Solar Coronal Mass Ejections (CMEs) & Relevant Solar Radio Bursts Yao Chen Institute of Space Sciences, Shandong University Initiation and Energy Release of CMEs Outline
More informationThe Interior Structure of the Sun
The Interior Structure of the Sun Data for one of many model calculations of the Sun center Temperature 1.57 10 7 K Pressure 2.34 10 16 N m -2 Density 1.53 10 5 kg m -3 Hydrogen 0.3397 Helium 0.6405 The
More informationToward Interplanetary Space Weather: Strategies for Manned Missions to Mars
centre for fusion, space and astrophysics Toward Interplanetary Space Weather: Strategies for Manned Missions to Mars Presented by: On behalf of: Jennifer Harris Claire Foullon, E. Verwichte, V. Nakariakov
More informationCESAR BOOKLET General Understanding of the Sun: Magnetic field, Structure and Sunspot cycle
CESAR BOOKLET General Understanding of the Sun: Magnetic field, Structure and Sunspot cycle 1 Table of contents Introduction to planetary magnetospheres and the interplanetary medium... 3 A short introduction
More informationModule 4: Astronomy - The Solar System Topic 2 Content: Solar Activity Presentation Notes
The Sun, the largest body in the Solar System, is a giant ball of gas held together by gravity. The Sun is constantly undergoing the nuclear process of fusion and creating a tremendous amount of light
More information1. Solar Atmosphere Surface Features and Magnetic Fields
1. Solar Atmosphere Surface Features and Magnetic Fields Sunspots, Granulation, Filaments and Prominences, Coronal Loops 2. Solar Cycle: Observations The Sun: applying black-body radiation laws Radius
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 informationSolar Flare Variations
Solar Flare Variations Advisors: Phillip Chamberlin, Rachel Hock and Tom Woods NSF By Chris Moore Outline Overview of solar activity Relevance Proxies Halloween flares Procedures Analysis Conclusion Goals
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 informationExplosive Solar Phenomena. Nat Gopalswamy NASA/GSFC
Explosive Solar Phenomena Nat Gopalswamy NASA/GSFC Africa Space Science School Kigali Rwanda July 1 2014 What are explosive phenomena? These phenomena represent sudden release of energy on the sun, confined
More informationPrentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 24 Studying the Sun 24.1 The Study of Light Electromagnetic Radiation Electromagnetic radiation includes gamma rays, X-rays, ultraviolet light, visible
More informationThe Solar Wind Space physics 7,5hp
The Solar Wind Space physics 7,5hp Teknisk fysik '07 1 Contents History... 3 Introduction... 3 Two types of solar winds... 4 Effects of the solar wind... 5 Magnetospheres... 5 Atmospheres... 6 Solar storms...
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 informationSolar Flares and CMEs. Solar Physics 1
Solar Flares and CMEs Solar Physics 1 What is a solar flare? What is a CME? A solar flare is a sudden eruption of energetic charged particles from the Sun s corona. A coronal mass ejection (CME) is, by
More information10:10-10 :35 P.K.Manoharan National Centre for Radio Astrophysics
23 rd November, 2011 10:10-10 :35 P.K.Manoharan National Centre for Radio Astrophysics Radio observations, combined with the groundbased optical observations and spacebased data can provide a crossreferenced
More informationA STATISTICAL STUDY ON CORONAL MASS EJECTION AND MAGNETIC CLOUD AND THEIR GEOEFFECTIVENESS
A STATISTICAL STUDY ON CORONAL MASS EJECTION AND MAGNETIC CLOUD AND THEIR GEOEFFECTIVENESS Rajiv Kumar 1 Government Pench Valley PG college Parasia Distt.CHHINDWARA M.P., INDIA E-mail: captainrajiv@live.com
More informationAstronomy Ch 16 The Sun. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch 16 The Sun MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) The light we see from the Sun comes from which layer?
More informationAcceleration of the Solar Wind
From Sun to Mud: Solar and Space Physics for the UG Classroom Acceleration of the Andrew Jordan All images from SOHO spacecraft This presentation helps introductory physics students apply their skills
More informationIntroductory Lecture II: An Overview of Space Storms
Introductory Lecture II: An Overview of Space Storms Jan J. Sojka Center for Atmospheric and Space Science Utah State University Logan, Utah 28 July 2010 Overview Space weather and its storms. Super storms
More informationarxiv: v1 [astro-ph.sr] 2 Sep 2013
arxiv:1309.0417v1 [astro-ph.sr] 2 Sep 2013 ISSN 1845 8319 SIMULTANEOUS YOHKOH /SXT AND TRACE OBSERVATIONS OF SOLAR PLASMA EJECTIONS E. CHMIELEWSKA 1, M. TOMCZAK 1, T. MROZEK 1,2 1 Astronomical Institute,
More informationSolar Observation Class Project
Name: School: Grade or Level: Lesson Plan #: Date: Object Solar Observation Class Project The object of this classroom exercise to involve as individuals or as teams, students in the actual astronomical
More informationLecture 17 The Sun October 31, 2018
Lecture 17 The Sun October 31, 2018 1 2 Exam 2 Information Bring a #2 pencil! Bring a calculator. No cell phones or tablets allowed! Contents: Free response problems (2 questions, 10 points) True/False
More informationChapter 10 Our Star. X-ray. visible
Chapter 10 Our Star X-ray visible Radius: 6.9 10 8 m (109 times Earth) Mass: 2 10 30 kg (300,000 Earths) Luminosity: 3.8 10 26 watts (more than our entire world uses in 1 year!) Why does the Sun shine?
More informationPhys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 8
Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 8 MULTIPLE CHOICE 1. Granulation is caused by a. sunspots. * b. rising gas below the photosphere. c. shock waves in the corona. d. the
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 informationAstronomy 150: Killer Skies. Lecture 18, March 1
Assignments: Astronomy 150: Killer Skies HW6 due next Friday at start of class HW5 and Computer Lab 1 due Night Observing continues next week Lecture 18, March 1 Computer Lab 1 due next Friday Guest Lecturer:
More informationA Closer Look at the Sun
Our Star A Closer Look at the Sun Our goals for learning Why was the Sun s energy source a major mystery? Why does the Sun shine? What is the Sun s structure? Why was the Sun s energy source a major mystery?
More informationAn x-ray image of teeth. Can you see the filling?
X-Rays APA National Aeronautics and Space Administration, Science Mission Directorate. (2010). X-Rays. Retrieved December 12, 2012, from Mission:Science website: http://missionscience.nasa.gov /ems/11_xrays.html
More information10/18/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline
10/18/17 Lecture Outline 11.1 A Closer Look at the Sun Chapter 11: Our Star Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on
More informationSolar Transients P.K. Manoharan
Solar Transients P.K. Manoharan Radio Astronomy Centre National Centre for Radio Astrophysics Tata Institute of Fundamental Research Ooty 643001, India 1 Solar Flares and associated Coronal Mass Ejections
More informationAnnouncements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11
Announcements - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Review for Test #2 Oct 11 Topics: The Solar System and its Formation The Earth and our Moon
More informationProgress of MHD Simulations for the Interplanetary Propagation of Coronal Mass Ejections
Progress of MHD Simulations for the Interplanetary Propagation of Coronal Mass Ejections C. Verbeke, J. Pomoell, S. Poedts ISEST workshop, Jeju, 19.09.2017 Overview Introduction Constraining CME model
More informationWeight of upper layers compresses lower layers
Weight of upper layers compresses lower layers Gravitational equilibrium: Energy provided by fusion maintains the pressure Gravitational contraction: Provided energy that heated core as Sun was forming
More information4 Layers of the Sun. CORE : center, where fusion occurs
4 Layers of the Sun CORE : center, where fusion occurs RADIATION LAYER: energy transfer by radiation (like energy coming from a light bulb or heat lamp which you can feel across the room) CONVECTION LAYER:
More informationAsymmetric Magnetic Reconnection in Coronal Mass Ejection Current Sheets
Asymmetric Magnetic Reconnection in Coronal Mass Ejection Current Sheets Nicholas Murphy, 1 Mari Paz Miralles, 1 Crystal Pope, 1,2 John Raymond, 1 Kathy Reeves, 1 Dan Seaton, 3 & David Webb 4 1 Harvard-Smithsonian
More informationProton-proton cycle 3 steps PHYS 162 1
Proton-proton cycle 3 steps PHYS 162 1 4 Layers of the Sun CORE : center, where fusion occurs RADIATION: energy transfer by radiation CONVECTION: energy transfer by convection PHOTOSPHERE: what we see
More information