The Physics of Solar Flares Examining Solar Flares and Radio Bursts By Caylin Mendelowitz and Claire Rosen.

Slides:



Advertisements
Similar presentations
MT4510 Solar Theory Thomas Neukirch
Advertisements

Chapter 11: Our Star © 2015 Pearson Education, Inc.
Copyright © 2012 Pearson Education, Inc. Chapter 10 Our Star 1.
Solar Theory (MT 4510) Clare E Parnell School of Mathematics and Statistics.
The magnetic nature of solar flares Paper by E.R. Priest & T.G. Forbes Review presented by Hui Song.
ACTIVITY ON THE SUN: Prominences Sunspots Solar Flares CME’s – Coronal Mass Ejections Solar Wind Space Weather.
R. P. Lin Physics Dept & Space Sciences Laboratory University of California, Berkeley The Solar System: A Laboratory for the Study of the Physics of Particle.
Chapter 8 The Sun – Our Star.
Chapter 16 Modeling the solar interior The vibrating sun Neutrinos Solar atmosphere: –Photosphere –Chromosphere –Corona Sunspots Solar magnetic fields.
General Properties Absolute visual magnitude M V = 4.83 Central temperature = 15 million 0 K X = 0.73, Y = 0.25, Z = 0.02 Initial abundances: Age: ~ 4.52.
1 Grades 3 - 5: Introduction. 2 Better Observation Of The Sun And Earth Importance of Space Technology.
Guiding Questions 1.What is the source of the Sun’s energy? 2.What is the internal structure of the Sun? 3.How can we measure the properties of the Sun’s.
Copyright © 2012 Pearson Education, Inc. Radius: 6.9  10 8 m (109 times Earth) Mass: 2  kg (300,000 Earths) Luminosity: 3.8  watts Our Star.
This Set of Slides This set of slides covers our Sun, nuclear processes, solar flares, auroras, and more… Units covered 49, 50, 51.
The Sun Astronomy 311 Professor Lee Carkner Lecture 23.
Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.
Physical Astronomy Professor Lee Carkner Lecture 11
F1B: Determine the Dominant Processes of Particle Acceleration Phase , Open the Frontier UV Spectroscopic determin- ation of pre/post-shock density,
Solar Activities and Space Weather Lecture 16. Guiding Questions 1.What are solar active regions? How do we know that sun spots are regions of strong.
The Sun and the Heliosphere: some basic concepts…
Our Sun. Why do we care about the Sun... - Light, heat, life - Space weather solar wind (1,000,000 mph) flares (UV, x-ray radiation) disturb Earth's magnetic.
The Sun The Sun is a star Huge ball of glowing ionized gas… plasma. Gravity vs. Nuclear Fusion Gravity wants to crush the star Fusion wants to explode.
Multiwavelength observations of a partially occulted solar flare Laura Bone, John C.Brown, Lyndsay Fletcher.
The Relation between Soft X-ray Ejections and Hard X-ray Emission on November 24 Flare H. Takasaki, T. Morimoto, A. Asai, J. Kiyohara, and K. Shibata Kwasan.
The Sun ROBOTS Summer Solar Structure Core - the center of the Sun where nuclear fusion releases a large amount of heat energy and converts hydrogen.
Solar Drivers of Space Weather Steven Hill NOAA/SEC June 14, 2007 Research Experience for Undergraduates.
Outstanding Issues Gordon Holman & The SPD Summer School Faculty and Students.
Inner Workings of the Sun (87). Sun is mostly hydrogen and helium gas (plasma). Core (15,000,000 ° C): –Fuels the sun, where the fusing of Hydrogen 
Simultaneous monitoring observations of solar active regions at millimeter wavelengths at radio telescopes RT-7.5 BMSTU (Russia) and RT-14 Metsahovi radio.
The Sun.
Advanced Solar Theory (MT5810) OUTLINE 1.Observational properties of the Sun 2.MHD equations (revision) 3.Induction equation - solutions when R m >1 4.Magnetic.
 Structure of the Sun  Starting at the center and working outward  The Core  The Radiative Zone  The Convective Zone  The Photosphere  The Chromosphere.
The Sun The Sun imaged in white light by the SOHO spacecraft.
© 2010 Pearson Education, Inc. Solar Thermostat Decline in core temperature causes fusion rate to drop, so core contracts and heats up. Rise in core temperature.
Chapter 9 Our Star, the Sun. What do you think? What is the surface of the Sun like? Does the Sun rotate? What makes the Sun shine?
II. MAGNETOHYDRODYNAMICS (Space Climate School, Lapland, March, 2009) Eric Priest (St Andrews)
Our Star, the Sun. The Sun is the Largest Object in the Solar System The Sun contains more than 99.85% of the total mass of the solar system If you.
Chapter 10 Our Star A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun’s structure?
Energy Budgets of Flare/CME Events John Raymond, J.-Y. Li, A. Ciaravella, G. Holman, J. Lin Jiong Qiu will discuss the Magnetic Field Fundamental, but.
Flare-Associated Oscillations Observed with NoRH Ayumi Asai (NSRO) Nobeyama Symposium 2004 : 2004/10/26.
Units to cover: 52, 53, Observatories in Space.
Sun, Moon, Earth, How do they work together to help life survive? our sun.
Show 1 -- photosphere & sunspots SUN COURSE - SLIDE SHOW 4 Show 2 -- corona & solar cycle Today: Sun today + waves + prominences +UFO’s Show 3 -- SOHO.
Reading Unit 31, 32, 51. The Sun The Sun is a huge ball of gas at the center of the solar system –1 million Earths would fit inside it! –Releases the.
Universe Tenth Edition Chapter 16 Our Star, the Sun Roger Freedman Robert Geller William Kaufmann III.
The Sun Part 2.
Our Star, the Sun. The Sun is the Largest Object in the Solar System The Sun contains more than 99.85% of the total mass of the solar system If you.
Sun phenomena. sunspots By tracking them, we realized the sun rotates Click here.
Our amazing sun. sunspots By tracking them, we realized the sun rotates Click here.
The Sun. Sun Fact Sheet The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. Diameter: 1,390,000 km (Earth 12,742 km or nearly.
© 2017 Pearson Education, Inc.
THE SUN The star we see by day.
CH29: The Sun Mrs. Kummer, 2016.
The Sun and Our Earth The Structure of Our Sun The Energy of Our Sun
Sun: General Properties
PROPERTIES OF THE SUN Essential Questions
Solar and Heliospheric Physics
Overview of the Sun Jie Zhang Art Poland
Section 2: Solar Activity
Properties of the Sun Visual Vocabulary.
Introduction to Space Weather
What is the sun? What is the structure of the sun?
The Sun and Our Earth The Structure of Our Sun The Energy of Our Sun
Chapter 9 The Sun.
SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS
WHAT DO YOU THINK? How does the mass of the Sun compare with that of the rest of the Solar System? Are there stars nearer the Earth than the Sun is? What.
The Sun.
Grades 3 - 5: Introduction
Grades 3 - 5: Introduction
CORONAL MASS EJECTIONS
Presentation transcript:

The Physics of Solar Flares Examining Solar Flares and Radio Bursts By Caylin Mendelowitz and Claire Rosen

OUTLINE Flares Bursts Solar Activity Energy Storage Energy Release Energy Requirements Flare Prediction Summary

Solar Interior Solar interior Gregory, p. 202

Solar Flares What are they? Radiation –optical (H  ) –radio Phases –activation –impulsive –late

Radio Bursts Different Types –type I : thermal –type II & IV: plasma oscillations (shock) & synchrotron –type III & V: plasma oscillations (electrons) & synchrotron Association with flare phases –type III & V coincide with impulsive phase –type II & IV follow impulsive phase –type I in late phase (storm phase)

Solar Activity 22 year cycle Signs of solar activity –flares, CME’s, filaments, sunspots Solar magnetic field –frozen field lines –differential rotation --> twisted magnetic field lines –convection --> kinks –buoyancy -->loops (connect sunspots) Gregory, p.221

Energy Storage Open field lines B|| (above) – B|| (below) =  0 K, where  0 is the permeability of free space and K is surface current density Figure 4 Gregory, p.220

Carroll, p. 424 Field Loop with Current Sheet

Energy Release Accelerated particles –excite plasma oscillations --> type III bursts –synchrotron radiation-- type IV and V bursts –heat plasma --> H  double ribbons X-ray or H  loop prominence loop expands as CME -shock excites plasma oscillations --> type II bursts Tandberg-Hanssen and Emslie, cover

Energy Requirements Typical field strength of active region B = 300 G. Flare energy is ergs Magnetic energy density is = B 2 /8  = 3580 ergs/cm 3 W = P  dV = PV. Solving for V we get V = W/P and –so the minimum volume needed to contain the energy is V = 2.79 * cm 3 Approximate to cube, so L = 3*10 9 cm Length of H  ribbon is cm -- Physical dimensions compare Reconnection time –  R = ½ (R m ) 1/4  A 1/2  D 1/2 = 3sec Time scale compares

Flare Prediction Coronal Mass Ejections (CME’s) Sigmoid regions Zeeman effect Magnetograph Dooling, p. 2

Summary Flares (general) - cause? –Origins --> magnetic energy storage –Mechanism --> reconnection Correlation between radio and optical emission –thermal emission --> H  ribbon (optical) –plasma oscillations and synchrotron --> radio waves Prediction