From coronal mass ejections to mouse keratinocytes

Size: px
Start display at page:

Download "From coronal mass ejections to mouse keratinocytes"

Transcription

1 From coronal mass ejections to mouse keratinocytes By Robin Thompson Supervised by Dr Ruth Baker and Christian Yates, Centre for Mathematical Biology (University of Oxford)

2 Where it all began... Find a technique to detect and track coronal mass ejections (CMEs) from the sun to Earth.

3 What is a CME? An eruption of plasma and magnetic field from the sun, travelling roughly radially outwards. Typical mass 1012 kg, typical speed km/s. Leading Edge Cavity Filament

4

5 WHY BOTHER? Upon impact with Earth, interplanetary coronal mass ejections (ICMEs) can be responsible for severe space weather effects, e.g. Aurora enhancement Disruption of telecommunications facilities, power grids and spacecraft The development of more sensitive electronics means we now need greater understanding of CMEs, including predicting both their arrival and the consequences of their impact with Earth.

6 October 2003 Image CME in yellow circle. The darkened areas at centre and to the left are where SMEI does not take data because the Sun and Moon are in this area. The grid overlay indicates 60-degree increments in the fi eld of view. When the CME extends to the third ring degrees - it has reached the plane of the Earth. The far left and right points correspond with the anti-sun direction into deep space.

7 If we look at lots of these images over time, we can see CMEs move. We can subtract any constant/slow-moving known sources of light (e.g. stars/planets) from our images. LET'S PLAY... Spot the CME

8

9 Raw SMEI image, May 2003 CME

10 Automatic Detection

11 The Tappin-Howard model

12 Our result We now have a completely automatic program that will warn us whenever a C M E is likely to hit the E arth, up to 12 hours in advance.

13 Cell adhesion Cells binding together with differing adhesiveness, due to different amounts of protein being present. During the development of the body's structure and organs, cells migrate to their target sites. Cellto-cell adhesion then enables them to aggregate and form cohesive tissues.

14 Further examples... Mouse keratinocytes grown under conditions that limit cell-to-cell adhesion. Keratinocyte skin cells adhere to form a protective layer against UV rays. Cancerous tumour invasion. Wound repair. Tissue engineering.

15 WHY BOTHER MODELLING? Puts cell migration and adhesion into framework where current hypotheses can be tested and refined, and experimentally verifiable predictions can be made. The differential adhesion hypothesis in action...

16 Types of model Cell-based (stochastic). Includes randomness often prevalent in biological systems. Population-based (deterministic). Less computational work, use tools from PDE analysis.

17 Within these two categories there are various sub-types. Cell-based models include: Lattice based. Velocity jump (run and tumble).

18 Our stochastic model Cell-based. Cells move on a fixed, one-dimensional lattice [0,1]. Cells jump to midpoint of neighbouring compartments only, with a cell in compartment i having probabilities Ti+ and Tiof moving up to i+1 and down to i-1 respectively. No flux boundary conditions. Adhesion (alpha is adhesion coefficient) and volume filling (carrying capacity S).

19 Stochastic simulation

20 The stochastic mean equations Derive a set of mean equations (k ODEs) that approximate the average behaviour of the stochastic system.

21 The continuum limit Taking the continuum limit in space (letting compartment size h tend to 0) leads to the following partial differential equation for the average behaviour of the stochastic system (can then use PDE analysis/only 1 equation):

22 Alpha < 0.75 We approximate the solution of the PDE system numerically. For small alpha, the deterministic system mimics the stochastic system well.

23 Alpha > 0.75 (diffusivity D(rho) can become negative) Certain density values leads to nonsensical (unphysical) solutions. PDE ill posed.

24 Solution of mean equations Instead use finite difference methods to numerically approximate solutions of the mean equations themselves. Solutions mimic the stochastics even for large alpha.

25 Varying the number of compartments and ICs Different types of patterning (metastable steady states). Highly dependent on ICs. All mimicked by mean equations.

26 Differences between stochastic and deterministic systems Can find ICs such that, for high alpha, the mean equations and stochastic system produce different solutions (although the average stochastic behaviour is still that of the mean equations). Can see none/one/two peaks. For these ICs, PDE behaviour sensitive to perturbations (random perturbations given by stochastic system).

27 The story so far... Can simulate our cell adhesion model. Have deterministic systems that mimic the average behaviour of the stochastics both in the small alpha and large alpha regimes. For certain ICs in high alpha regime, individual stochastic simulations produce different behaviour to deterministic systems. What next...?

28 Implementation on a growing domain The traditional compartment splitting method allow a randomly chosen 'compartment split' event instead of a cell movement. Old parent compartment replaced by two daughter compartments of the same size, with cells redistributed binomially. Many problems including that which compartment splits hugely affects the behaviour of the system, so little point looking at deterministic systems (average behaviour of the stochastic system).

29 New method for implementing domain growth Compartments grow by a small amount at a time (1 cell size). When double the original size, the compartment splits into two compartments (to stop cell jumps becoming unphysical), and the cells are redistributed. No sudden large change in cell density at any point on the domain.

30 3 Scenarios (exponentially growing domain) Small growth rate still see patterning. Large growth rate patterning destroyed. Medium growth rate patterning still evident but eventually destroyed.

31 Implementation of my method Can derive stochastic mean equations and PDE with domain growth incorporated. PDE still ill posed in the high alpha regime. Difficulty in how to implement mean equations over long timescales.

32 Future work Extend model to 2 species (simulate differential adhesion hypothesis?) Extend model to 2 spatial dimensions. Explore possibility of implementing velocity jump models on growing domain.

33 Thanks... Dr Ruth Baker (Centre for Mathematical Biology, University of Oxford). Christian Yates (Centre for Mathematical Biology, University of Oxford). Professor Endre Suli (Worcester College, University of Oxford). Centre for Mathematical Biology, University of Oxford. The Nuffield Foundation. The Oxford University SIAM Student Chapter.

The Automatic Detection and Tracking of Interplanetary Coronal Mass Ejections (ICMEs) By Robin Thompson Supervised by Dr Tim Howard, SwRI

The Automatic Detection and Tracking of Interplanetary Coronal Mass Ejections (ICMEs) By Robin Thompson Supervised by Dr Tim Howard, SwRI The Automatic Detection and Tracking of Interplanetary Coronal Mass Ejections (ICMEs) By Robin Thompson Supervised by Dr Tim Howard, SwRI What is a CME? An eruption of plasma and magnetic field from the

More information

Going from microscopic to macroscopic on non-uniform growing domains

Going from microscopic to macroscopic on non-uniform growing domains Going from microscopic to macroscopic on non-uniform growing domains Christian A. Yates, 1, Ruth E. Baker, 2, Radek Erban, 3, and Philip K. Maini 4, 1 Centre for Mathematical Biology, Mathematical Institute,

More information

EUHFORIA: Modeling the dangers of the sun.

EUHFORIA: Modeling the dangers of the sun. EUHFORIA: Modeling the dangers of the sun. 1 Introduction When we look at the Sun in visible light, it looks rather boring. However, when we observe the Sun at other wavelengths, it gets very interesting!

More information

Solar Activity Space Debris

Solar 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 information

The Sun. Never look directly at the Sun, especially NOT through an unfiltered telescope!!

The 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 information

Solar Activity The Solar Wind

Solar 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 information

Guidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.

Guidepost. 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 information

Even if not soon to. humans will still be in Space (ISS)

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 information

THE SOLAR WIND & SOLAR VARIABILITY

THE 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 information

Our Sun. The centre of our solar system

Our Sun. The centre of our solar system Our Sun The centre of our solar system Nicolaus Copernicus Our Sun The sun represents 99.86% of the mass in our solar system. It is ¾ hydrogen and ¼ helium. More than 1 million Earths can fit inside the

More information

The Sun as Our Star. Properties of the Sun. Solar Composition. Last class we talked about how the Sun compares to other stars in the sky

The Sun as Our Star. Properties of the Sun. Solar Composition. Last class we talked about how the Sun compares to other stars in the sky The Sun as Our Star Last class we talked about how the Sun compares to other stars in the sky Today's lecture will concentrate on the different layers of the Sun's interior and its atmosphere We will also

More information

A new mechanism to account for acceleration of the solar wind

A new mechanism to account for acceleration of the solar wind A new mechanism to account for acceleration of the solar wind Henry D. May Email: hankmay@earthlink.net Abstract An enormous amount of effort has been expended over the past sixty years in attempts to

More information

Lesson 3 THE SOLAR SYSTEM

Lesson 3 THE SOLAR SYSTEM Lesson 3 THE SOLAR SYSTEM THE NATURE OF THE SUN At the center of our solar system is the Sun which is a typical medium sized star. Composed mainly of Hydrogen (73% by mass), 23% helium and the rest is

More information

Chapter 8 The Sun Our Star

Chapter 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 information

An Introduction to Space Weather. J. Burkepile High Altitude Observatory / NCAR

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 information

Outline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.

Outline. 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 information

Geomagnetic storms. Measurement and forecasting

Geomagnetic 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 information

On 1 September 1859, a small white light flare erupted on the Solar surface

On 1 September 1859, a small white light flare erupted on the Solar surface The Sun Our Star On 1 September 1859, a small white light flare erupted on the Solar surface 17 hours later Magnetometers recorded a large disturbance Aurorae were seen in the Carribean, Telegraphs went

More information

A Closer Look at the Sun

A 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 information

Solar Flares and CMEs. Solar Physics 1

Solar 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 information

An Automatic Segmentation Algorithm for Solar Filaments in H-Alpha Images using a Context-based Sliding Window

An Automatic Segmentation Algorithm for Solar Filaments in H-Alpha Images using a Context-based Sliding Window An Automatic Segmentation Algorithm for Solar Filaments in H-Alpha Images using a Context-based Sliding Window Ibrahim A. Atoum College of Applied Sciences Al Maarefa Colleges for Science and Technology

More information

Lec 7: Classification of Stars, the Sun. What prevents stars from collapsing under the weight of their own gravity? Text

Lec 7: Classification of Stars, the Sun. What prevents stars from collapsing under the weight of their own gravity? Text 1 Astr 102 Lec 7: Classification of Stars, the Sun What prevents stars from collapsing under the weight of their own gravity? Text Why is the center of the Sun hot? What is the source of the Sun s energy?

More information

The Structure of the Sun. CESAR s Booklet

The 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 information

Student Instruction Sheet: Unit 4 Lesson 3. Sun

Student Instruction Sheet: Unit 4 Lesson 3. Sun Student Instruction Sheet: Unit 4 Lesson 3 Suggested time: 1.25 Hours What s important in this lesson: Sun demonstrate an understanding of the structure, and nature of our solar system investigate the

More information

The Dancing Lights Program

The Dancing Lights Program The Sun Teacher Background: The Dancing Lights Program Margaux Krahe Many people think the Sun is just a fiery yellow ball. The Sun is not actually burning because fire requires oxygen. Really, the Sun

More information

The Sun. 1a. The Photosphere. A. The Solar Atmosphere. 1b. Limb Darkening. A. Solar Atmosphere. B. Phenomena (Sunspots) C.

The Sun. 1a. The Photosphere. A. The Solar Atmosphere. 1b. Limb Darkening. A. Solar Atmosphere. B. Phenomena (Sunspots) C. The Sun 1 The Sun A. Solar Atmosphere 2 B. Phenomena (Sunspots) Dr. Bill Pezzaglia C. Interior Updated 2014Feb08 A. The Solar Atmosphere 1. Photosphere 2. Chromosphere 3. Corona 4. Solar Wind & earthly

More information

Connecting Magnetic Clouds to Solar Surface Features

Connecting Magnetic Clouds to Solar Surface Features Connecting Magnetic Clouds to Solar Surface Features Vasyl Yurchyshyn Coronal mass ejecta (CMEs) are known to cause strongest geomagnetic storms Most of the strongest storms are associated with arrival

More information

Space Weather and Satellite System Interaction

Space 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 information

Chapter 14 Our Star Pearson Education, Inc.

Chapter 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 information

Response 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 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 information

The Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:

The 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 information

Tracking Sunspots. Overview: Objectives: Lesson Preparation: Procedure: Details. Materials. Standards

Tracking Sunspots. Overview: Objectives: Lesson Preparation: Procedure: Details. Materials. Standards Tracking Sunspots Overview: Students will examine sunspots and track them at different latitudes on the Sun. This activity is adapted from the Tracking Sunspots activity on NASA s Solar and Heliocentric

More information

College Physics B - PHY2054C

College 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 information

Geomagnetic Disturbance Report Reeve Observatory

Geomagnetic 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 information

INCREASED LEVEL OF UV AND X-RAY RADIATION

INCREASED 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 information

Solar Magnetic Fields Jun 07 UA/NSO Summer School 1

Solar 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 information

Stars and Galaxies. Content Outline for Teaching

Stars and Galaxies. Content Outline for Teaching Section 1 Stars A. Patterns of stars - constellations 1. Ancient cultures used mythology or everyday items to name constellations 2. Modern astronomy studies 88 constellations 3. Some constellations are

More information

Modelling the Initiation of Solar Eruptions. Tibor Török. LESIA, Paris Observatory, France

Modelling 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 information

Chapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He

Chapter 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 information

Ooty Radio Telescope Space Weather

Ooty Radio Telescope Space Weather Ooty Radio Telescope Space Weather P.K. Manoharan Radio Astronomy Centre National Centre for Radio Astrophysics Tata Institute of Fundamental Research Ooty 643001, India mano@ncra.tifr.res.in Panel Meeting

More information

The 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 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 information

Space Weather Awareness in the Arctic. Torsten Neubert Head of Section for Solar System Physics

Space Weather Awareness in the Arctic. Torsten Neubert Head of Section for Solar System Physics Space Weather Awareness in the Arctic Torsten Neubert Head of Section for Solar System Physics Technology in the Arctic There is significant potential Resources Tourism helped by receding ocean ice There

More information

Chapter 10 Our Star. X-ray. visible

Chapter 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 information

The 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 % 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 information

The Magnetic Sun. CESAR s Booklet

The 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 information

Chapter 14 Lecture. Chapter 14: Our Star Pearson Education, Inc.

Chapter 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 information

Chapter 14 Our Star A Closer Look at the Sun. Why was the Sun s energy source a major mystery?

Chapter 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 information

Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances

Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers

More information

The Project. National Schools Observatory

The Project. National Schools Observatory Sunspots The Project This project is devised to give students a good understanding of the structure and magnetic field of the Sun and how this effects solar activity. Students will work with sunspot data

More information

High energy particles from the Sun. Arto Sandroos Sun-Earth connections

High 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 information

The Sun. 1a. The Photosphere. A. The Solar Atmosphere. 1b. Limb Darkening. A. Solar Atmosphere. B. Phenomena (Sunspots) C.

The Sun. 1a. The Photosphere. A. The Solar Atmosphere. 1b. Limb Darkening. A. Solar Atmosphere. B. Phenomena (Sunspots) C. The Sun 1 The Sun A. Solar Atmosphere 2 B. Phenomena (Sunspots) Dr. Bill Pezzaglia C. Interior Updated 2006Sep18 A. The Solar Atmosphere 1. Photosphere 2. Chromosphere 3. Corona 4. Solar Wind 3 1a. The

More information

Space Weather. S. Abe and A. Ikeda [1] ICSWSE [2] KNCT

Space 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 information

Toward Interplanetary Space Weather: Strategies for Manned Missions to Mars

Toward 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 information

Chapter 14 Lecture. The Cosmic Perspective Seventh Edition. Our Star Pearson Education, Inc.

Chapter 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 information

Solar Flare Variations

Solar 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

Helios in Greek and Sol in Roman

Helios 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 information

Uncertainties in estimates of the occurrence rate of rare space weather events

Uncertainties in estimates of the occurrence rate of rare space weather events Uncertainties in estimates of the occurrence rate of rare space weather events Jeffrey J. Love Geomagnetism Program USGS Natural Hazards Mission jlove@usgs.gov Love, J. J., 2012. Credible occurrence probabilities

More information

STCE Newsletter. 18 Jan Jan 2016

STCE Newsletter. 18 Jan Jan 2016 Published by the STCE - this issue : 29 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 information

Nuclear Spectroscopy: Radioactivity and Half Life

Nuclear 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 information

SPACE WEATHER: STORMS FROM THE SUN

SPACE 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 information

Ba (Z = 56) W (Z = 74) preferred target Mo (Z = 42) Pb (Z = 82) Pd (Z = 64)

Ba (Z = 56) W (Z = 74) preferred target Mo (Z = 42) Pb (Z = 82) Pd (Z = 64) Produced by accelerating electrons with high voltage and allowing them to collide with metal target (anode), e.g, Tungsten. Three Events (Two types of x-ray) a) Heat X-Ray Tube b) bremsstrahlung (braking

More information

A Model for Integrin Binding in Cells

A Model for Integrin Binding in Cells A Model for Integrin Binding in Cells By: Kara Huyett Advisor: Doctor Stolarska 31 st of August, 2015 Cell movement, and cell crawling in particular, has implications in various biological phenomena. For

More information

How is Earth s Radiation Belt Variability Controlled by Solar Wind Changes

How 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 information

Teacher Background: The Dancing Lights Program

Teacher Background: The Dancing Lights Program Teacher Background: The Dancing Lights Program The Sun Many people think the Sun is just a fiery yellow ball. The Sun isn t actually burning because fire requires oxygen. Really, the Sun a giant ball of

More information

1. Solar Atmosphere Surface Features and Magnetic Fields

1. 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 information

Module 4: Astronomy - The Solar System Topic 2 Content: Solar Activity Presentation Notes

Module 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 information

Invention of microscopes and telescopes expanded understanding of the Earth revealing new things

Invention of microscopes and telescopes expanded understanding of the Earth revealing new things Miss Loulousis Began with careful observation Scientists in China began keeping records of earthquakes as early as 780BCE Maya tracked movements of the sun, moon, and planets Created calendars from observations

More information

Multi-wavelength VLA and Spacecraft Observations of Evolving Coronal Structures Outside Flares

Multi-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 information

Understanding Cell Motion and Electrotaxis with Computational Methods

Understanding Cell Motion and Electrotaxis with Computational Methods Understanding Cell Motion and Electrotaxis with Computational Methods Blake Cook 15th of February, 2018 Outline 1 Biological context 2 Image analysis 3 Modelling membrane dynamics 4 Discussion Outline

More information

1 Radioactivity BEFORE YOU READ. Atomic Energy. National Science Education Standards STUDY TIP

1 Radioactivity BEFORE YOU READ. Atomic Energy. National Science Education Standards STUDY TIP CHAPTER 4 1 Radioactivity SECTION Atomic Energy BEFORE YOU READ After you read this section, you should be able to answer these questions: What are three types of radioactive decay? How does radiation

More information

Solar eruptive phenomena

Solar eruptive phenomena Solar eruptive phenomena Andrei Zhukov Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium 26/01/2018 1 Eruptive solar activity Solar activity exerts continous influence on the solar

More information

Interplanetary coronal mass ejections that are undetected by solar coronagraphs

Interplanetary coronal mass ejections that are undetected by solar coronagraphs Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012920, 2008 Interplanetary coronal mass ejections that are undetected by solar coronagraphs T. A. Howard 1 and

More information

10/17/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline

10/17/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline 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 FIRE? Chemical

More information

An X-ray Observations of A Gradual Coronal Mass Ejections (CMEs) on 15th April 2012

An X-ray Observations of A Gradual Coronal Mass Ejections (CMEs) on 15th April 2012 International Letters of Chemistry, Physics and Astronomy Online: 2014-02-06 ISSN: 2299-3843, Vol. 27, pp 13-19 doi:10.18052/www.scipress.com/ilcpa.27.13 2014 SciPress Ltd., Switzerland An X-ray Observations

More information

Astronomy Ch 16 The Sun. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy 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 information

About the Van Allen Probes Mission

About the Van Allen Probes Mission Van Allen Probes Exploring th About the Van Allen Probes Mission To help us understand how Earth responds to changes in the sun s energy and how that response affects life and society, NASA launched the

More information

Solar Activity during the Rising Phase of Solar Cycle 24

Solar Activity during the Rising Phase of Solar Cycle 24 International Journal of Astronomy and Astrophysics, 213, 3, 212-216 http://dx.doi.org/1.4236/ijaa.213.3325 Published Online September 213 (http://www.scirp.org/journal/ijaa) Solar Activity during the

More information

Sun s Properties. Overview: The Sun. Composition of the Sun. Sun s Properties. The outer layers. Photosphere: Surface. Nearest.

Sun 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 information

Chapter 8 Geospace 1

Chapter 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 information

Announcements. - 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 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 information

Solar Flare Durations

Solar 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 information

Relation between Solar Activity Features and Geomagnetic Activity Indices during Cycle-24

Relation between Solar Activity Features and Geomagnetic Activity Indices during Cycle-24 Corona Journal of Science and Technology ISSN : 2319 6327 (Online), Vol. 4, No. III (215), pp. 7-12 @Corona Publication http://www.coronapublication.com Relation between Solar Activity Features and Geomagnetic

More information

Chap 14: The Sun A Typical Star Here s the Story I ll Unfold for you

Chap 14: The Sun A Typical Star Here s the Story I ll Unfold for you Chap 14: The Sun A Typical Star Here s the Story I ll Unfold for you What s it made of? A star: self-supporting partially ionized gas balancing gravity w/ pressure Nuclear fusion and how it powers the

More information

Solar Structure. Connections between the solar interior and solar activity. Deep roots of solar activity

Solar Structure. Connections between the solar interior and solar activity. Deep roots of solar activity Deep roots of solar activity Michael Thompson University of Sheffield Sheffield, U.K. michael.thompson@sheffield.ac.uk With thanks to: Alexander Kosovichev, Rudi Komm, Steve Tobias Connections between

More information

Signatures of Geomagnetic Storms and Coronal Mass Ejections on Electron and Ion Temperatures At Low Latitude Upper Ionosphere

Signatures of Geomagnetic Storms and Coronal Mass Ejections on Electron and Ion Temperatures At Low Latitude Upper Ionosphere International Journal of Physics and Applications. ISSN 0974-3103 Volume 7, Number 1 (2015), pp. 43-48 International Research Publication House http://www.irphouse.com Signatures of Geomagnetic Storms

More information

Astronomy 101 Lab: Solar Observing

Astronomy 101 Lab: Solar Observing Name: Astronomy 101 Lab: Solar Observing Pre-Lab Assignment: In this lab, you will determine the rotation rate of the Sun, determine the speed of material ejected from the Sun in a coronal mass ejection,

More information

Earth Space Systems. Semester 1 Exam. Astronomy Vocabulary

Earth Space Systems. Semester 1 Exam. Astronomy Vocabulary Earth Space Systems Semester 1 Exam Astronomy Vocabulary Astronomical Unit- Aurora- Big Bang- Black Hole- 1AU is the average distance between the Earth and the Sun (93 million miles). This unit of measurement

More information

Geomagnetic Disturbances (GMDs) History and Prediction

Geomagnetic 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 information

The Sun ASTR /17/2014

The 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 information

The Sun. The Chromosphere of the Sun. The Surface of the Sun

The Sun. The Chromosphere of the Sun. The Surface of the Sun Key Concepts: Lecture 22: The Sun Basic properties of the Sun The outer layers of the Sun: Chromosphere, Corona Sun spots and solar activity: impact on the Earth Nuclear Fusion: the source of the Sun s

More information

Sun Earth Connection Missions

Sun 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 information

The Solar Wind Space physics 7,5hp

The 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 information

Space Physics. An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres. May-Britt Kallenrode. Springer

Space 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 information

Magnetic storms. Anke Witzky. 29th October 2008

Magnetic storms. Anke Witzky. 29th October 2008 Magnetic storms Anke Witzky 29th October 2008 1 CONTENTS 1 Contents 1 Are magnetic storms some kind of weather? 2 2 How humans recovered space weather 2 3 What happens out there? 4 4 Magnetic storms an

More information

Classification of Coronal Mass Ejections and Image Processing Techniques

Classification of Coronal Mass Ejections and Image Processing Techniques Classification of Coronal Mass Ejections and Image Processing Techniques Chris Lowder Institute for Astronomy, University of Hawai i at Manoa Advisor : Dr. Shadia Habbal Department of Physics, Georgia

More information

Nicholas J. Giordano. Chapter 30. Nuclear Physics. Marilyn Akins, PhD Broome Community College

Nicholas J. Giordano.   Chapter 30. Nuclear Physics. Marilyn Akins, PhD Broome Community College Nicholas J. Giordano www.cengage.com/physics/giordano Chapter 30 Nuclear Physics Marilyn Akins, PhD Broome Community College Atomic Nuclei Rutherford s discovery of the atomic nucleus caused scientists

More information

INTERPLANETARY ASPECTS OF SPACE WEATHER

INTERPLANETARY 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 information

Episode 402: Fields, field lines and field strength

Episode 402: Fields, field lines and field strength Episode 402: Fields, field lines and field strength This episode introduces the notion of a field of force and how we can diagrammatically represent such a field using field lines. The actual strength

More information

Magnetic Drivers of CME Defection in the Low Corona

Magnetic Drivers of CME Defection in the Low Corona Magnetic Drivers of CME Defection in the Low Corona C. Kay (Boston University) M. Opher (Boston University) R. M. Evans (NASA GSFC/ORAU T. I. Gombosi (University of Michigan) B. van der Holst (University

More information

Review III. ASTR 371, Fall Jovian Planets and Rings (Lecture Notes 9; Chap 12, 14)

Review III. ASTR 371, Fall Jovian Planets and Rings (Lecture Notes 9; Chap 12, 14) ASTR 371, Fall 2016 Review III 9. Jovian Planets and Rings (Lecture Notes 9; Chap 12, 14) 9.1-2 Introduction, Motion a. Carefully study the data for the Jovian planets. Must know the general properties

More information