10/18/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline

Size: px
Start display at page:

Download "10/18/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline"

Transcription

1 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 FIRE? Chemical Energy Content ~ 10,000 years Luminosity Is it on FIRE? NO! Chemical Energy Content ~ 10,000 years Luminosity 1

2 10/18/17 Is it CONTRACTING? Gravitational Potential Energy ~ 25 million years Luminosity Is it CONTRACTING? E = mc2 Einstein, 1905 Is it CONTRACTING? NO! Gravitational Potential Energy ~ 25 million years Luminosity It is powered by NUCLEAR ENERGY! Nuclear Potential Energy (core) ~ 10 billion years Luminosity Weight of upper layers compresses lower layers Pearson Education, Inc. Weight of upper layers compresses lower layers. 2

3 Gravitational equilibrium: Gravity pulling in balances pressure pushing out. Energy balance: Thermal energy released by fusion in core balances radiative energy lost from surface. Gravitational contraction provided energy that heated the core as the Sun was forming. What is the Sun's structure? Contraction stopped when fusion started replacing the energy radiated into space. Radius: m (109 times Earth) Mass: kg (300,000 Earths) Solar wind: A flow of charged particles from the surface of the Sun Luminosity: watts 3

4 Corona: Outermost layer of solar atmosphere ~ 1 million K Chromosphere: Middle layer of solar atmosphere ~ K Photosphere: Visible surface of the Sun ~ 6000 K Convection zone: Energy transported upward by rising hot gas Radiation zone: Energy transported upward by photons Core: Energy generated by nuclear fusion ~ 15 million K 4

5 11.2 Nuclear Fusion in the Sun How does nuclear fusion occur in the Sun? Our goals for learning: How does nuclear fusion occur in the Sun? How does the energy from fusion get out of the Sun? How do we know what is happening inside the Sun? High temperatures enable nuclear fusion to happen in the core. Fission Big nucleus splits into smaller pieces. (Nuclear power plants) Fusion Small nuclei stick together to make a bigger one. (Sun, stars) The Sun releases energy by fusing four hydrogen nuclei into one helium nucleus. The Proton proton chain is how hydrogen fuses into helium in the Sun. 5

6 Thought Question IN 4 protons OUT 4 He nucleus 2 gamma rays 2 positrons 2 neutrinos Total mass is 0.7% lower. What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy? A. The core would expand and heat up slightly. B. The core would expand and cool. C. The Sun would blow up like a hydrogen bomb. Thought Question Solar Thermostat What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy? A. The core would expand and heat up slightly. B. The core would expand and cool. C. The Sun would blow up like a hydrogen bomb. Solar thermostat keeps the rate of fusion steady. Decline in core temperature causes fusion rate to drop, so core contracts and heats up. Rise in core temperature causes fusion rate to rise, so core expands and cools down. How does the energy from fusion get out of the Sun? Energy gradually leaks out of the radiation zone in the form of randomly bouncing photons. 6

7 Convection (rising hot gas) takes energy to the surface. Bright blobs on photosphere where hot gas reaches the surface How do we know what is happening inside the Sun? We learn about the inside of the Sun by making mathematical models observing solar vibrations observing solar neutrinos Patterns of vibration on the surface tell us about what the Sun is like inside. Data on solar vibrations agree with mathematical models of solar interior Pearson Education, Inc. 7

8 10/18/17 Solar neutrino problem: Neutrinos created during fusion fly directly through the Sun. Early searches for solar neutrinos failed to find the predicted number. Observations of these solar neutrinos can tell us what's happening in the core Pearson Education, Inc. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number. Solar neutrino problem: More recent observations find the right number of neutrinos, but some have changed form. These careful measurements were awarded the Nobel Prize in physics in Pearson Education, Inc. The solar neutrino problem led to the understanding that neutrinos have mass 11.3 The Sun Earth Connection Our goals for learning: What causes solar activity? How does solar activity vary with time? A full-sky neutrino map, centered on the Sun, produced by the Super-Kamiokande neutrino observatory in Japan. 8

9 What causes solar activity? Solar activity is like "weather" on Earth. Sunspots Solar flares Solar prominences All these phenomena are related to magnetic fields. Sunspots Are cooler than other parts of the Sun's surface (4000 K). Zeeman Effect We can measure magnetic fields in sunspots by observing the splitting of spectral lines. Are regions with strong magnetic fields. Charged particles spiral along magnetic field lines. Loops of bright gas often connect sunspot pairs. 9

10 10/18/17 Magnetic activity also causes solar prominences that erupt high above the Sun's surface. Magnetic activity causes solar flares that send bursts of X rays and charged particles into space. Coronal mass ejections send bursts of energetic charged particles out through the solar system. The corona appears bright in X-ray photos in places where magnetic fields trap hot gas. How does solar activity vary with time? Charged particles streaming from the Sun can disrupt electrical power grids and disable communications satellites. 10

11 The number of sunspots rises and falls in 11-year cycles. The sunspot cycle has something to do with the winding and twisting of the Sun's magnetic field. How does solar activity vary with time? Sunspots and Earth s climate Does solar activity and/or the sunspot cycle affect the Earth s climate? The Maunder minimum ( ) corresponds to a time of very low temperatures recorded in Europe and North American known as the Little Ice Ages. However, clear connections have not been established and the study of solar activity s possible effects on climate remains an active field of research. It is unclear whether the sunspot cycle affects Earth s climate in any way, but it almost certainly is not responsible for global warming Pearson Education, Inc. 11

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

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

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

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

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

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

14.1 A Closer Look at the Sun

14.1 A Closer Look at the Sun 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? NO! Chemical energy content Luminosity ~

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

Today The Sun. Events

Today The Sun. Events Today The Sun Events Last class! Homework due now - will count best 5 of 6 Final exam Dec. 20 @ 12:00 noon here Review this Course! www.case.edu/utech/course-evaluations/ The Sun the main show in the solar

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

A100 Exploring the Universe: How Stars Work. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: How Stars Work. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: How Stars Work Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu October 07, 2014 Read: Chaps 14, 15 10/07/12 slide 1 Exam scores posted in Mastering Questions

More information

Convection causes granules. Photosphere isn t actually smooth! Granules Up-Close: like boiling water. Corona or of the Sun. Chromosphere: sphere of

Convection causes granules. Photosphere isn t actually smooth! Granules Up-Close: like boiling water. Corona or of the Sun. Chromosphere: sphere of Overview 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 source

More information

9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is

9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is 1 9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is produced by the proton-proton chain in which four hydrogen

More information

The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun

The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun The Sun The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x 10 33 g = 330,000 M Earth = 1 M Sun Radius of Sun = 7 x 10 5 km = 109 R Earth = 1 R Sun Luminosity of Sun =

More information

Hydrogen Lines. What can we learn from light? Spectral Classification. Visible Hydrogen Spectrum Lines: Series. Actual Spectrum from SDSS

Hydrogen Lines. What can we learn from light? Spectral Classification. Visible Hydrogen Spectrum Lines: Series. Actual Spectrum from SDSS What can we learn from light? Hydrogen Lines Temperature Energy Chemical Composition Speed towards or away from us All from the! Lower E, Lower f, λ Visible! Higher E, Higher f, λ Visible Hydrogen Spectrum

More information

The General Properties of the Sun

The 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 information

A100 Exploring the Universe: How Stars Work. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: How Stars Work. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: How Stars Work Martin D. Weinberg UMass Astronomy weinberg@astro.umass.edu October 11, 2012 Read: Chaps 14, 15 10/11/12 slide 1 Exam scores posted in Mastering Exam keys posted

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

The Sun. October 21, ) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots

The Sun. October 21, ) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots The Sun October 21, 2002 1) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots Review Blackbody radiation Measuring stars distance luminosity brightness and distance

More information

Correction to Homework

Correction 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 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

The Sun is the nearest star to Earth, and provides the energy that makes life possible.

The Sun is the nearest star to Earth, and provides the energy that makes life possible. 1 Chapter 8: The Sun The Sun is the nearest star to Earth, and provides the energy that makes life possible. PRIMARY SOURCE OF INFORMATION about the nature of the Universe NEVER look at the Sun directly!!

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

The Sun Our Extraordinary Ordinary Star

The Sun Our Extraordinary Ordinary Star The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the

More information

An Overview of the Details

An Overview of the Details The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the

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

The Sun sends the Earth:

The 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 information

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

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 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 information

An Overview of the Details

An Overview of the Details Guiding Questions The Sun Our Extraordinary Ordinary Star 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the Sun

More information

11/19/08. Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity. Weight of upper layers compresses lower layers

11/19/08. Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity. Weight of upper layers compresses lower layers Gravitational equilibrium: The outward push of pressure balances the inward pull of gravity Weight of upper layers compresses lower layers Gravitational equilibrium: Energy provided by fusion maintains

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 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

The Sun. How are these quantities measured? Properties of the Sun. Chapter 14

The Sun. How are these quantities measured? Properties of the Sun. Chapter 14 The Sun Chapter 14 The Role of the Sun in the Solar System > 99.9% of the mass Its mass is responsible for the orderly orbits of the planets Its heat is responsible for warming the planets It is the source

More information

Astronomy Chapter 12 Review

Astronomy 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 information

How the Sun Works. Presented by the

How the Sun Works. Presented by the How the Sun Works Presented by the The Sun warms our planet every day, provides the light by which we see and is absolutely necessary for life on Earth. In this presentation, we will examine the fascinating

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

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

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

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 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 information

Astronomy Exam 3 - Sun and Stars

Astronomy Exam 3 - Sun and Stars Astronomy Exam 3 - Sun and Stars Study online at quizlet.com/_4zgp6 1. `what are the smallest group of stars in the H-R diagram 2. A star has a parallax of 0.05". what is the distance from the earth? white

More information

Weight of upper layers compresses lower layers

Weight 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 information

The Sun. Chapter 12. Properties of the Sun. Properties of the Sun. The Structure of the Sun. Properties of the Sun.

The Sun. Chapter 12. Properties of the Sun. Properties of the Sun. The Structure of the Sun. Properties of the Sun. Chapter 12 The Sun, Our Star 1 With a radius 100 and a mass of 300,000 that of Earth, the Sun must expend a large amount of energy to withstand its own gravitational desire to collapse To understand this

More information

Stars and Galaxies. The Sun and Other Stars

Stars and Galaxies. The Sun and Other Stars CHAPTER 22 Stars and Galaxies LESSON 2 The Sun and Other Stars What do you think? Read the two statements below and decide whether you agree or disagree with them. Place an A in the Before column if you

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

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

The Quiet Sun The sun is currently being studied by several spacecraft Ulysses, SOHO, STEREO, and ACE.

The Quiet Sun The sun is currently being studied by several spacecraft Ulysses, SOHO, STEREO, and ACE. The Quiet Sun The sun is currently being studied by several spacecraft Ulysses, SOHO, STEREO, and ACE. Messenger also contains instruments that can do some solar studies. http://www.stereo.gsfc.nasa.gov

More information

Some Good News. Announcements. Lecture 10 The Sun. How does the Sun shine? The Sun s Energy Source

Some Good News. Announcements. Lecture 10 The Sun. How does the Sun shine? The Sun s Energy Source Announcements Homework due today. Put your homework in the box NOW. Please STAPLE them if you have not done yet. Quiz#3 on Tuesday (Oct 5) Announcement at the end of this lecture. If you could not pick

More information

Astronomy 1 Fall Reminder: When/where does your observing session meet? [See from your TA.]

Astronomy 1 Fall Reminder: When/where does your observing session meet? [See  from your TA.] Astronomy 1 Fall 2016 Reminder: When/where does your observing session meet? [See email from your TA.] Lecture 9, October 25, 2016 Previously on Astro-1 What is the Moon made of? How did the Moon form?

More information

1 A= one Angstrom = 1 10 cm

1 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 information

The Sun 11/6/2018. Phys1411 Introductory Astronomy. Topics we have covered. Topics for Today class. Sun Spots

The Sun 11/6/2018. Phys1411 Introductory Astronomy. Topics we have covered. Topics for Today class. Sun Spots Foundations of Astronomy 13e Seeds Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 8 The Sun Topics we have covered I. Introduction A. Viewing the Sun B. General Definition C. General Properties

More information

The Sun: Our Star. A glowing ball of gas held together by its own gravity and powered by nuclear fusion

The Sun: Our Star. A glowing ball of gas held together by its own gravity and powered by nuclear fusion Our Star, the Sun The Sun: Our Star A glowing ball of gas held together by its own gravity and powered by nuclear fusion Radius: 700,000 km (435,000 miles) Diameter: 1.392 million km (865,000 miles) Circumference:

More information

The Sun: Our Star. The Sun is an ordinary star and shines the same way other stars do.

The Sun: Our Star. The Sun is an ordinary star and shines the same way other stars do. The Sun: Our Star The Sun is an ordinary star and shines the same way other stars do. Announcements q Homework # 4 is due today! q Units 49 and 51 Assigned Reading Today s Goals q Today we start section

More information

Radiation Zone. AST 100 General Astronomy: Stars & Galaxies. 5. What s inside the Sun? From the Center Outwards. Meanderings of outbound photons

Radiation 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 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

The interior of the Sun. Space Physics - Project by Christopher Keil. October 17, Supervisor: Prof. Kjell Rnnemark

The interior of the Sun. Space Physics - Project by Christopher Keil. October 17, Supervisor: Prof. Kjell Rnnemark The interior of the Sun Space Physics - Project by Christopher Keil October 17, 2006 Supervisor: Prof. Kjell Rnnemark Umeå University Institute of Physics Contents 1 Introduction 2 2 The Structure of the

More information

The Sun. Nearest Star Contains most of the mass of the solar system Source of heat and illumination

The Sun. Nearest Star Contains most of the mass of the solar system Source of heat and illumination The Sun Nearest Star Contains most of the mass of the solar system Source of heat and illumination Outline Properties Structure Solar Cycle Energetics Equation of Stellar Structure TBC Properties of Sun

More information

The Sun. The Sun Is Just a Normal Star 11/5/2018. Phys1411 Introductory Astronomy. Topics. Star Party

The 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 information

Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere.

Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere. Chapter 29 and 30 Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere. Explain how sunspots are related to powerful magnetic fields on the sun.

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. SESAME Astronomy Week 4. Thursday, February 10, 2011

The Sun. SESAME Astronomy Week 4. Thursday, February 10, 2011 The Sun SESAME Astronomy Week 4 1 1 Our star Not special: typical mass, typical temperature, typical size, typical planetary system about halfway through its 10 billion year lifespan 2 2 Vital statistics

More information

Lecture 13: The Sun, and how stars work. Astronomy 111 Wednesday October 11, 2017

Lecture 13: The Sun, and how stars work. Astronomy 111 Wednesday October 11, 2017 Lecture 13: The Sun, and how stars work Astronomy 111 Wednesday October 11, 2017 Reminders Star party tomorrow night! Homework #6 due Monday How do stars work? What is a star? What is a star composed of?

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

The Sun 11/27/2017. Phys1411 Introductory Astronomy. Exam 3. Topics we have covered. Sun Spots. Topics for Today class

The Sun 11/27/2017. Phys1411 Introductory Astronomy. Exam 3. Topics we have covered. Sun Spots. Topics for Today class Foundations of Astronomy 13e Seeds Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 8 The Sun Exam 3 Wednesday November 29 th Homework for Chapter 7 and 8 are online on MindTap: Due Wednesday

More information

Our Star: The Sun. Layers that make up the Sun. Understand the Solar cycle. Understand the process by which energy is generated by the Sun.

Our Star: The Sun. Layers that make up the Sun. Understand the Solar cycle. Understand the process by which energy is generated by the Sun. Goals: Our Star: The Sun Layers that make up the Sun. Understand the Solar cycle. Understand the process by which energy is generated by the Sun. Components of the Sun Solar Interior: Core: where energy

More information

Astr 1050 Mon. March 30, 2015 This week s Topics

Astr 1050 Mon. March 30, 2015 This week s Topics Astr 1050 Mon. March 30, 2015 This week s Topics Chapter 14: The Sun, Our Star Structure of the Sun Physical Properties & Stability Photosphere Opacity Spectral Line Formation Temperature Profile The Chromosphere

More information

The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star

The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star Why is the Sun hot and bright? Surface Temperature of the Sun: T =

More information

Stars. The size of the Sun

Stars. The size of the Sun Stars Huge spheres of gas floating in space Composed primarily of H, He. Produce their own energy. Our Galaxy: 10 11 (100 billion) stars. The Sun: a typical star Stars range from ~ 0.1 to ~ 20 M M = solar

More information

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 8

Phys 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 information

Chapter 24: Studying the Sun. 24.3: The Sun Textbook pages

Chapter 24: Studying the Sun. 24.3: The Sun Textbook pages Chapter 24: Studying the Sun 24.3: The Sun Textbook pages 684-690 The sun is one of the 100 billion stars of the Milky Way galaxy. The sun has no characteristics to make it unique to the universe. It is

More information

Our Dynamic Star. Dr. Katherine Auld Bentonville Public Library March 14, 2017

Our Dynamic Star. Dr. Katherine Auld Bentonville Public Library March 14, 2017 Our Dynamic Star Dr. Katherine Auld Bentonville Public Library March 14, 2017 Overview Basics Energy Source History Changes in the Sun Sunspots CME How do We Know? Changes on Earth Aurora Ice Ages Ocean

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

AST 100 General Astronomy: Stars & Galaxies

AST 100 General Astronomy: Stars & Galaxies AST 100 General Astronomy: Stars & Galaxies On to Our Nearest Star: the SUN ANNOUNCEMENTS PLEASE CHANGE CLICKER FREQUENCY TO 26 De-Mystifying science The case of the Sun Ancient philosophers/scientists

More information

Astronomy 1 Winter 2011

Astronomy 1 Winter 2011 Astronomy 1 Winter 2011 Lecture 19; February 23 2011 Asteroids Comets Meteors Previously on Astro-1 Homework Due 03/02/11 On your own: answer all the review questions in chapters 16 17 and 18 To TAs: answer

More information

Facts About The Sun. The Sun is a star found at the of the Solar System. It makes up around % of the Solar System s mass.

Facts About The Sun. The Sun is a star found at the of the Solar System. It makes up around % of the Solar System s mass. Facts About is a star found at the of the Solar System. It makes up around % of the Solar System s mass. At around 1,392,000 kilometres (865,000 miles) wide, the Sun s is about 110 times wider than Earth

More information

Types of Stars 1/31/14 O B A F G K M. 8-6 Luminosity. 8-7 Stellar Temperatures

Types of Stars 1/31/14 O B A F G K M. 8-6 Luminosity. 8-7 Stellar Temperatures Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars For nearby stars - measure distances with parallax 1 AU d p 8-2 Parallax A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3

More information

1-4-1A. Sun Structure

1-4-1A. 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 information

PTYS/ASTR 206. The Sun 3/1/07

PTYS/ASTR 206. The Sun 3/1/07 The Announcements Reading Assignment Review and finish reading Chapter 18 Optional reading March 2006 Scientific American: article by Gene Parker titled Shielding Space Travelers http://en.wikipedia.org/wiki/solar_variability

More information

Name: Date: 2. The temperature of the Sun's photosphere is A) close to 1 million K. B) about 10,000 K. C) 5800 K. D) 4300 K.

Name: Date: 2. The temperature of the Sun's photosphere is A) close to 1 million K. B) about 10,000 K. C) 5800 K. D) 4300 K. Name: Date: 1. What is the Sun's photosphere? A) envelope of convective mass motion in the outer interior of the Sun B) lowest layer of the Sun's atmosphere C) middle layer of the Sun's atmosphere D) upper

More information

Reading Clicker Q 2/7/17. Topics for Today and Thur. ASTR 1040: Stars & Galaxies

Reading Clicker Q 2/7/17. Topics for Today and Thur. ASTR 1040: Stars & Galaxies ASTR 1040: Stars & Galaxies Solar granulation Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 7 Tues 7 Feb 2017 zeus.colorado.edu/astr1040-toomre Topics for Today and Thur Consider Sun s energy

More information

Lecture 14: The Sun and energy transport in stars. Astronomy 111

Lecture 14: The Sun and energy transport in stars. Astronomy 111 Lecture 14: The Sun and energy transport in stars Astronomy 111 Energy transport in stars What is a star? What is a star composed of? Why does a star shine? What is the source of a star s energy? Laws

More information

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012 Choose the answer that best completes the question. Read each problem carefully and read through all the answers.

More information

Our Sun Our Star. Image credit: JAXA. OU-L P SC 100 Spring, /81

Our Sun Our Star. Image credit: JAXA. OU-L P SC 100 Spring, /81 Our Sun Our Star Image credit: JAXA OU-L P SC 100 Spring, 2009 1/81 1 Diameter: 1,400,000 km = 864,000 miles = 4.5 light-seconds 1,300,000 Earths could fit inside! 109 Earths would fit across the diameter

More information

Announcements. There is no homework next week. Tuesday s sections (right after the midterm) will be cancelled.

Announcements. There is no homework next week. Tuesday s sections (right after the midterm) will be cancelled. 1 Announcements The Midterm is one week away! Bring: Calculator, scantron (big red form), pencil No notes, cellphones, or books allowed. Homework #4 is due this thursday There is no homework next week.

More information

The Sun - II. Alexei Gilchrist

The Sun - II. Alexei Gilchrist The Sun - II Alexei Gilchrist Some resources http://www.nineplanets.org/sol.html The Universe: Secrets of the Sun video Search on youtube Secrets of the Sun (references are to clips here http://www.youtube.com/view_play_list?p=4eef5255d3eef425

More information

8.2 The Sun pg Stars emit electromagnetic radiation, which travels at the speed of light.

8.2 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 information

Astronomy 210. Outline. Nuclear Reactions in the Sun. Neutrinos. Solar Observing due April 15 th HW 8 due on Friday.

Astronomy 210. Outline. Nuclear Reactions in the Sun. Neutrinos. Solar Observing due April 15 th HW 8 due on Friday. Astronomy 210 Outline This Class (Lecture 30): Solar Neutrinos Next Class: Stars: Physical Properties Solar Observing due April 15 th HW 8 due on Friday. The Sun Our closest star The Outer Layers of the

More information

Lecture 17 The Sun October 31, 2018

Lecture 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 information

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes Today Stars Properties (Recap) Nuclear Reactions proton-proton chain CNO cycle Stellar Lifetimes Homework Due Stellar Properties Luminosity Surface Temperature Size Mass Composition Stellar Properties

More information

1 A Solar System Is Born

1 A Solar System Is Born CHAPTER 16 1 A Solar System Is Born SECTION Our Solar System California Science Standards 8.2.g, 8.4.b, 8.4.c, 8.4.d BEFORE YOU READ After you read this section, you should be able to answer these questions:

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

How does the Sun shine? What is the Sun s structure? Lifetime of the Sun. Luminosity of the Sun. Radiation Zone. Core 3/30/17

How does the Sun shine? What is the Sun s structure? Lifetime of the Sun. Luminosity of the Sun. Radiation Zone. Core 3/30/17 What is the Sun s structure? From inside out, the layers are: Core Radiation Zone Convection Zone Photosphere Chromosphere Corona How does the Sun shine? The Sun has its own energy source Main difference

More information

Agenda. 15. Our Star I say Live, Live, because of the Sun, The dream, the excitable gift. The Sun s Energy Source Why Does the Sun Shine?

Agenda. 15. Our Star I say Live, Live, because of the Sun, The dream, the excitable gift. The Sun s Energy Source Why Does the Sun Shine? 15. Our Star I say Live, Live, because of the Sun, The dream, the excitable gift. Anne Sexton (1928 1974) American poet Goodbye my friend it s hard to die When all the birds are singing in the sky Now

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

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

Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m

Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m The Sun Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million earths inside the sun! 70% Hydrogen,

More information

AST 101 Intro to Astronomy: Stars & Galaxies

AST 101 Intro to Astronomy: Stars & Galaxies REVIEW FROM LAST CLASS AST 101 Intro to Astronomy: Stars & Galaxies Do we have direct evidence for fusion in the Sun? ANNOUNCEMENTS: First MIDTERM on FRIDAY 02/27 YES! Neutrinos REVIEW FROM LAST CLASS

More information

Ay 1 Lecture 8. Stellar Structure and the Sun

Ay 1 Lecture 8. Stellar Structure and the Sun Ay 1 Lecture 8 Stellar Structure and the Sun 8.1 Stellar Structure Basics How Stars Work Hydrostatic Equilibrium: gas and radiation pressure balance the gravity Thermal Equilibrium: Energy generated =

More information

3/26/2018. The Sun. Phys1403 Introductory Astronomy. Topics in Chapter 8 that we will cover. Topics in Chapter 8 that we will cover.

3/26/2018. The Sun. Phys1403 Introductory Astronomy. Topics in Chapter 8 that we will cover. Topics in Chapter 8 that we will cover. Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 8 The Sun Topics in Chapter 8 that we will cover General Properties Solar Atmosphere and Surface Temperature

More information

ASTR 100. Lecture 15: The Sun

ASTR 100. Lecture 15: The Sun ASTR 100 Lecture 15: The Sun Start reading about: The Sun (Ch. 10), Spectra (Ch. 5), Stars (Ch. 11) Next week: Stars and Spectra Midterm: Tuesday, February 18 th UW planetarium: Tuesday, March 4 th 3:00pm

More information

Summer 2013 Astronomy - Test 3 Test form A. Name

Summer 2013 Astronomy - Test 3 Test form A. Name Summer 2013 Astronomy - Test 3 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as

More information