The Powerhouse at the Center of the Sun. The interior of the Sun is a region of extreme physical conditions.

Slides:

Advertisements

Similar presentations

Unit 3 Energy and Work.

Advertisements

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?

Stellar Evolution. 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.

Announcements Welcome back to Standard Time! Wednesday night star parties begin this week, 8:45 pm, weather permitting. Attend one for 4 points extra credit!

Energy Production in the Sun Physics 113 Goderya Chapter(s): 8 Learning Outcomes:

2. Our favourite star The Sun photographed in soft X-rays.

ASTR100 (Spring 2008) Introduction to Astronomy Our Star Prof. D.C. Richardson Sections

CH – THE SUN Chapter 29 – March 13 th, 2015.

Stellar Interiors Astronomy 315 Professor Lee Carkner Lecture 10.

Center of Mass. Motion of the Center of Mass The center of mass of a system moves as if all of the mass of the system were concentrated at that point.

26 July 2005AST 2010: Chapter 151 The Sun: A Nuclear Powerhouse.

1 The Sun Our star - inside and out. 2 Earth having a really, really bad day.

Astronomy 100 Tuesday, Thursday 2:30 - 3:45 pm Tom Burbine

Ch9 THE SUN AND STARS The star we see by day. Ch9 The Sun, Our Star The Sun is an average star. From the Sun, we base our understanding of all stars in.

Momentum For N particles: Why bother introducing one more definition? Most general form of the Newton’s law: Valid when mass is changing Valid in relativistic.

Today’s APODAPOD  Read Chapter 11  Homework and Quiz 9 this week on Friday  Last Solar Lab on TOMORROW at NOON The Sun Today A100 The Sun.

Unit 2 – The Atom Nuclear Chemistry Fusion and Fission.

Opening Activity 1.As a star runs out of nuclear energy, what do you think will occur to the size of the star? Provide an explanation as to why you think.

PHYS The Solar Atmosphere Photosphere: visible “surface” of the Sun, about 500 km thick. Moving outwards temperature falls from 8000 K to 4500 K.

Stars Thursday, February 28. Thu, Feb 28: Stars Tue, Mar 4: Planets Problem Set #7 due Thu, Mar 6: Past & Future Problem Set #7 returned 1:30 pm Final.

During the nineteenth century, scientists suggested that the Earth was hundreds of millions of years old. During the nineteenth century, scientists suggested.

Unit 8 Section 2: Nuclear Reactions

Section 1: Structure of the Sun

Fission= to split In Biology, tissue grows by the division of cells.

Nuclear Reactions: AN INTRODUCTION TO FISSION & FUSION Farley Visitors Center.

PHYS 205 Powerhouse PHYS 205 Possible sources Chemical Energy: Sun has hydrogen and if it has oxygen, than we can make water. will last 18,000 years.

The Sun Section 1 Section 1: Structure of the Sun Preview Objectives The Sun’s Energy Nuclear Fusion Mass Changing into Energy The Sun’s Interior The Sun’s.

Earth Science 24.3B The Sun’s Interior The Solar Interior.

Chapter 29 The Sun 29.1 Structure of the Sun

Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Solar Interior/ Nuclear Fusion.

THERMONUCLEAR FUSION (HYDROGEN “BURNING”) Stars condense out of the gas and dust clouds in the Milky Way Galaxy. As they collapse into a spherical shape.

Section 1: Structure of the Sun

A105 Stars and Galaxies  News Quiz Today  Review Exam 1  Homework 6 (the Sun) due Thursday Today’s APODAPOD.

The power plant of the Sun and stars. Nuclear Reactions in Stellar Interiors H + H 2 H + e + + nu H + 2 H 3 He + gamma 3 He + 3 He 4 He + H + H Net effect:

© 2010 Pearson Education, Inc. 1. The Sun appears bright orange because of the extremely hot fires that are constantly burning carbon. TRUE or FALSE 2.

E = mc 2. E = mc 2 is everywhere! E = mc 2 Energy (in joules) = Mass (in kilograms) X = Mass (in kilograms) X The Speed of Light Squared (in meters squared.

The Heart of the Sun Energy Generation in Sun-like Stars.

1 23. A chemist claimed that in Experiment 2, the pH of the sample solution was greater at a value of 0.2 mL of titrant added than at a value of 1.8.

© 2010 Pearson Education, Inc. Our goals for learning:  Why was the Sun’s energy source a major mystery?  Why does the Sun shine?  What is the Sun’s.

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?

The “fuel cycle” of the Sun. Last time: chemical reactions have far too little energy available per mass to power the Sun over geological time.

Lecture 16…Significance of the Hertzsprung Russell Diagram.

Galaxies The basic structural unit of matter in the universe is the galaxy A galaxy is a collection of billions of _____________, gas, and dust held together.

NUCLEAR FUSION.

Introduction to Nuclear Fission and Fusion

Sun Nuclear Reactions If the mass in the center of the solar nebula is large enough, gravity will collapse more and more material, producing higher and.

Nuclear Reactions: FISSION & FUSION ã Nuclear reactions deal with interactions between the nuclei of atoms ã Both fission and fusion processes deal with.

Nuclear Reactions: AN INTRODUCTION TO FISSION & FUSION Farley Visitors Center.

Main Sequence Stars Internal structure Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.

Chapters 14 and 15 Stellar Evolution and Stellar Remnants.

The Sun. Properties M = 2 X kg = 300,000 M Earth R = 700,000 km > 100 R Earth 70% H, 28% He T = 5800 K surface, 15,000,000 K core.

Fission and Fusion are both nuclear reactions that involve the particles in the nucleus of an atom.

The Sun?. The Sun is a star! There are an incredible amount of stars in the universe. Yay! What is a star…?

After the Big Bang. ENERGY & MASS The infant Universe was searingly HOT! It was full of energy of intense radiation. Albert Einstein’s equation E=mc2.

Earth in Space Benchmarks

Nuclear Energy.

Burning … is a chemical reaction: fusion with oxygen Coal:

The Sun and its hidden powerhouse

Our star, the SUN.

How Does the Sun Get Its Energy?

Charles Hakes Fort Lewis College 1.

Section 1: Structure of the Sun

Lecture 17- Nuclear Reactions in Stellar Interiors

Nuclear Energy.

Burning … is a chemical reaction: fusion with oxygen Coal:

The Sun and Other Stars 14-2.

Fusion in the Sun.

The sun: Our very own star

Presentation transcript:

The Powerhouse at the Center of the Sun

The interior of the Sun is a region of extreme physical conditions

Next topic: what is the luminosity of the Sun telling us? Luminosity = 3.847X10 26 Watts What fuel cycle could provide this? What fuel cycle could provide this for the lifetime of the Sun?

Say it with equations! (easy ones) Luminosity = power =energy/time Energy=powerXtime (Watts X seconds = Joules) Time=energy/power Let’s see how long we could keep the Sun shining with a known, powerful energy source

Coal Coal runs civilization Energy content: 24 MegaJoules/kilogram= 2.4X10 7 Joules/kg If the Sun were made of coal, how long could it “burn”, providing its current power or luminosity?

Power and the Sun Mass of Sun = 2X10 30 kilograms Total energy content of “coal Sun”=(2X10 30 )X(2.4X10 7 ) =4.8X10 37 Joules Time the Sun could “keep this up” = energy/luminosity =4.8X10 37 /3.8X10 26 =1.3X10 11 seconds Is this a lot or a little????

A strong conclusion: energy drawn from coal burning, or any other chemical reaction, is grossly inadequate to power the Sun over geological timescales

Some vastly more powerful energy source (than chemical reactions) must be occurring in the Sun and stars

A microscopic view of chemical reactions: interactions of the electron cloud

Nuclear reactions: interactions among the nuclei (Figure 17.2)

Nuclear Reactions in Stellar Interiors H + H 2 H + e + + nu H + 2 H 3 He + gamma 3 He + 3 He 4 He + H + H Net effect: 4H 4 He Question: why does this occur exclusively in the core of a star? Demo

A small mass difference between Hydrogen and Helium 4 Hydrogen atoms: 6.693E-27 kg 1 Helium atom: 6.645E-27 kg Difference = 0.048E-27 kg Difference = 0.7 percent Why is this small difference important?

The Einstein Energy-Mass equivalence relation E=mc 2 c=speed of light You get a lot of bang for the buck: 6.3E+14 J/kg

Stars have a lot of fuel in the form of hydrogen These abundances Are characteristic of the Solar photosphere, and Nearly all other stars

The Power Source of Main Sequence Stars MS stars fuse hydrogen into helium, releasing prodigious amounts of energy in the process. Their fuel source is the matter of which they are made

The Structure of Main Sequence Stars The Powerhouse

How can we tell if this is right? Detect neutrinos emitted from the center of the Sun.

The Neutrino Sun: A View into the Solar Interior

Nuclear reactions explain a lot about the Sun, but what is going on on the rest of the Main Sequence?

The fuel for a main sequence star is its own mass in the form of hydrogen. The total amount of fuel is proportional to the total mass of the star. What are the masses of stars?

How We Determine Masses of Stars Method:observation of binary stars (double stars)

Binary stars are numerous (e.g. Sirius )

We can see orbital motion of Sirius B around Sirius A

Masses of stars determine the gravitational force, and thus the acceleration of the stars