OUR STAR SOL. GOALS You will have a basic understanding of how a star functions and how they convert matter into energy You will discuss and write down.

Slides:



Advertisements
Similar presentations
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.
Advertisements

Chapter 11: Our Star © 2015 Pearson Education, Inc.
Copyright © 2012 Pearson Education, Inc. Chapter 10 Our Star 1.
The Sun, our favorite star! WE CAN SEE IT REALLY WELL. The Sun is the basis for all of our knowledge of stars. Why?
THE SUN Bob Davis. Stats Diameter: 1,392,000 Mass: 2 × kilograms Age: 4,570,000,000 years Mostly Hydrogen and Helium Surface Temp: 5,778 K Core.
THE SUN: AWESOME AND ACTIVE
The Sun Astronomy 311 Professor Lee Carkner Lecture 23.
The star we see but seldom notice
The Sun. Overview 1.What is the composition of the Sun? 2.Why does the Sun shine? 3.How do we know its temperature? 4.Why is the Sun hot? (what’s it’s.
The sun and our solar system Grade 9 Science Space Part 2.
The Sun Earth Science - Mr. Gallagher. The Sun is the Earth's nearest star. Similar to most typical stars, it is a large ball of hot electrically charged.
Section 1: Structure of the Sun
For Us, the sun is the provider of Energy; The Provider of Life.
Full name Period II. Chapter 14, section 2: The Sun A. The Sun: is our local star. 1. Spectral Class: G2. 2. Distance to Earth:149,600,000 km *At the speed.
Chapter 5 Lesson 1: The Sun. What is the Sun? A star which produces its own energy (light) There are stars which can make ten million times what the sun.
The Sun 24.3 A typical star powered by nuclear reactions Mostly the (fusion of hydrogen to form helium) Which releases energy.
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.
THE SUN. CLASSIFICATION OF THE SUN Class G Color Yellow Surface Temperature 5,000 – 6,000 ºC Elements hydrogen and helium Greek word for Sun is Helios.
Chapter 28 The Sun Ch Structure of the Sun.
Chapter 29 The Sun 29.1 Structure of the Sun
The Sun Chapter 28.
Survey of the Universe Tom Burbine
The Solar Interior Core Radiation Zone Convection Zone.
The Sun Astronomy 311 Professor Lee Carkner Lecture 23.
Samantha Lythgoe Introductory Astronomy 1040
Definition: All space and objects within the Sun’s gravitational influence. (sun is sol, helios)
OUR SUN THE CLOSEST STAR. Composition of the Sun The Sun is composed of at least 80 of the elements found on Earth. Sun is mostly composed of 91.2% Hydrogen,
Section 1: Structure of the Sun
The Sun’s Size, Heat and Temperature After completing this section, students will explain nuclear fusion, and describe the sun and compare it to other.
Our sun is a star located at the center of our Solar System. It is a huge, spinning ball of hot gas and nuclear reactions that lights up the Earth and.
Unit 2 Lesson 3 The Sun Copyright © Houghton Mifflin Harcourt Publishing Company.
Solar Properties Has more than 99% the mass of our solar system Has more than 99% the mass of our solar system Diameter: 1,390,000 km Diameter: 1,390,000.
Heat Transfer in the Atmosphere Essential Question: How is heat transferred in the atmosphere?
It can be powered by NUCLEAR ENERGY! Luminosity ~ 10 billion years Nuclear Potential Energy (core) E = mc 2 - Einstein, 1905.
The Sun – Our Star Our sun is considered an “average” star and is one of the 100 BILLION stars that make up the Milky Way galaxy. But by no MEANS does.
24.3 – The Sun. *Interior *Visible Surface/ Photosphere *Atmosphere.
The Sun By: Sam Belanger. What is it? The sun is G2 star Closest star to Earth Contains: hydrogen 70%, 28% helium, metals and other materials 2% Largest.
Our Star The Sun.
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?
© 2010 Pearson Education, Inc. The Sun. © 2010 Pearson Education, Inc. Why was the Sun’s energy source a major mystery?
Our Sun & Nuclear Fusion (Chapter 7). Student Learning Objectives Compare properties of the Earth and Sun Describe the layers of the Sun and how energy.
10.2 Nuclear Fusion 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.
The Sun By: JGilliam The Sun’s CompositionIdentifying Stars Composition ▪ Hydrogen and Helium together make up 99% of the sun’s mass. ▪ 75% of the sun’s.
Solar Spectra: a Lesson on the Sun: Mrs. Pape’s Solar Lesson Bernalillo Middle School Bernalillo, NM © Contact Information: School.
What factors make the Sun a star, not a planet?
MMSA Earth-Space Science The Sun. Energy Output: 4 x Watts If we could 1 second of this energy in its entirety, convert it to electricity and sold.
The Study of Light The Sun. Objectives 0 Explain how the sun produces energy which is transferred to the Earth by radiation. 0 Explain how incoming solar.
The Sun 1)H-R diagram 2)Solar Structure 3)Nuclear Fusion 4)Solar Neutrinos 5)Solar Wind/Sunspots October 21, 2002.
Introduction to The Sun Our sun is a star located at the center of our Solar System. It is a huge, spinning ball of hot gas and nuclear reactions that.
Unit 2 Lesson 3 The Sun Copyright © Houghton Mifflin Harcourt Publishing Company.
The sun By Erin and Madeleine 7J.
Our Sun & Nuclear Fusion
The Sun.
Fusion vs Fission Fission Fusion Division of an atom’s nucleus
The Closest Star- Our Sun
Astronomy-Part 8 Notes Here Comes The Sun
The Sun.
The Sun Our local star.
The source of light, heat and (nearly all) energy on the earth.
Properties of the Sun Visual Vocabulary.
Section 1: Structure of the Sun
The Structure of the Sun
Our Star the Sun Our Star….. the Sun.
Do Now 12/9/09 What is the sun made of???
Our Sun & Nuclear Fusion
Sun Lesson 3.
Our Star The Sun.
Sci. 2-2 The Sun: Our Very Own Star
Presentation transcript:

OUR STAR SOL

GOALS You will have a basic understanding of how a star functions and how they convert matter into energy You will discuss and write down key vocabulary related to the structure and functions within stars

JUST TO RECAP THE STATS WE KNOW… Age: 4.6 Billion years Diameter: 1,391,000 km Mass: x 10^30 kg It’s a star It’s not on fire!!!!!

HISTORY… OR SOMETHING LIKE IT The Sun was revered by many ancient peoples.

EGYPTIANS The sun was revered as Ra. Carried across the sky in a Barque (ship) Accompanied by lesser gods for the daily journey

ANCIENT GREEKS The sun was hailed as Helios. Carried across the sky in a chariot drawn by fiery horses.

ROMANS Celebrated the birthday of the Sun as a holiday called “Sol Invictus,” literally “Unconquered Sun.”

MORE RECENT GREEKS The location of where the sun rose in the sky gave rise to the Zodiac. It was considered a planet

WHAT WE KNOW ABOUT THE SUN It is divided into 4 distinct layers Core Radiative Zone Convective Zone Photosphere Above this is the Atmosphere of the Sun

THE CORE 20-25% of the radius of the Sun 150 x density of water 15.7 million K 99% of the energy in the Sun is produced here

DETAILS OF FUSION Proton-Proton fusion happens 9.7 x 10^37 times each second in the core 6.2 x 10^11 kg /s of Helium is produced each second in this reaction About 1 x10^-13 x the mass of the Earth each second or x10^-19 x the Sun’s mass (slow enough for billions of years worth of fuel)

DETAILS OF THE FUSION CONTINUED… 0.7% of the mass of Helium produced is released as energy This equates to x 10^26 Watts of energy per second x 10^24 80 Watt lightbulbs for 1 second or… One 80 Watt bulb for x 10^17 years

THE RADIATIVE ZONE 25-70% the radius of the Sun Temperature drops to between 7 and 2 million K

DETAILS OF THE RADIATIVE ZONE Temperature gradients within the zone are to high for convection to happen Energy is transferred by photons being emitted and absorbed by atoms

THE CONVECTIVE ZONE From about 70% of the radius of the sun to 200,000 km below its surface Temperatures low enough that atoms are no longer ionized Densities low enough that convection can occur

CONTINUED… Material is heated at the surface of the radiative zone and rises up where its energy is transferred to the photosphere Its temperature drops to 5700 K and then sinks back to the radiative zone to be reheated

PHOTOSPHERE The visible surface of the Sun 10 to 100’s of kilometers thick Observations of this layer resulted in the discovery of Helium

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2025 SlidePlayer.com. Inc. All rights reserved.