Chapter 14 Our Star.

Slides:



Advertisements
Similar presentations
What is the fate of our sun and other stars?
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.
Chapter 11: Our Star © 2015 Pearson Education, Inc.
Copyright © 2012 Pearson Education, Inc. Chapter 10 Our Star 1.
The Sun The Sun is a star. The Sun is a star. It is 4,500 million years old It is 4,500 million years old It takes 8 minutes for its light to reach.
Our Star, the Sun Chapter Eighteen.
ASTR100 (Spring 2008) Introduction to Astronomy Our Star Prof. D.C. Richardson Sections
Copyright © 2012 Pearson Education, Inc. Radius: 6.9  10 8 m (109 times Earth) Mass: 2  kg (300,000 Earths) Luminosity: 3.8  watts Our Star.
Announcements Star Assignment 2, due Monday March 15 –READ chapter 15, do Angel quiz Global Warming Project, due Wednesday March 17 –Sample 4 web sites.
This Set of Slides This set of slides covers our Sun, nuclear processes, solar flares, auroras, and more… Units covered 49, 50, 51.
Chapter 10 Our Star.
The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Luminosity of Sun = 4 x erg/s =
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.
The Sun a medium sized star 93,000,000 miles away 109 times diameter of Earth 1 million Earths could fit in the Sun Made of gas: 82% hydrogen, 17% helium,
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.
Our Sun. Why do we care about the Sun... - Light, heat, life - Space weather solar wind (1,000,000 mph) flares (UV, x-ray radiation) disturb Earth's magnetic.
Lesson 3.3: The Sun.
Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Chapter 10 Our Star.
Chapter 14 Our Star
Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:
Ch. 6: The Sun. Chemical energy? The Sun’s luminosity is about 4x10 26 joules per second. Its mass is about 2x10 30 kg. What is its energy source?
The Sun 24.3 A typical star powered by nuclear reactions Mostly the (fusion of hydrogen to form helium) Which releases energy.
The Sun.
The Sun Chapter 3 Lesson 6 Page 122.
Facts about the sun Sun Cycle Layers of the sun Sun’s Energy Terms Magnetic field $ 200 $ 200$200 $ 200 $ 200 $400 $ 400$400 $ 400$400 $600 $ 600$600.
Information about Midterm #1 Grades are posted on course website Average = 129/180, s.d. = 27 Highest 180/180 Scores below 100 => “serious concerns” Next.
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,
The Sun – Our Local Star Only star in our solar system Consists mostly of Hydrogen Gas Hydrogen turns into helium producing energy that is the source of.
Our Star.
Lecture 19: The Sun Our Star Some Facts about the Sun  distance from Earth: 1.5 x 10 8 km  luminosity: 3.86 x W  mass: 1.98 x kg (3.33.
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.
© 2010 Pearson Education, Inc. Solar Thermostat Decline in core temperature causes fusion rate to drop, so core contracts and heats up. Rise in core temperature.
© 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.
1. Name one part of the sun. 2. Is the sun a solid, liquid or gas? 3. How hot was the center of the sun when it officially became a star?
It can be powered by NUCLEAR ENERGY! Luminosity ~ 10 billion years Nuclear Potential Energy (core) E = mc 2 - Einstein, 1905.
I.The Solar Spectrum : Sun’s composition and surface temperature II.Sun’s Interior: Energy source, energy transport, structure, helioseismology. III.Sun’s.
Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Chapter 10 Our Star.
A ________________ is a huge mass made of very hot gases (____________________ and ____________________) which produces energy through ________ ___________.
Bellwork What two properties effect the force of gravity?
The Sun Chapter 14.2.
© 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?
Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Chapter 10 Our Star.
© 2010 Pearson Education, Inc. The Sun. © 2010 Pearson Education, Inc. Why was the Sun’s energy source a major mystery?
OUR SUN. Solar Nebula: - Cloud of gas and dust that developed into the solar system. - Our Sun was developed as a star from the burning of Hydrogen gas.
Our Star The Sun. Our Star Our Sun is a star that is at the center of our solar system. The Sun is a hot ball of glowing gasses. Deep inside the core,
Sun Notes. Characteristics CLOSEST star to earth CLOSEST star to earth The bright star in the center is Proxima Centauri.
Sun, Moon, Earth, How do they work together to help life survive? our sun.
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.
I.The Solar Spectrum : Sun’s composition and surface temperature II.Sun’s Interior: Energy source, energy transport, structure, helioseismology. III.Sun’s.
Outer Layers of the Sun Photosphere –Limb darkening –Sun spots Chromosphere Corona Prominences, flares, coronal mass ejections Reading
The Sun The SUN Chapter 29 Chapter 29.
© 2010 Pearson Education, Inc. Chapter 8 The Sun and Other Stars.
EARTH SUN (SOL) Radius = 1 Radius = 109 Density =1 Density = Gravity =1 Gravity = 28.0 Temperature ~ 300K Temperature ~ 5,800K.
Chapter 14 Our Star. Why was the Sun’s energy source a major mystery?
© 2017 Pearson Education, Inc.
The Sun.
Chapter 11: Our Star © 2015 Pearson Education, Inc.
(8th) Chapter 14-2 Cornell Notes
The Sun: Our Very Own Star
Chapter 20 Section 2: The Sun
What is the fate of our sun and other stars?
The Sun: Our Star.
The Sun Our local star.
Do Now 12/9/09 What is the sun made of???
Astronomy 04 Astronomy 04 The Solar System Chapter 15:
The Centre of the Solar System Earth Science 11
Chapter 17 The Sun.
The Sun and Other Stars 14-2.
Presentation transcript:

Chapter 14 Our Star

Radius: 6.9 x 108 m (109 times Earth) Mass: 2 x 1030 kg (300,000 Earths) Luminosity: 3.8 x 1026 watts Good Sun movies to download: http://es.rice.edu/ES/humsoc/Galileo/Things/g_sunspots.html Images compiled from Owen Gingerich’s copy of the first edition of Istoria e Dimostrazioni Wave_fade.mpg photosphere:chromosphere:corona, optical:UV:X-ray http://www.lmsal.com/YPOP/FilmFestival/index.html C2_1mth.mpg http://lasco-www.nrl.navy.mil/

What powers the sun? The Sun's energy is produced by the thermonuclear process called hydrogen fusion Small nuclei combine to form larger nuclei

Proton – Proton Reaction The Sun releases energy by fusing four hydrogen nuclei into one helium nucleus. The overall reaction is:

Gravitational contraction: Provided energy that heated core as Sun was forming Contraction stopped when fusion began, which created outward pressure Gravitational equilibrium: Energy provided by fusion maintains the pressure that balances gravity

Solar Thermostat 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

Radiation Zone: Energy transported upward by photons

Convection Zone: Energy transported upward by rising hot gas

Photosphere: Visible surface of Sun ~ 6,000 K

Surface has a speckled or honeycomb appearance called granulation.

Chromosphere: Middle layer of solar atmosphere ~ 104 - 105 K

Corona: Outermost layer of solar atmosphere ~1 million K

How does the energy from fusion get out of the Sun? Energy gradually leaks out of radiation zone in form of randomly bouncing photons. Called the random walk. Can take

Convection (rising hot gas) takes energy to surface

Bright blobs on photosphere are where hot gas is flowing towards the surface. Dark areas are where gases are falling inward.

Solar Activity Solar activity is associated with strong magnetic fields on the sun.

Solar wind - A flow of charged particles from the surface of the Sun

Sunspots Are cooler than other parts of the Sun’s surface (4000 K)

Strong magnetic fields often connect sunspot pairs

Solar flares- bursts of X-rays and charged particles into space Last only a few minutes

Solar prominences eruptions of clouds of hot gases that form huge arches high above the sun’s surface. May last for several weeks to months.

Rare, solar tornado

Corona appears bright in X-ray photos in places where magnetic fields trap hot gas Wave_fade.mpg photosphere:chromosphere:corona, optical:UV:X-ray http://www.lmsal.com/YPOP/FilmFestival/index.html

Coronal mass ejections send bursts of energetic charged particles out through the solar system

Number of sunspots rises and falls in 11-year cycle

Sunspot cycle has something to do with winding and twisting of Sun’s magnetic field

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

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