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Copyright © 2010 Pearson Education, Inc. Chapter 9 The Sun
Copyright © 2010 Pearson Education, Inc. Chapter 9 The Sun
Copyright © 2010 Pearson Education, Inc. Large Tsunami Shock Wave on the Sun
Copyright © 2010 Pearson Education, Inc. SOHO Solar and Helospheric Observatory Solar and Helospheric Observatory
NSO – New Mexico
Copyright © 2010 Pearson Education, Inc. Units of Chapter 9 The Sun in Bulk The Solar Interior The Solar Atmosphere The Active Sun The Heart of the Sun
Copyright © 2010 Pearson Education, Inc. Question 1 a) core b) corona c) photosphere d) chromosphere e) convection zone The visible light we see from our Sun comes from which part?
Copyright © 2010 Pearson Education, Inc. The Sun in Bulk
Copyright © 2010 Pearson Education, Inc. The Sun in Bulk Interior structure of the Sun Outer layers are not to scale. The core is where nuclear fusion takes place.
Copyright © 2010 Pearson Education, Inc. Question 2 The density of the Sun is most similar to that of a) a comet. b) Jupiter. c) Earth. d) interstellar gas. e) an asteroid.
Copyright © 2010 Pearson Education, Inc. The Sun in Bulk Luminosity – total energy radiated by the Sun – can be calculated from the fraction of that energy that reaches Earth. Total luminosity is about 4 × W – the equivalent of 10 billion 1-megaton nuclear bombs per second.
Copyright © 2010 Pearson Education, Inc. The Solar Interior Mathematical models, consistent with observation and physical principles, provide information about the Sun’s interior. In equilibrium, inward gravitational force must be balanced by outward pressure.
Copyright © 2010 Pearson Education, Inc. Question 3 The Sun is stable as a star because a) gravity balances forces from pressure. b) the rate of fusion equals the rate of fission. c) radiation and convection balance. d) mass is converted into energy. e) fusion doesn’t depend on temperature.
Copyright © 2010 Pearson Education, Inc. The Solar Interior Doppler shifts of solar spectral lines indicate a complex pattern of vibrations.
Copyright © 2010 Pearson Education, Inc. The Solar Interior Solar density and temperature, according to the standard solar model.
Copyright © 2010 Pearson Education, Inc. The Solar Interior Energy transport: The radiation zone is relatively transparent; the cooler convection zone is opaque.
Copyright © 2010 Pearson Education, Inc. The Solar Interior The visible top layer of the convection zone is granulated, with areas of upwelling material surrounded by areas of sinking material. Solar Granulation
Copyright © 2010 Pearson Education, Inc. The Solar Atmosphere Spectral analysis can tell us what elements are present, but only in the chromosphere and photosphere.
Copyright © 2010 Pearson Education, Inc. The Solar Atmosphere The cooler chromosphere is above the photosphere. Difficult to see directly, as photosphere is too bright, unless Moon covers photosphere and not chromosphere during eclipse
Copyright © 2010 Pearson Education, Inc. The Solar Atmosphere Small solar storms in chromosphere emit spicules. Solar Chromosphere
Copyright © 2010 Pearson Education, Inc. The Solar Atmosphere Solar corona can be seen during eclipse if both photosphere and chromosphere are blocked.
Copyright © 2010 Pearson Education, Inc. The Solar Atmosphere Corona is much hotter than layers below it – must have a heat source, probably electromagnetic interactions.
Copyright © 2010 Pearson Education, Inc. The Active Sun SunspotsSunspots appear dark because slightly cooler than surroundings.
Copyright © 2010 Pearson Education, Inc.
The Active Sun Sunspots come and go, typically in a few days. Sunspots are linked by pairs of magnetic field lines.
Copyright © 2010 Pearson Education, Inc. The Active Sun The rotation of the Sun drags magnetic field lines around with it, causing kinks.
Copyright © 2010 Pearson Education, Inc. The Active Sun The Sun has an 11-year sunspot cycle, during which sunspot numbers rise, fall, and then rise again.
Copyright © 2010 Pearson Education, Inc. Question 7 The number of sunspots and solar activity in general peaks a) every 27 days, the apparent rotation period of the Sun’s surface. b) once a year. c) every 5½ years. d) every 11 years. e) approximately every 100 years.
Copyright © 2010 Pearson Education, Inc. The Active Sun This is really a 22-year cycle, because the spots switch polarities between the northern and southern hemispheres every 11 years. Maunder minimum: few, if any, sunspots.
Copyright © 2010 Pearson Education, Inc. The Active Sun Areas around sunspots are active; large eruptions may occur in photosphere. Solar prominence is large sheet of ejected gas.
Copyright © 2010 Pearson Education, Inc. The Active Sun Solar flare Solar flare is a large explosion on Sun’s surface, emitting a similar amount of energy to a prominence, but in seconds or minutes rather than days or weeks.
Copyright © 2010 Pearson Education, Inc. The Active Sun A coronal mass ejection emits charged particles that can affect the Earth.coronal mass ejection
Copyright © 2010 Pearson Education, Inc. Filament/Prominence Eruption
Copyright © 2010 Pearson Education, Inc. The Active Sun Solar wind escapes Sun mostly through coronal holes, which can be seen in X-ray images.
Copyright © 2010 Pearson Education, Inc. The Active Sun Solar corona changes along with sunspot cycle; is much larger and more irregular at sunspot peak.
Copyright © 2010 Pearson Education, Inc. Question 6 What is probably responsible for the increase in temperature of the corona far from the Sun’s surface? a) a higher rate of fusion b) the Sun’s magnetism c) higher radiation pressures d) absorption of X rays e) convection currents
Copyright © 2010 Pearson Education, Inc. The Heart of the Sun Nuclear fusion requires that like-charged nuclei get close enough to each other to fuse. This can happen only if the temperature is extremely high – over 10 million K.
Copyright © 2010 Pearson Education, Inc. The Heart of the Sun The process that powers most stars is a three- step fusion process.
Copyright © 2010 Pearson Education, Inc. Question 4 The proton–proton cycle involves what kind of fusion process? a) carbon (C) into oxygen (O) b) helium (He) into carbon (C) c) hydrogen (H) into helium (He) d) neon (Ne) into silicon (Si) e) oxygen (O) into iron (Fe)
Copyright © 2010 Pearson Education, Inc. The Heart of the Sun Neutrinos are emitted directly from the core of the Sun, and escape, interacting with virtually nothing. Being able to observe these neutrinos would give us a direct picture of what is happening in the core. Unfortunately, they are no more likely to interact with Earth-based detectors than they are with the Sun; the only way to spot them is to have a huge detector volume and to be able to observe single interaction events.
Copyright © 2010 Pearson Education, Inc. Question 8 The solar neutrino problem refers to the fact that astronomers a) cannot explain how the Sun is stable. b) detect only one-third the number of neutrinos expected by theory. c) cannot detect neutrinos easily. d) are unable to explain how neutrinos oscillate between other types. e) cannot create controlled fusion reactions on Earth.
Copyright © 2010 Pearson Education, Inc. Question 5 A neutrino can escape from the solar core within minutes. How long does it take a photon to escape? a) minutes b) hours c) months d) hundreds of years e) about a million years
Copyright © 2010 Pearson Education, Inc. The Heart of the Sun Neutrino observatories Super Kamiokande, Japan Sudbury Neutrino Observatory Canada
Copyright © 2010 Pearson Education, Inc. Summary of Chapter 9 The Sun is held together by its own gravity and powered by nuclear fusion. Outer layers of the Sun: photosphere, chromosphere, corona. The corona is very hot. Mathematical models and helioseismology give us a picture of the interior of the Sun. Sunspots occur in regions of high magnetic fields; darker spots are cooler.
Copyright © 2010 Pearson Education, Inc. Summary of Chapter 9, cont. Nuclear fusion converts hydrogen to helium, releasing energy. Solar neutrinos come directly from the solar core, although observations have told us more about neutrinos than about the Sun.
Objectives Explore the structure of the Sun. The Sun Describe the solar activity cycle and how the Sun affects Earth. Compare the different types of spectra.
The Sun. How Old Is Our Sun? Stars like the Sun shine for nine to ten billion years The Sun is about 4.5 billion years old, judging by the age of moon.
© 2006 Pearson Prentice Hall Lecture Outlines PowerPoint Chapter 23 Earth Science 11e Tarbuck/Lutgens Modified for educational purposes only By S. Koziol.
Exploring the Universe Chapter Energy From the Sun.
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Our Sun – Physical Properties. 109 Earths would fit across the diameter of the sun!! Diameter: 1,400,000 km, 864,000 miles 4.5 light-seconds 1,300,000.
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Chapter 2 Stars and Galaxies. Where are you? The Earth circles the sun The sun is one of billions of billions of stars. To measure distances between stars.
Chapter 29.1 Structure of the Sun Std 1e: Students know the Sun is a typical star and is powered by nuclear reactions, primarily the fusion of hydrogen.
24.1 The Study of Light Visible light from sun is only a small part of whats emitted Electromagnetic waves –Radio waves, IR, light, UV,
Our star, the Sun is a big ball of gas And it's 99 percent of our solar system's mass It's an average star in our Milky Way Warming the Earth every day.
Stars 2 Star Field as seen through the Hubble Space Telescope.
© 2005 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their.
Copyright © by Holt, Rinehart and Winston. All rights reserved. ResourcesChapter menu Table of Contents Section 1 Stars Section 2 The Life Cycle of Stars.
13 Universal Gravitation Everything pulls on everything else.
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The Sun: An Important Star The Suns Affects on the Earth The Sun is the only star in our solar system. It gives the energy needed by all the Earths.
The average distance from Earth to the sun is 1.1 ly 2.1 million km 3.1 million mi. 4.1 billion km 5.1 AU.
THE SOLAR PHOTOSPHERE (contd.) 1. The Suns effective and surface temperature Suns effective temperature is a measure of the Suns radiation coming from.
Objectives Determine the size and shape of the Milky Way, as well as Earths location within it. The Milky Way Galaxy Describe how the Milky Way formed.
Source: HAO's PSPT project These images were taken by the Precision Solar Photometric Telescope at Mauna Loa Solar Observatory in Hawaii. They show how.
Where might we find life in the Solar System? Temperatures of planets.
PHOTOSPHERE The lowest layer of the Suns atmosphere that is also the visible part we see.
Life cycle of stars Nebulae to supernova. Stars and radiation Stars are huge nuclear reactors that give off different forms of radiation (see below) all.
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LECTURE 15, OCTOBER 21, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.
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