Star Formation. Interstellar Medium (ISM): Gas & dust between stars. ( atoms/cm 3 ) Composition
|
|
- August Jonathan Whitehead
- 7 years ago
- Views:
Transcription
1 Star Formation Interstellar Medium (ISM): Gas & dust between stars ( atoms/cm 3 ) Composition Gas: 70% H (neutral H, H +, H 2 ) 22 25% He 3 5% metals Dust: Silicate grains (rock/sand) Graphite (Carbon) Basic organic material
2 Star Formation Nebula (Large cloud of ISM) - low density (200 atoms/cm3) - T ~ 20 K - D ~ 150 L.Y. - M ~ MSuns Great Orion Nebula
3 Gravity causes: - globule contraction - material accumulation - central region to heat up Rotation causes: - Densest region to become spherical (proto-star) - Outer gases cast off into proto-planetary disk
4 Star Formation A protostar s mass will determine the star s: - temperature (Spectral Class) Position on - luminosity (Absolute Magnitude) Main Sequence - length of protostar stage (in fact, all stages) A star s evolution depends on how massive it is: Low Mass (0.08 M Suns < M < 2 M Suns ) Intermediate Mass (2 M Suns < M < 8 M Suns ) High Mass (M > 8 M Suns ) We ll trace Sun s evolution then compare more massive stars to it
5 Star Formation HR Diagram is used to map out each star s evolutionary cycle. 1. Cool protostar collapses under gravity 2. Pressure inside builds up which increases temperature 3. Gas pressure increases, but gravity is too strong; collapse continues 4. Once T core ~ 15 million K, H He fusion reactions start in core
6 Stage 1: Protostar
7 Protostar Protostar s mass determines R, T, L, & formation time. Higher mass more gravity larger in size hotter more luminous quicker formation Vice versa for lower mass stars Upper: 120 M Sun P rad too great Lower: 0.08 M Sun too cool for H-fusion to begin (Brown Dwarf)
8 Stage 2: Main Sequence A STAR IS BORN!!! (Once fusion reactions in the core begin & the star stabilizes) Hydrostatic Equilibrium: Inward Gravity = Outward Pressure
9 Main Sequence Longest stage (90%) of star s life Core Hydrogen gradually replaced with Helium (Presently the is Sun s core is 35% H, 64% He)
10 Main Sequence Following Relations Hold True for MS Stars Size: R = M Luminosity: L = M Lifespan: t = 1 M 2 Answers to each property are given in solar units
11 Main Sequence Exercise: Find R, L, & t for a star with a mass of 4 M Suns R L Sun Sun = = 6.96 x x m W T Sun t Sun = 5800 K = years R L Life Solar Units 2 R Sun 128 L Sun 1/16 t Sun Physical Units x 10 9 m 4.90 x W 6.25 x 10 8 years
12 Solar Structure
13 Solar Structure We cannot see beneath the surface, but we create a model based on computer simulations & physical equations
14 Solar Core Diameter = 280,000 km (0.2 D Sun ) Density = 160 g/cm 3 T core = 15 million Kelvin Temperature is high enough to: Create a fully ionized plasma Generate energy through nuclear fusion
15 Nuclear Fusion
16 Nuclear Fusion 4 H 1 He (+ 2 e + + 2ν + 2γ) Mass of 4 H nuclei > mass of 1 He nucleus Difference in mass is converted into energy. Δ m energy according to E = mc 2 Astronomers estimate that the Sun will run out of core Hydrogen core Hydrogen in a little under 10 Billion years.
17 Radiation Zone (350,000 km region that surrounds core) Energy is transported by absorption/emission of photons by atoms: photons are emitted in random directions Radiation Zone Core Atoms How long does it take the average photon to make it out of the Sun? ~ 1 Million Years!!!
18 Convection Zone energy is transported mostly through convection currents (210,000 km above radiation zone) Hot gas (bright) rises and heats surroundings; cool gas (dark) sinks Photospheric Granulation
19 Photosphere marks the Sun s outer boundary (500 km) photons emitted into space ( light sphere ) Solar spectrum made from gases here
20 Chromosphere Gaseous region (2300 km) above photosphere Appears red, due to strong Hα emission Can only view using proper filter (Hα) or during a Solar Eclipse Note: Helium was first observed in here
21 Corona Large (10 6 km), hot (10 6 K) region of diffuse gas surrounding Sun Heated to such high temperatures by the Sun s magnetic field Visible during a total solar eclipse or with use of coronagraph
22 Solar Wind Continual stream of high energy ions and electrons that travel through interplanetary space at speeds of ~ 300 km/s. Earth s magnetic field deflects the solar wind
23 Sunspots Sunspots: large, dark areas that appear on the photosphere Central dark region (umbra) surrounded by flowing gases (penumbra) D ~ 10,000 50,000 km; T ~ K Spectrum of sunspot indicates magnetic influence
24 Solar Dynamo Differential rotation causes magnetic field to wrap around Sun, forming kinks that penetrate the photosphere
25 Solar Cycle Continual wrapping more kinks more activity Once max. occurs, magnetic field re-stabilizes (with magnetic poles reversed) and the cycle begins again.
26 Solar Activity Solar Flares violent eruptions of solar material (10 6 H-bombs)
27 Coronal Mass Ejection High energy explosions (10 12 H-bombs) resulting from coronal gas getting trapped within tangled magnetic kinks
28 Coronal Mass Ejections If directed toward Earth, they can: - Cause power outages - Disrupt satellite function - Harm astronauts - Destroy atmosphere/ozone?
29 Main Sequence Interior structure differs by mass Fusion process differs as well; - low mass: proton-proton chain - high mass: CNO cycle
30 Post-Main Sequence (Low Mass Stars) Once the core Hydrogen supply runs out: - Inert Helium core left behind starts to contract - H-burning shell surrounds the core - Excess heat causes the star to expand (Subgiant)
31 Post-Main Sequence (Low Mass Stars) Simultaneously, the star expands and cools while the He core contracts and heats up Once T core ~ 10 8 K, He C fusion begins The star now stabilizes as a Red Giant
32 Stage 3: Red Giant Helium (in core) begins to fuse into Carbon (basic element of life) (H-burning shell adds more He to core) Triple-α Process Size grows to ~ R = 2x 10 8 km Stellar winds increase
33 Red Giant Once the core Helium supply runs out: - Inert Carbon core is left behind and starts to contract - Helium just above core fuses into Carbon (He-burning shell) (H-burning shell remains above) - Excess heat causes the star to expand (2 nd Red Giant stage)
34 2nd Red Giant Stage Low mass stars won t get hot enough to start fusing Carbon
35 Post-Main Sequence (Intermediate/High Mass Stars) Same process occurs for higher mass stars when core Hydrogen runs out but the stars become Supergiants (Stage 3) Carbon fuses into heavier elements
36 Supergiants Multiple layers of fusion shells form around the core Iron (Fe) is the last element to be created inside stellar cores Supergiants can become highly unstable due to imbalance between Inward Gravity & Outward Pressure
37 Pulsating Variable Stars Stars found in the Instability Strip of the HR Diagram experience a cyclic change in size & temperature changes in luminosity. Period-Luminosity Relationship (used as a way to determine distance)
Solar Nebula Theory. Basic properties of the Solar System that need to be explained:
Solar Nebula Theory Basic properties of the Solar System that need to be explained: 1. All planets orbit the Sun in the same direction as the Sun s rotation 2. All planetary orbits are confined to the
More information7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.
1. Most interstellar matter is too cold to be observed optically. Its radiation can be detected in which part of the electromagnetic spectrum? A. gamma ray B. ultraviolet C. infrared D. X ray 2. The space
More informationStellar Evolution. The Basic Scheme
Stellar Evolution The Basic Scheme Stars live for a very long time compared to human lifetimes. Even though stellar life-spans are enormous, we know how stars are born, live, and die. All stars follow
More informationStellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
More informationWHERE DID ALL THE ELEMENTS COME FROM??
WHERE DID ALL THE ELEMENTS COME FROM?? In the very beginning, both space and time were created in the Big Bang. It happened 13.7 billion years ago. Afterwards, the universe was a very hot, expanding soup
More informationSolar Energy Production
Solar Energy Production We re now ready to address the very important question: What makes the Sun shine? Why is this such an important topic in astronomy? As humans, we see in the visible part of the
More informationUNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
More informationNuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
More informationMain sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya
Main sequence stars Haris Ðapo 1 Akdeniz University, Antalya Antalya Lecture 3. Haris Ðapo (Akdeniz University) Main sequence stars Main sequence stars 1 / 22 Outline 1 Introduction 2 Hydrogen burning
More informationBe Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
More informationSTUDY GUIDE: Earth Sun Moon
The Universe is thought to consist of trillions of galaxies. Our galaxy, the Milky Way, has billions of stars. One of those stars is our Sun. Our solar system consists of the Sun at the center, and all
More informationMultiple Choice Identify the choice that best completes the statement or answers the question.
Test 2 f14 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Carbon cycles through the Earth system. During photosynthesis, carbon is a. released from wood
More informationSolar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
More informationLecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
More informationThe Sun: Our nearest star
The Sun: Our nearest star Property Surface T Central T Luminosity Mass Lifetime (ms) Value 5500K 15x10 6 K 2 x 10 33 ergs 4 x 10 33 grams 10 billion years Solar Structure Build a model and find the central
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationAy 20 - Lecture 9 Post-Main Sequence Stellar Evolution. This file has many figures missing, in order to keep it a reasonable size.
Ay 20 - Lecture 9 Post-Main Sequence Stellar Evolution This file has many figures missing, in order to keep it a reasonable size. Main Sequence and the Range of Stellar Masses MS is defined as the locus
More informationThe Sun and Solar Energy
I The Sun and Solar Energy One of the most important forces behind global change on Earth is over 90 million miles distant from the planet. The Sun is the ultimate, original source of the energy that drives
More information8. The evolution of stars a more detailed picture
8. The evolution of stars a more detailed picture 8.1Pre Main-Sequence Evolution Evolution onto the main sequence begins with a cloud of cold gas which contracts under self-gravity. Potential Energy is
More informationWELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
More informationTHE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk
THE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk 1.INTRODUCTION Late in the nineteenth century, astronomers had tools that revealed a great deal about stars. By that time, advances in telescope
More informationScience Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
More informationTest 2 --- Natural Sciences 102, Professors Rieke --- VERSION B March 3, 2010
Enter your answers on the form provided. Be sure to write your name and student ID number on the first blank at the bottom of the form. Please mark the version (B) in the Key ID space at the top of the
More informationIntroduction to Astronomy. Lecture 4: Our star, the Sun
Introduction to Astronomy Lecture 4: Our star, the Sun 1 Sun Facts Age = 4.6 x 10 9 years Mean Radius = 7.0x10 5 km = 1.1x10 2 R = 1R Volume = 1.4x10 18 km 3 = 1.3x10 6 R = 1V Mass = 2x10 30 kg = 3.3x10
More informationThe Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
More information1 Introduction. Name: 1.1 Spectral Classification of Stars. PHYS-1050 Hertzsprung-Russell Diagram Solutions Spring 2013
Name: 1 Introduction Read through this information before proceeding on with the lab. 1.1 Spectral Classification of Stars 1.1.1 Types of Spectra Astronomers are very interested in spectra graphs of intensity
More informationThe Main Point. Lecture #34: Solar System Origin II. Chemical Condensation ( Lewis ) Model. How did the solar system form? Reading: Chapter 8.
Lecture #34: Solar System Origin II How did the solar system form? Chemical Condensation ("Lewis") Model. Formation of the Terrestrial Planets. Formation of the Giant Planets. Planetary Evolution. Reading:
More informationStructure and Properties of Atoms
PS-2.1 Compare the subatomic particles (protons, neutrons, electrons) of an atom with regard to mass, location, and charge, and explain how these particles affect the properties of an atom (including identity,
More informationClass 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationLecture 10 Formation of the Solar System January 6c, 2014
1 Lecture 10 Formation of the Solar System January 6c, 2014 2 Orbits of the Planets 3 Clues for the Formation of the SS All planets orbit in roughly the same plane about the Sun. All planets orbit in the
More informationHigh resolution images obtained with Solar Optical Telescope on Hinode. SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ)
High resolution images obtained with Solar Optical Telescope on Hinode SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ) Temperature stratification of solar atmosphere G-band Ca
More informationA i A i. µ(ion) = Z i X i
Lecture 2 Review: calculation of mean atomic weight of an ionized gas (µ) Given a mass fraction X i (or abundance) for an ionic (or atomic) species with atomic weight A i, we can can calculate µ by: For
More informationUsing Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
More information8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
More informationThe Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
More informationCalifornia Standards Grades 9 12 Boardworks 2009 Science Contents Standards Mapping
California Standards Grades 912 Boardworks 2009 Science Contents Standards Mapping Earth Sciences Earth s Place in the Universe 1. Astronomy and planetary exploration reveal the solar system s structure,
More informationHomework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How
More informationOrigins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
More information4 HOW OUR SOLAR SYSTEM FORMED 750L
4 HOW OUR SOLAR SYSTEM FORMED 750L HOW OUR SOLAR SYSTEM FORMED A CLOSE LOOK AT THE PLANETS ORBITING OUR SUN By Cynthia Stokes Brown, adapted by Newsela Planets come from the clouds of gas and dust that
More informationThe sun and the solar corona
The sun and the solar corona Introduction The Sun of our solar system is a typical star of intermediate size and luminosity. Its radius is about 696000 km, and it rotates with a period that increases with
More informationCosmic Journey: Teacher Packet
Cosmic Journey: Teacher Packet Compiled by: Morehead State University Star Theatre with help from Bethany DeMoss Table of Contents Table of Contents 1 Corresponding Standards 2 Vocabulary 4 Sizing up the
More informationThe Layout of the Solar System
The Layout of the Solar System Planets fall into two main categories Terrestrial (i.e. Earth-like) Jovian (i.e. Jupiter-like or gaseous) [~5000 kg/m 3 ] [~1300 kg/m 3 ] What is density? Average density
More informationLecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
More informationSummary: Four Major Features of our Solar System
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
More informationChapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
More informationChapter 6 Formation of Planetary Systems Our Solar System and Beyond
Chapter 6 Formation of Planetary Systems Our Solar System and Beyond The solar system exhibits clear patterns of composition and motion. Sun Over 99.9% of solar system s mass Made mostly of H/He gas (plasma)
More informationFXA 2008. UNIT G485 Module 5 5.5.1 Structure of the Universe. Δλ = v λ c CONTENTS OF THE UNIVERSE. Candidates should be able to :
1 Candidates should be able to : CONTENTS OF THE UNIVERSE Describe the principal contents of the universe, including stars, galaxies and radiation. Describe the solar system in terms of the Sun, planets,
More informationHeating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
More information1 A Solar System Is Born
CHAPTER 3 1 A Solar System Is Born SECTION Formation of the Solar System BEFORE YOU READ After you read this section, you should be able to answer these questions: What is a nebula? How did our solar system
More informationHoward Eskildsen often uploads some of his wonderful and exquisite solar
Solar Images Taken with Calcium K-Line Filters Howard L. Cohen January 2014 (Rev. March 2015) Howard Eskildsen s beautiful images of the Sun uploaded to the AAC website may appear strange and unfamiliar
More informationStudy Guide due Friday, 1/29
NAME: Astronomy Study Guide asteroid chromosphere comet corona ellipse Galilean moons VOCABULARY WORDS TO KNOW geocentric system meteor gravity meteorite greenhouse effect meteoroid heliocentric system
More informationDE2410: Learning Objectives. SOLAR SYSTEM Formation, Evolution and Death. Solar System: To Size Scale. Learning Objectives : This Lecture
DE2410: Learning Objectives SOLAR SYSTEM Formation, Evolution and Death To become aware of our planet, solar system, and the Universe To know about how these objects and structures were formed, are evolving
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT THE HERTZSPRUNG RUSSELL DIAGRAM
PROJECT 4 THE HERTZSPRUNG RUSSELL DIGRM Objective: The aim is to measure accurately the B and V magnitudes of several stars in the cluster, and plot them on a Colour Magnitude Diagram. The students will
More informationL3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
More informationUnit 8 Lesson 2 Gravity and the Solar System
Unit 8 Lesson 2 Gravity and the Solar System Gravity What is gravity? Gravity is a force of attraction between objects that is due to their masses and the distances between them. Every object in the universe
More informationAstro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
More informationReview 1. Multiple Choice Identify the choice that best completes the statement or answers the question.
Review 1 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. When hydrogen nuclei fuse into helium nuclei a. the nuclei die. c. particles collide. b. energy
More informationChapter 8 Formation of the Solar System. What theory best explains the features of our solar system? Close Encounter Hypothesis
Chapter 8 Formation of the Solar System What properties of our solar system must a formation theory explain? 1. Patterns of motion of the large bodies Orbit in same direction and plane 2. Existence of
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More informationWeek 1-2: Overview of the Universe & the View from the Earth
Week 1-2: Overview of the Universe & the View from the Earth Hassen M. Yesuf (hyesuf@ucsc.edu) September 29, 2011 1 Lecture summary Protein molecules, the building blocks of a living organism, are made
More informationTHE SOLAR SYSTEM - EXERCISES 1
THE SOLAR SYSTEM - EXERCISES 1 THE SUN AND THE SOLAR SYSTEM Name the planets in their order from the sun. 1 2 3 4 5 6 7 8 The asteroid belt is between and Which planet has the most moons? About how many?
More informationThe Earth, Sun, and Moon
reflect The Sun and Moon are Earth s constant companions. We bask in the Sun s heat and light. It provides Earth s energy, and life could not exist without it. We rely on the Moon to light dark nights.
More informationStudy Guide: Solar System
Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.
More informationIntroduction and Origin of the Earth
Page 1 of 5 EENS 1110 Tulane University Physical Geology Prof. Stephen A. Nelson Introduction and Origin of the Earth This page last updated on 30-Jul-2015 Geology, What is it? Geology is the study of
More informationENERGY TRANSPORT WITHIN A STAR
M. Pettini: Structure and Evolution of Stars Lecture 8 ENERGY TRANSPORT WITHIN A STAR 8.1 Introduction Up to now, we have considered how energy is generated within the interior of stars by the processes
More informationIV. Molecular Clouds. 1. Molecular Cloud Spectra
IV. Molecular Clouds Dark structures in the ISM emit molecular lines. Dense gas cools, Metals combine to form molecules, Molecular clouds form. 1. Molecular Cloud Spectra 1 Molecular Lines emerge in absorption:
More information4 HOW OUR SOLAR SYSTEM FORMED 1020L
4 HOW OUR SOLAR SYSTEM FORMED 1020L HOW OUR SOLAR SYSTEM FORMED A CLOSE LOOK AT THE PLANETS ORBITING OUR SUN By Cynthia Stokes Brown, adapted by Newsela Planets are born from the clouds of gas and dust
More informationSolar System Formation
Solar System Formation Solar System Formation Question: How did our solar system and other planetary systems form? Comparative planetology has helped us understand Compare the differences and similarities
More informationAy 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable
Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater
More informationFrancesco Piacentini. Title. Page 1
Page 1 Page 2 Layers core -- nuclear burning central part of the Sun radiative zone -- the layer below convection zone where energy is transported by photons convection zone -- layer of the Sun just below
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationLesson Plan G2 The Stars
Lesson Plan G2 The Stars Introduction We see the stars as tiny points of light in the sky. They may all look the same but they are not. They range in size, color, temperature, power, and life spans. In
More informationName Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
More informationSolar Wind: Theory. Parker s solar wind theory
Solar Wind: Theory The supersonic outflow of electrically charged particles, mainly electrons and protons from the solar CORONA, is called the SOLAR WIND. The solar wind was described theoretically by
More information4 HOW OUR SOLAR SYSTEM FORMED 890L
4 HOW OUR SOLAR SYSTEM FORMED 890L HOW OUR SOLAR SYSTEM FORMED A CLOSE LOOK AT THE PLANETS ORBITING OUR SUN By Cynthia Stokes Brown, adapted by Newsela Planets are born from the clouds of gas and dust
More informationHR Diagram Student Guide
Name: HR Diagram Student Guide Background Information Work through the background sections on Spectral Classification, Luminosity, and the Hertzsprung-Russell Diagram. Then complete the following questions
More informationThe Expanding Universe
Stars, Galaxies, Guided Reading and Study This section explains how astronomers think the universe and the solar system formed. Use Target Reading Skills As you read about the evidence that supports the
More informationThe spectacular eruption of a volcano, the magnificent scenery of a
Section 1.1 1.1 What Is Earth Science 1 FOCUS Section Objectives 1.1 Define Earth science. 1.2 Describe the formation of Earth and the solar system. Build Vocabulary Word Parts Ask students to use a dictionary
More informationThe Solar System - II
The Solar System - II Alexei Gilchrist [The Story of the Solar System] Some resources o o o Section 13.3 of Voyages (references and links at end) References noted in these slides The Story of the Solar
More information1.1 A Modern View of the Universe" Our goals for learning: What is our place in the universe?"
Chapter 1 Our Place in the Universe 1.1 A Modern View of the Universe What is our place in the universe? What is our place in the universe? How did we come to be? How can we know what the universe was
More informationThe atmospheres of different planets
The atmospheres of different planets Thomas Baron October 13, 2006 1 Contents 1 Introduction 3 2 The atmosphere of the Earth 3 2.1 Description and Composition.................... 3 2.2 Discussion...............................
More informationAtomic Structure: Chapter Problems
Atomic Structure: Chapter Problems Bohr Model Class Work 1. Describe the nuclear model of the atom. 2. Explain the problems with the nuclear model of the atom. 3. According to Niels Bohr, what does n stand
More informationDESCRIPTION ACADEMIC STANDARDS INSTRUCTIONAL GOALS VOCABULARY BEFORE SHOWING. Subject Area: Science
DESCRIPTION Host Tom Selleck conducts a stellar tour of Jupiter, Saturn, Uranus, Neptune, and Pluto--the outer planets of Earth's solar system. Information from the Voyager space probes plus computer models
More informationNOTES: GEORGIA HIGH SCHOOL SCIENCE TEST THE SOLAR SYSTEM
NOTES: GEORGIA HIGH SCHOOL SCIENCE TEST THE SOLAR SYSTEM 1.What is a Solar system? A solar system consists of: * one central star, the Sun and * nine planets: Mercury, Venus, Earth, Mars, Jupiter, Saturn,
More information5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
More informationObjectives 404 CHAPTER 9 RADIATION
Objectives Explain the difference between isotopes of the same element. Describe the force that holds nucleons together. Explain the relationship between mass and energy according to Einstein s theory
More informationSolar Activity and Earth's Climate
Rasmus E. Benestad Solar Activity and Earth's Climate Second Edition Published in association with Springer Praxis ids Publishing Publisl PRAXI Chichester, UK Contents Preface to the second edition Preface
More informationPhotons. ConcepTest 27.1. 1) red light 2) yellow light 3) green light 4) blue light 5) all have the same energy. Which has more energy, a photon of:
ConcepTest 27.1 Photons Which has more energy, a photon of: 1) red light 2) yellow light 3) green light 4) blue light 5) all have the same energy 400 nm 500 nm 600 nm 700 nm ConcepTest 27.1 Photons Which
More informationThe Universe. The Solar system, Stars and Galaxies
The Universe The Universe is everything. All us, the room, the U.S. the earth, the solar system, all the other stars in the Milky way galaxy, all the other galaxies... everything. How big and how old is
More information13 Space Photos To Remind You The Universe Is Incredible
13 Space Photos To Remind You The Universe Is Incredible NASA / Via photojournal.jpl.nasa.gov New ultraviolet images from NASA s Galaxy Evolution Explorer shows a speeding star that is leaving an enormous
More informationSpectral Classification of Stars
Department of Physics and Geology Astronomy 1402 Spectral Classification of Stars The purpose of this laboratory activity is to introduce you to stellar spectral classification. You will have an opportunity
More information3 HOW WERE STARS FORMED?
3 HOW WERE STARS FORMED? David Christian explains how the first stars were formed. This two-part lecture begins by focusing on what the Universe was like in its first 200 million years of existence, a
More informationastronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.
1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were increased,
More informationName: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
More informationPLAGIARISM. Types of Plagiarism considered here: Type I: Copy & Paste Type II: Word Switch Type III: Style Type IV: Metaphor Type V Idea
SPECIAL THANKS TO DR. CECILIA BAMBAUM, WHO HAS GRACIOUSLY AGREED TO ALLOW US TO POST THIS DOCUMENT IT WILL BE USED BY SEVERAL TEACHERS DURING THE YEAR TO HELP EXPLAIN PLAGIARISM IN ALL ITS FORMS TO FIRESIDE
More informationChemical Building Blocks: Chapter 3: Elements and Periodic Table
Name: Class: Date: Chemical Building Blocks: Chapter 3: Elements and Periodic Table Study Guide Multiple Choice Identify the letter of the choice that best completes the statement or answers the question.
More informationEDUCATOR S GUIDE. amnh.org/education/stars INSIDE:
EDUCATOR S GUIDE amnh.org/education/stars INSIDE: Suggestions to Help You Come Prepared Essential Questions for Student Inquiry Strategies for Teaching with the Show Online Resources Correlations to Standards
More informationExplain the Big Bang Theory and give two pieces of evidence which support it.
Name: Key OBJECTIVES Correctly define: asteroid, celestial object, comet, constellation, Doppler effect, eccentricity, eclipse, ellipse, focus, Foucault Pendulum, galaxy, geocentric model, heliocentric
More informationCoronal Heating Problem
Mani Chandra Arnab Dhabal Raziman T V PHY690C Course Project Indian Institute of Technology Kanpur Outline 1 2 3 Source of the energy Mechanism of energy dissipation Proposed mechanisms Regions of the
More informationChapter 8 Welcome to the Solar System
Chapter 8 Welcome to the Solar System 8.1 The Search for Origins What properties of our solar system must a formation theory explain? What theory best explains the features of our solar system? What properties
More information