Clicker Question: Clicker Question: Clicker Question: Clicker Question: What is the remnant left over from a Type Ia (carbon detonation) supernova:

Similar documents
Chapter 14 The Milky Way Galaxy

The Formation of Stars

Distance Measuring Techniques and The Milky Way Galaxy

The Milky Way & Galaxies

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye

The Milky Way Galaxy

The Milky Way - Chapter 23

Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.

Classifying Stars. Scientists classify stars by: 1. Temperature 2. Brightness

Chapter 23 The Milky Way Galaxy Pearson Education, Inc.

The Universe. is space and everything in it.

Ch. 25 In-Class Notes: Beyond Our Solar System

Accretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants

Beyond Our Solar System Chapter 24

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti

Chapter 15 The Milky Way Galaxy. The Milky Way

Lecture 30. The Galactic Center

View of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?

Physics HW Set 3 Spring 2015

Chapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.

25.2 Stellar Evolution. By studying stars of different ages, astronomers have been able to piece together the evolution of a star.

Lecture Outlines. Chapter 23. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Beyond the Solar System 2006 Oct 17 Page 1 of 5

Life Cycle of a Star - Activities

Our View of the Milky Way. 23. The Milky Way Galaxy

Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION

Chapter 19: Our Galaxy

Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.

Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way. The Curtis View. Our Galaxy. The Shapley View 3/27/18

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.

LIFE CYCLE OF A STAR

The Universe. But first, let s talk about light! 2012 Pearson Education, Inc.

Three Major Components

Stars and Galaxies 1

Chapter 33 The History of a Star. Introduction. Radio telescopes allow us to look into the center of the galaxy. The milky way

Astronomy 114. Lecture 29: Internal Properties of Galaxies. Martin D. Weinberg. UMass/Astronomy Department

A100 Exploring the Universe: The Milky Way as a Galaxy. Martin D. Weinberg UMass Astronomy

The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds.

A100H Exploring the Universe: Discovering Galaxies. Martin D. Weinberg UMass Astronomy

Our Galaxy. Chapter Twenty-Five. Guiding Questions

Stars and Galaxies. Content Outline for Teaching

Earth Science, 13e Tarbuck & Lutgens

Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars

Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE

Our goals for learning: 2014 Pearson Education, Inc. We see our galaxy edge-on. Primary features: disk, bulge, halo, globular clusters All-Sky View

Astro 1050 Fri. Apr. 14, 2017

Stars and their properties: (Chapters 11 and 12)

Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Prentice Hall EARTH SCIENCE

ASTR 200 : Lecture 22 Structure of our Galaxy

The Galaxy. (The Milky Way Galaxy)

Galaxies. CESAR s Booklet

LIFE CYCLE OF A STAR

Today. When does a star leave the main sequence?

Announcement: Quiz Friday, Oct 31

Name Date Period. 10. convection zone 11. radiation zone 12. core

Chapter 20 Stellar Evolution Part 2. Secs. 20.4, 20.5

Stellar Evolution Notes

The Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way

8.8A describe components of the universe, including stars, nebulae, galaxies and use models such as HR diagrams for classification

The Life Cycles of Stars. Dr. Jim Lochner, NASA/GSFC

Ch. 29 The Stars Stellar Evolution

Structure of the Milky Way. Structure of the Milky Way. The Milky Way

Stellar Evolution: Outline

The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.

The Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way

Lecture 29. Our Galaxy: "Milky Way"

Stars, Galaxies & the Universe Lecture Outline

10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure

The Night Sky. The Universe. The Celestial Sphere. Stars. Chapter 14

The Milky Way Galaxy. Some thoughts. How big is it? What does it look like? How did it end up this way? What is it made up of?

AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

L = 4 d 2 B p. 4. Which of the letters at right corresponds roughly to where one would find a red giant star on the Hertzsprung-Russell diagram?

L = 4 d 2 B p. 1. Which outer layer of the Sun has the highest temperature? A) Photosphere B) Corona C) Chromosphere D) Exosphere E) Thermosphere

Study Guide Chapter 2

Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM

Directed Reading A. Section: The Life Cycle of Stars TYPES OF STARS THE LIFE CYCLE OF SUNLIKE STARS A TOOL FOR STUDYING STARS.

Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

The Milky Way Galaxy and Interstellar Medium

Galaxies and Star Systems

Life and Death of a Star 2015

2004 Pearson Education Inc., publishing as Addison-Wesley

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)?

The distance modulus in the presence of absorption is given by

Figure 69.01a. Formation of Stars

Universe Now. 9. Interstellar matter and star clusters

The hazy band of the Milky Way is our wheel-shaped galaxy seen from within, but its size

chapter 31 Stars and Galaxies

Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008

Why Do Stars Leave the Main Sequence? Running out of fuel

Astro 21 first lecture. stars are born but also helps us study how. Density increases in the center of the star. The core does change from hydrogen to

Chapter 30. Galaxies and the Universe. Chapter 30:

Stellar Astronomy Sample Questions for Exam 4

The Milky Way Galaxy. Sun you are here. This is what our Galaxy would look like if we were looking at it from another galaxy.

Astronomy Stars, Galaxies and Cosmology Exam 3. Please PRINT full name

ASTR Midterm 2 Phil Armitage, Bruce Ferguson

A protostar forming in the Orion Nebula. This also has protoplanetary discs, and will probably become a planetary system.

Transcription:

Test 3 results D C Grades posted in cabinet and Grades posted on-line B A F If you are not properly registered then come see me for your grade What is the ultimate origin of the elements heavier than helium that make up your body? (a) They were present when the Universe was created. (b) They were created in low mass (< 8 solar mass) stars (c) They were created in high mass (> 8 solar mass) stars (d) They were created by neutron capture in interstellar space A protostar that will eventually turn into a star like the Sun, is when compared to the Sun: What is the remnant left over from a Type Ia (carbon detonation) supernova: A: larger B: a neutron star + an expanding shell B: fainter C: a black hole + an expanding shell C: hotter D: no remnant, just the expanding shell A: a white dwarf + an expanding shell D: less massive A Type Ia supernova is the: A: explosion of a massive star that has fused elements in its core all they way up to iron. B: explosive burning of hydrogen on the surface of a white dwarf. C: explosion of a white dwarf in a binary star system after mass has been transferred onto it from a companion star. D: Implosion of a blue supergiant to form a black hole. 1

The Milky Way Galaxy Take a Giant Step Outside the Milky Way Artist's Conception Example (not to scale) c b a d Take a Giant Step Outside the Milky Way Artist's Conception Example (not to scale) Perseus arm from above ("face-on") see disk and bulge Orion arm Sun Cygnus arm Carina arm from the side ("edge-on") Another galaxy: NGC 4414. The Milky Way roughly resembles it. M31 2

1. Disk The Three Main Structural Components of the Milky Way - 30,000 pc diameter (or 30 kpc) - contains young and old stars, gas, dust. Has spiral structure - vertical thickness roughly 100 pc - 2 kpc (depending on component. Most gas and dust in thinner layer, most stars in thicker layer) 3. Bulge - About 4 kpc across - old stars, some gas, dust - central black hole of 3 x 10 6 solar masses - spherical 2. Halo - at least 30 kpc across - contains globular clusters, old stars, little gas and dust, much "dark matter" - roughly spherical Shapley (1917) found that Sun was not at center of Milky Way Stellar Orbits Shapley used distances to variable RR Lyrae stars (a kind of Horizontal Branch star) in Globular Clusters to determine that Sun was 16 kpc from center of Milky Way. Modern value 8 kpc. Halo: stars and globular clusters swarm around center of Milky Way. Very elliptical orbits with random orientations. They also cross the disk. Bulge: similar to halo. Disk: rotates. Precise Distance to Galactic Center Distance = 7.94 +/- 0.42 kpc SgrA* Where is our solar system located? A: near the center of the Milky Way Galaxy in the bulge. B: 4 kpc from the center of the Milky Way in the halo. C: 8 kpc from the center of the Milky Way in the disk. D: 20 kpc from the center of the Milky Way in the disk. Eisenhauer et al. 2003 Orbital motion 6.37 mas/yr 3

What lurks at the center of our galaxy? A: A giant star cluster. B: A 30 solar mass black hole. C: A 3 million solar mass black hole. D: Darth Vader Rotation of the Disk Sun moves at 225 km/sec around center. An orbit takes 240 million years. Stars closer to center take less time to orbit. Stars further from center take longer. => rotation not rigid like a phonograph record or a merry-go-round. Rather, "differential rotation". Over most of disk, rotation velocity is roughly constant. The "rotation curve" of the Milky Way Spiral Structure of Disk Spiral arms best traced by: Young stars and clusters Emission Nebulae HI Molecular Clouds (old stars to a lesser extent) Disk not empty between arms, just less material there. Problem: How do spiral arms survive? Given differential rotation, arms should be stretched and smeared out after a few revolutions (Sun has made 20 already): The spiral should end up like this: The Winding Dilemma Real structure of Milky Way (and other spiral galaxies) is more loosely wrapped. 4

Proposed solution: Arms are not material moving together, but mark peak of a compressional wave circling the disk: Traffic-jam analogy: A Spiral Density Wave Traffic jam on a loop caused by merging Now replace cars by stars and gas clouds. The traffic jams are actually due to the stars' collective gravity. The higher gravity of the jams keeps stars in them for longer. Calculations and computer simulations show this situation can be maintained for a long time. 90% of Matter in Milky Way is Dark Matter Gives off no detectable radiation. Evidence is from rotation curve: Molecular gas clouds pushed together in arms too => high density of clouds => high concentration of dust => dust lanes. Also, squeezing of clouds initiates collapse within them => star formation. Bright young massive stars live and die in spiral arms. Emission nebulae mostly in spiral arms. So arms always contain same types of objects, but individual objects come and go. 10 Rotation Velocity (AU/yr) 5 1 Milky Way Rotation Curve Solar System Rotation Curve: when almost all mass at center, velocity decreases with radius ("Keplerian") 1 10 20 30 R (AU) observed curve Curve if Milky Way ended where visible matter pretty much runs out. Not enough radiating matter at large R to explain rotation curve => "dark" matter! Dark matter must be about 90% of the mass! Composition unknown. Probably mostly exotic particles that don't interact with ordinary matter at all (except gravity). Some may be brown dwarfs, dead white dwarfs Most likely it's a dark halo surrounding the Milky Way. Mass of Milky Way How long does it take our solar system to orbit once around the Milky Way? A: 1 year B: 2 million years C: 250 million years D: 250 billion years (longer than the age of the universe) 6 x 10 11 solar masses within 40 kpc of center. 5

Seeing into the center of the Milky Way What makes up most of the mass (90%) of the Milky Way Galaxy? A: hydrogen gas B: stars C: dead stars (white dwarfs, neutron stars, and black holes) D: we don t know Seeing into the center of the Milky Way 6