23. The Milky Way Galaxy The Sun’s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter.

Slides:



Advertisements
Similar presentations
Chapter 15: The Milky Way Galaxy
Advertisements

Chapter 21: The Milky Way. William Herschel’s map of the Milky Way based on star counts In the early 1800’s William Herschel, the man who discovered the.
Our Galaxy `. Interstellar dust obscures our view at visible wavelengths along lines of sight that lie in the plane of the galactic disk.
An early attempt to locate the Sun’s position in the Milky Way was done by William Herschel (who also discovered Uranus) Herschels’ Milky Way Map.
Introduction to Astrophysics Lecture 13: The Milky Way Galaxy.
Galaxies-I. By the 1700’s the old notion that the Earth was the center of the Universe was overthrown by the success of Newton’s theory of universal gravitation,
Slide 1 Andromeda galaxy M31Milky Way galaxy similar to M31.
Chapter 15 The Milky Way Galaxy.
The Milky Way Galaxy Chapter 15. The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint.
Galaxies Galaxies M81. The Milky Way Galaxy.
The Milky Way PHYS390 Astrophysics Professor Lee Carkner Lecture 19.
Chapter 15 The Milky Way Galaxy.
Chapter 23: Our Galaxy Our location in the galaxy Structure of the galaxy Dark matter Spiral arm formation Our own supermassive black hole.
The Mass of the Galaxy We can use the orbital velocity to deduce the mass of the Galaxy (interior to our orbit): v orb 2 =GM/R. This comes out about 10.
The Milky Way Galaxy 19 April 2005 AST 2010: Chapter 24.
Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 23 Our Galaxy CHAPTER 23 Our Galaxy.
9B The Milky Way Our Galactic Home. 9B 9B Goals Structure of our Galaxy. Its size and shape. How do stars and things move through it? Mass and Dark Matter.
The Milky Way Center, Shape Globular cluster system
The Milky Way. Structure of the Milky Way The Milky Way.
Chapter 14 Our Galaxy The Milky Way Revealed Our Goals for Learning What does our galaxy look like? How do stars orbit in our galaxy?
The Milky Way Galaxy Immanuel Kant (1724 – 1804) German philosopher The infinitude of creation is great enough to make a world, or a Milky Way of worlds,
The Milky Way Galaxy. The Milky Way We see a band of faint light running around the entire sky. Galileo discovered it was composed of many stars. With.
The Milky Way Galaxy.
Chapter 15: Chapter 15: The Milky Way Galaxy. Lesson Plan Idea of Gallaxies Idea of Gallaxies Parson’s observations Parson’s observations Hubble’s observations.
Our Galaxy The Milky Way. The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band.
The Milky Way Our Galaxy Please press “1” to test your transmitter.
The Milky Way Galaxy Chapter 12:. The Milky Way Almost everything we see in the night sky belongs to the Milky Way. We see most of the Milky Way as a.
The Milky Way and Other Galaxies Science A-36 12/4/2007.
Chapter 20: Galaxies So far we have talked about “small” things like stars, nebulae and star clusters. Now it’s time to get big!
The Milky Way Galaxy.
The Milky Way Appears as a band of light stretching across the sky There are dark regions along the band, giving the appearance of a lack of stars This.
The Milky Way Galaxy Our home in the Universe. Overview Galaxies = groupings of matter within empty Universe –contain stars, dust, gas –formed in early.
Chapter 23 The Milky Way Galaxy.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Chapter 14 Variable Stars The Milky Way.
Chapter 13 Exploring Our Galaxy
Susan CartwrightOur Evolving Universe1 The Milky Way n From a dark site the Milky Way can be seen as a broad band across the sky l l What is it?   telescopes.
The Nature of Galaxies Chapter 17. Other Galaxies External to Milky Way –established by Edwin Hubble –used Cepheid variables to measure distance M31 (Andromeda.
Galaxies GALAXY -comes from the ancient Greeks and their word for “milk”- galactos.
Chapter 14 The Milky Way Galaxy What do you think? Where in the Milky Way is the solar system located? How fast is the Sun moving in the Milky Way? How.
Discovering the Universe Ninth Edition Discovering the Universe Ninth Edition Neil F. Comins William J. Kaufmann III CHAPTER 15 The Milky Way Galaxy CHAPTER.
Lecture Outlines Astronomy Today 7th Edition Chaisson/McMillan © 2011 Pearson Education, Inc. Chapter 23.
Introduction to Galaxies 5/23/2013. BR: Milky Way Scale The Milky Way has a diameter of approximately 8.25 x 10 9 AU (8.25 billion AU). 206,265 AU = 3.26.
The Milky Way Galaxy. HW #9 – MasteringAstro “Stars and Galaxies” Available now Tuesday April 17 th Due BEFORE CLASS Tuesday April 24 th Observing logs.
1 The Milky Way Galaxy We live on the quiet outskirts of a galaxy of approximately 100 Billion stars. This galaxy, the Milky Way, is roughly disk-shaped.
Lecture 30: The Milky Way. topics: structure of our Galaxy structure of our Galaxy components of our Galaxy (stars and gas) components of our Galaxy (stars.
Chapter 19 Our Galaxy.
What does our galaxy look like?
The Milky Way Galaxy. Sky Maps in Different Bands.
“OUR GALAXY” Definition of a Galaxy: a huge group of individual stars, star clusters, dust, and gas bound together by gravity.
UNIT 1 The Milky Way Galaxy.
Copyright © 2015, W. W. Norton & Company Prepared by Lisa M. Will, San Diego City College Lecture Slides CHAPTER 15: Our Galaxy: The Milky Way Understanding.
Copyright © 2010 Pearson Education, Inc. Clicker Questions Chapter 14 The Milky Way Galaxy.
Our Milky Way Galaxy. The Milky Way Almost everything we see in the night sky belongs to the Milky Way. We see most of the Milky Way as a faint band of.
Copyright © 2010 Pearson Education, Inc. Chapter 14 The Milky Way Galaxy Lecture Outline.
Galaxies: Our Galaxy: the Milky Way. . The Structure of the Milky Way Galactic Plane Galactic Center The actual structure of our Milky Way is very hard.
Universe Tenth Edition
Milky Way: Galactic Structure and Dynamics Milky Way has spiral structure Galactic Bulge surrounds the Center Powerful radio source Sagittarius A at Center.
Our Galaxy Chapter Twenty-Five. Guiding Questions 1.What is our Galaxy? How do astronomers know where we are located within it? 2.What is the shape and.
Nov 19, 2003Astronomy 100 Fall 2003 Next week is Thanksgiving Break. No homework until you get back. On Friday… Exam 2 Grades are posted. Nighttime observing.
ASTR 113 – 003 Spring 2006 Lecture 09 March 29, 2006 Review (Ch4-5): the Foundation Galaxy (Ch 25-27) Cosmology (Ch28-29) Introduction To Modern Astronomy.
7.2 Galaxies pp
The Milky Way Galaxy. What are each of these?
Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.
© 2017 Pearson Education, Inc.
© 2017 Pearson Education, Inc.
The Milky Way Galaxy.
Our Milky Way Galaxy.
Galaxies.
Chapter 15 The Milky Way Galaxy.
Presentation transcript:

23. The Milky Way Galaxy The Sun’s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral arms Infrared & radio galactic nucleus observations

Our View of the Milky Way

The Sun’s Location in Our Galaxy William Herschel’s observations –The Solar System is disk-shaped Faint stars cluster in a band extending in all directions –The Solar System is near the galactic center The number of stars is about the same in all directions William Herschel’s nemesis –Interstellar extinction Interstellar dust obscures more distant stars Dark regions in the Milky Way are obscured, not empty A telltale phenomenon –Globular clusters surround the galactic center Spherical distributions of ~ 10 6 stars –Globular clusters orbit the galactic center Period-luminosity relationship of Cepheid variables

William Herschel’s Milky Way Map

Cepheid Period-Luminosity Relationship

RR Lyrae Light Curves

The Milky Way’s Numbers Disk –Flat disk ~ pcin diameter –Earth is ~ pcfrom the galactic center –Greatest abundance of stars Primarily bright young stars, especially OB associations Abundant new star formation Central bulge –Approximately spherical distribution of stars Primarily dim old stars Little new star formation Halo –Globular clusters Approximately spherical distribution of star clusters

Nonvisible Observations of Our Galaxy Basic physical processes –Selective scattering of EMR Shortvisiblewavelengths are scattered most LongIR & radiowavelengths are scattered least –Development of non-optical telescopes Radiotelescopes Thermal IRtelescopes –NearinfraredWavelengths relativelyclose tothe visible –Far infraredWavelengths relativelyfar fromthe visible Some benefits –Ability to see all of the Milky Way galaxy Central bulge Distribution of interstellar gas clouds

The Infrared Milky Way Far-Infrared View (25 µm, 60 µm, 100 µm) Near-Infrared View (1.2 µm, 2.2 µm, 3.4 µm)

The Milky Way Galaxy Edge-On

The NGC 4565 Galaxy Edge-On

Our Galaxy Has Spiral Arms Observations of other galaxies –Many disk-shaped galaxies have spiral arms Numberof spiral arms varies Distinctnessof spiral arms varies –Tentative conclusion The disk-shaped Milky Way may have spiral arms Observations of the Milky Way galaxy –Neutral hydrogen proton-electron spin-flip transitions Small energy difference between two possible states Produces an emission line at the 21 cm radio wavelength –Neutral hydrogen strongly concentrated in the disk Doppler shift of various nebulae reveals arm structure –Four major spiral arms –The Solar System is in the small Orion arm

Our Galaxy Has Spiral Arms Milky Way rotation

Proton-Electron Spin-Flip in Hydrogen

The Entire Sky at 21 Centimeters

Neutral Hydrogen in the Milky Way

M83 Galaxy at Three Wavelengths VisibleNear-Infrared 21 Centimeter

The Milky Way Galaxy Face-On

The Milky Way’s Dark Matter Basic observations –Stars & nebulae orbit the galactic center Identical to the pattern in the Solar System –Orbital mechanics KeplerianorbitsSpeed decreases with distance –Farthest planets in the Solar System have slowest orbital speeds Non-KeplerianorbitsSpeed is almost constant –Milky Way’s rotation curve is nearly constant –Sun’sspeedaround galactic center is ~ km. hr –1 –Sun’striparound galactic center is ~ yrs Basic conclusion –Most of the Milky Way’s mass is beyond the Sun The visible mass cannot account for this mass Much of the mass beyond the Sun is “dark matter”

Possible Forms of Dark Matter Massive compact halo objectsMACHOs –Very dim stars between 0.01 & 1.0 M Sun –Gravitational bending of light has been observed Tentatively, MACHOs account for < 40% of dark matter Known subatomic particles –Neutrinos, now known to have mass Weakly interacting massive particlesWIMPs –Predicted mathematically but not yet observed Masses 10 to 10,000 times the mass of a neutron

The Milky Way’s Rotation Curve

Microlensing by Halo Dark Matter

Density Waves Produce Spiral Arms The winding dilemma –No spiral galaxies revolve like a solid disk This is not too far from the case Any difference in rotation rate tends to destroy arms –All spiral galaxies have persistent arms Density wavesOne possible explanation –Waves aresimilar to those on ocean surfaces Propagation in slightly different directions Constructive & destructive wave interference –Constructive interference prone to extensive star formation –Destructive interference prone to minimal star formation –Waves arerelatively short-lived Many stars in spiral arms are OB associations –Very massive & short-lived at 3 to 15 million years »Only ~ 5% the rotation period of the Milky Way –Very prone to inducing additional compression & star formation

Problems With the Density Wave Model A driving mechanism to continue density waves –Basic issues A matter of spaceHuge distances are involved A matter of timeHuge time periods are involved –One possibility Barred spirals have asymmetrical gravitational fields –One problem Most spiral galaxies are not barred spirals –Another possibility Tidal influences of neighboring galaxies Types of spiral galaxies –Grand designspiralsClassicspiral forms The density wave model fits these galaxies well –FlocculentspiralsFuzzyspiral forms The density wave model fits these galaxies poorly

Grand-Design & Flocculent Spirals

Infrared & Radio Observations The Milky Way’s nucleus –Extremely crowded with stars One million stars as bright as Sirius As bright as 200 full moons –Dominated bya feature named Sagittarius A Powerful source of synchrotron radiation –Relativistic electrons spiraling in intense magnetic fields –Containsa feature named Sagittarius A* Thought to be the galactic center –Brightest radio source in its vicinity The mysterious identity of Sagittarius A* –Not a starToo energetic –Not a pulsarToo energetic –Not a supernova remnantNot expanding –Maybe a small supermassive black hole ~ 10 6 M Sun

Nucleus of the Milky Way Galaxy

Stars Orbiting the Galactic Center

An historic perspective –William Herschel’s Milky Way map Definite disk shape Same number of stars in all directions –The problem: Interstellar extinction Dust clouds scatter & absorb light –The solution: Globular clusters Cepheid variables give distance A modern perspective –A thin disk~ 50 kpc in diameter Sun~ 8 kpc from center –A central bulge~ 0.6 kpc high –A halo dominated by globular clusters Non-visible telescopic observations –Radio ’s21 cm spin-flip line –InfraredNear- & Far-IR ’s Spiral arms –Confirmed by 21 cm observations –4 major & several minor arms Dark matter – Rotation curve stays nearly constant Much unseen mass lies beyond Sun – Three major possibilities MACHOs Neutrinos & other known particles WIMPs Production of the spiral arms – The density wave model Constructive & destructive interference – Causal mechanism is unclear Asymmetry in barred spirals Tidal effects from nearby galaxies The Milky Way’s nucleus – Viewed in radio & IR ’s – Sagittarius A & Sagittarius A* Small supermassive black hole Important Concepts