Dark Matter: What is it?
|
|
- Nicholas Godwin Washington
- 5 years ago
- Views:
Transcription
1 Dark Matter: What is it? Dark Matter: What is it? Key Concepts 1) Some dark matter consists of MACHOs (MAssive Compact Halo Objects). 2) Some dark matter may consist of WIMPs (Weakly Interacting Massive Particles). 3) The universe contains five times as much dark matter as ordinary luminous matter. Dark matter could also be called invisible matter. The properties of invisible objects are rather difficult to determine. We know dark matter exists because of its gravitational pull on luminous matter; otherwise, information is lacking. Some of the dark matter in galaxy halos consists of Massive Compact Halo Objects (MACHOs, for short). MACHOs can be failed stars ; balls of gas smaller than a star but bigger than Jupiter. Strictly speaking, brown dwarfs are dim matter, not dark matter. A cold brown dwarf (T = 300 K) These failed stars are called brown dwarfs. Brown dwarfs are warm enough to glow feebly at infrared wavelengths. 1
2 MACHOs can be ex-stars ; very dense compact objects that once were stars. These ex-stars can be white dwarfs (dense), neutron stars (denser), or black holes (densest). White Dwarfs Remnants of low-mass stars: M * < 4 M sun Mass < 1.4 M sun Radius ~ 0.01R sun (size of the Earth) White dwarfs are initially bright, but eventually they cool and fade away. Neutron Stars Remnants of massive stars: 8 < M * <18 M sun (??) Mass ~ M sun (???) Radius ~ 10 km (size of a small city) Density ~ g/cc With all reserve, we advance the view that supernovae represent the transition from ordinary stars into neutron stars, which in their final stages consist of extremely closely packed neutrons -F. Zwicky & W. Baade 1930s A sugar-cube of neutron star stuff weighs as much as all of humanity! 2
3 Black Holes Close to a black hole: Gravity is so strong that nothing, not even light, can escape. Infalling matter is shredded by powerful tides and crushed to infinite density. Becomes a Black Hole Black : neither emits nor reflects light Hole : nothing entering can ever escape Seeing what can t be seen Q: If no light gets out of a black hole, how can we ever hope to find one? A: Look for the effects of their gravity on their surroundings: A star orbiting around an unseen massive companion. Less than 20% of the dark matter is MACHOs: Most of the dark matter in galaxy halos consists of exotic matter. Suppose there existed a type of massive elementary particle that didn t absorb, emit, or scatter photons. Particle Physics for Dummies Astronomers Electron: low mass, negative charge Proton: higher mass, positive charge Neutron: proton mass, no charge We d detect such a particle only by its gravitational pull on luminous matter. ordinary exotic Neutrino: VERY low mass, no charge What are Neutrinos? Weakly interacting neutral subatomic particles. Mass-less (or very nearly mass-less). Travel at (or very near) the speed of light. Interact with matter via the weak nuclear force. Can pass through lead 1 parsec thick! Cosmic Gall (John Updike) Neutrinos, they are very small. They have no charge and have no mass And do not interact at all. The earth is just a silly ball To them, through which they simply pass, Like dustmaids down a drafty hall Or photons through a pane of glass. 3
4 Neutrinos: Observed! Neutrinos make up part of the exotic dark matter. Detection of neutrinos is very difficult: Need massive amounts of detector materials. Work deep underground to shield out other radiation. We detect neutrinos from the Sun and from other sources. Although detecting neutrinos is difficult, it has been done! Although we don t know the mass of neutrinos exactly, we know it s tiny Most of the dark matter must be particles other than neutrinos. neutrinos electron One candidate for the position of dark matter : the WIMP. WIMP = Weakly Interacting Massive Particle Neutrinos provide < 10% of the dark matter. According to particle physics theory, WIMPs should be much like neutrinos only more massive. Dark matter is also found on larger scales, in clusters of galaxies. Neutrinos have already been detected: particle physicists are still trying to detect WIMPs. I predict a Nobel Prize for the 1 st to succeed! 4
5 Consider the Coma Cluster of galaxies; in the constellation Coma Berenices, about 100 million parsecs away. The Coma Cluster contains an intracluster medium (ICM) of very hot gas (T > 10 million Kelvin). It contains at least 10,000 galaxies, moving relative to each other at roughly 1000 km/sec. Visible light from stars in galaxies X-ray light from the very hot ICM Mass of stars in the Coma Cluster solar masses Mass of ICM (hot gas) in the Coma Cluster solar masses In the universe, there must be roughly five times as much dark matter as ordinary luminous matter (made from protons, neutrons, and electrons). 1/6 luminous Mass of dark matter in the Coma Cluster solar masses 5/6 dark 5
Cosmologists dedicate a great deal of effort to determine the density of matter in the universe. Type Ia supernovae observations are consistent with
Notes for Cosmology course, fall 2005 Dark Matter Prelude Cosmologists dedicate a great deal of effort to determine the density of matter in the universe Type Ia supernovae observations are consistent
More informationChapter 22 What do we mean by dark matter and dark energy?
Chapter 22 What do we mean by dark matter and dark energy? Unseen Influences Dark Matter: An undetected form of mass that emits little or no light, but whose existence we infer from its gravitational influence
More informationChapter 16 Dark Matter, Dark Energy, & The Fate of the Universe
16.1 Unseen Influences Chapter 16 Dark Matter, Dark Energy, & The Fate of the Universe Dark Matter: An undetected form of mass that emits little or no light but whose existence we infer from its gravitational
More informationDark Matter & Dark Energy. Astronomy 1101
Dark Matter & Dark Energy Astronomy 1101 Key Ideas: Dark Matter Matter we cannot see directly with light Detected only by its gravity (possible future direct detection in the lab) Most of the matter in
More informationChapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves
Chapter 23: Dark Matter, Dark Energy & Future of the Universe Galactic rotation curves Orbital speed as a function of distance from the center: rotation_of_spiral_galaxy.htm Use Kepler s Third Law to get
More informationThe Contents of the Universe (or/ what do we mean by dark matter and dark energy?)
The Contents of the Universe (or/ what do we mean by dark matter and dark energy?) Unseen Influences Dark Matter: An undetected form of mass that emits little or no light but whose existence we infer from
More information3 The lives of galaxies
Discovering Astronomy : Galaxies and Cosmology 24 3 The lives of galaxies In this section, we look at how galaxies formed and evolved, and likewise how the large scale pattern of galaxies formed. But before
More informationStructure of the Milky Way. Structure of the Milky Way. The Milky Way
Key Concepts: Lecture 29: Our first steps into the Galaxy Exploration of the Galaxy: first attempts to measure its structure (Herschel, Shapley). Structure of the Milky Way Initially, star counting was
More informationOur 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.
Our Galaxy 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. Early attempts to locate our solar system produced erroneous results.
More informationDark Matter. About 90% of the mass in the universe is dark matter Initial proposals: MACHOs: massive compact halo objects
1 Dark Matter About 90% of the mass in the universe is dark matter Initial proposals: MACHOs: massive compact halo objects Things like small black holes, planets, other big objects They must be dark (so
More informationReview of Lecture 15 3/17/10. Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath
Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath A2020 Disk Component: stars of all ages, many gas clouds Review of Lecture 15 Spheroidal Component: bulge & halo, old
More informationOur Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye
Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!
More informationToday. Gravitational Lenses 11/19/2013. Astronomy Picture of the Day
ASTR 1020: Stars & Galaxies November 15, 2013 Reading for Monday: Chapter 23, section 23.1-23.3. MasteringAstronomy homework on Galaxy Evolution is due tonight at midnight. Exam 3 is on Wednesday, Nov.
More informationLecture 18 : Black holes. Astronomy 111
Lecture 18 : Black holes Astronomy 111 Gravity's final victory A star more massive than about 18 M sun would leave behind a post-supernova core this is larger than 2-3 M sun :Neutron degeneracy pressure
More informationA100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: Stellar Remnants Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu March 24, 2015 Read: S3, Chap 18 03/24/15 slide 1 Exam #2: March 31 One week from today!
More informationFURTHER COSMOLOGY Book page T H E M A K E U P O F T H E U N I V E R S E
FURTHER COSMOLOGY Book page 675-683 T H E M A K E U P O F T H E U N I V E R S E COSMOLOGICAL PRINCIPLE Is the Universe isotropic or homogeneous? There is no place in the Universe that would be considered
More informationLIFE CYCLE OF A STAR
LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,
More informationLecture 13: The Sun, and how stars work. Astronomy 111 Wednesday October 11, 2017
Lecture 13: The Sun, and how stars work Astronomy 111 Wednesday October 11, 2017 Reminders Star party tomorrow night! Homework #6 due Monday How do stars work? What is a star? What is a star composed of?
More informationChapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter
13.1 Neutron Stars Lecture Outline Chapter 13 Neutron Stars and After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is
More informationChapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.
Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio
More informationChapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.
Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio
More information2) On a Hertzsprung-Russell diagram, where would you find red giant stars? A) upper right B) lower right C) upper left D) lower left
Multiple choice test questions 2, Winter Semester 2015. Based on parts covered after mid term. Essentially on Ch. 12-2.3,13.1-3,14,16.1-2,17,18.1-2,4,19.5. You may use a calculator and the useful formulae
More informationDark matter: summary
Dark matter: summary Gravity and detecting Dark Matter Massive objects, even if they emit no light, exert gravitational forces on other massive objects. m 1 r 12 m 2 We study the motions (dynamics) of
More informationA100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: Stellar Remnants Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu October 28, 2014 Read: S3, Chap 18 10/28/14 slide 1 Exam #2: November 04 One week from today!
More informationNeutron Stars. Chapter 14: Neutron Stars and Black Holes. Neutron Stars. What s holding it up? The Lighthouse Model of Pulsars
Neutron Stars Form from a 8-20 M Sun star Chapter 14: Neutron Stars and Black Holes Leftover 1.4-3 M Sun core after supernova Neutron Stars consist entirely of neutrons (no protons) Neutron Star (tennis
More informationLIFE CYCLE OF A STAR
LIFE CYCLE OF A STAR First stage = Protostar PROTOSTAR Cloud of gas and dust many light-years across Gravity tries to pull the materials together Eventually, at the center of the ball of dust and gas,
More informationNumber of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
More informationBlack Holes. Over the top? Black Holes. Gravity s Final Victory. Einstein s Gravity. Near Black holes escape speed is greater than the speed of light
Black Holes Over the top? What if the remnant core is very massive? M core > 2-3 M sun (original star had M > 18 M sun ) Neutron degeneracy pressure fails. Nothing can stop gravitational collapse. Collapses
More information29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A
29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A There are 20 questions (Note: There will be 32 on the real thing). Read each question and all of the choices before choosing.
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationChapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo
Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1
More informationDark Matter / Dark Energy
Dark Matter / Dark Energy 2 different things! The first hints of Dark Matter arose with observations of large motions in clusters of galaxies in the 1930 s. The case became compelling in the 1970 s with
More informationLecture 23: Black Holes Readings: Sections 24-3, 24-5 through 24-8
Lecture 23: Black Holes Readings: Sections 24-3, 24-5 through 24-8 Key Ideas Black Holes are totally collapsed objects Gravity so strong not even light can escape Predicted by General Relativity Schwarzschild
More informationMoment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
More informationThe 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.
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. Image taken from the European Southern Observatory in Chile
More informationBeyond Our Solar System Chapter 24
Beyond Our Solar System Chapter 24 PROPERTIES OF STARS Distance Measuring a star's distance can be very difficult Stellar parallax Used for measuring distance to a star Apparent shift in a star's position
More informationAstro-2: History of the Universe. Lecture 5; April
Astro-2: History of the Universe Lecture 5; April 23 2013 Previously.. On Astro-2 Galaxies do not live in isolation but in larger structures, called groups, clusters, or superclusters This is called the
More informationEvolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
More informationLecture 14: The Sun and energy transport in stars. Astronomy 111
Lecture 14: The Sun and energy transport in stars Astronomy 111 Energy transport in stars What is a star? What is a star composed of? Why does a star shine? What is the source of a star s energy? Laws
More information11/6/18. Today in Our Galaxy (Chap 19)
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Ryan Horton, Loren Matilsky Lecture 21 Tues 6 Nov 2018 zeus.colorado.edu/astr1040-toomre Edge-on spiral galaxy NGG 4013 Today in Our Galaxy (Chap 19)
More informationFigure 1: The universe in a pie chart [1]
Dark matter Marlene Götz (Jena) Dark matter is a hypothetical form of matter. It has to be postulated to describe phenomenons, which could not be explained by known forms of matter. It has to be assumed
More informationTo infinity, and beyond!
stars The night sky is filled with stars that shine at different levels of brightness. The brightness of the stars we observe can be related to the size of the star or its distance from Earth. In order
More informationLecture Outlines. Chapter 22. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 22 Astronomy Today 8th Edition Chaisson/McMillan Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 Neutron-Star Binaries 22.4 Gamma-Ray
More informationA. Thermal radiation from a massive star cluster. B. Emission lines from hot gas C. 21 cm from hydrogen D. Synchrotron radiation from a black hole
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 26 Thur 14 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre HST Abell 2218 Reading clicker what makes the light? What
More informationEarth Science, 13e Tarbuck & Lutgens
Earth Science, 13e Tarbuck & Lutgens Beyond Our Solar System Earth Science, 13e Chapter 24 Stanley C. Hatfield Southwestern Illinois College Properties of stars Distance Distances to the stars are very
More informationIntroduction to Cosmology Big Bang-Big Crunch-Dark Matter-Dark Energy The Story of Our Universe. Dr. Ugur GUVEN Aerospace Engineer / Space Scientist
Introduction to Cosmology Big Bang-Big Crunch-Dark Matter-Dark Energy The Story of Our Universe Dr. Ugur GUVEN Aerospace Engineer / Space Scientist The Age of the Universe Through various measurements
More informationAccretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants
Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath Review: Creating Stellar Remnants Binaries may be destroyed in white dwarf supernova Binaries be converted into black holes Review: Stellar
More informationThe Dark Side of the Universe: Dark matter in the galaxy and Cosmos
Utah State University DigitalCommons@USU Public Talks Astrophysics 1-18-2011 The Dark Side of the Universe: Dark matter in the galaxy and Cosmos Shane L. Larson Utah State University Follow this and additional
More informationChapter 18 The Bizarre Stellar Graveyard
Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White
More informationReview: HR Diagram. Label A, B, C respectively
Stellar Evolution Review: HR Diagram Label A, B, C respectively A C B a) A: White dwarfs, B: Giants, C: Main sequence b) A: Main sequence, B: Giants, C: White dwarfs c) A: Main sequence, B: White Dwarfs,
More informationA100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy
A100H Exploring the :, Dark Matter, Dark Energy Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 19, 2016 Read: Chaps 20, 21 04/19/16 slide 1 BH in Final Exam: Friday 29 Apr at
More information1. Star: A object made of gas found in outer space that radiates.
1. Star: A object made of gas found in outer space that radiates. 2. Stars produce extremely great quantities of energy through the process of. The chemical formula for nuclear fusion looks like this:
More informationThe Ecology of Stars
The Ecology of Stars We have been considering stars as individuals; what they are doing and what will happen to them Now we want to look at their surroundings And their births 1 Interstellar Matter Space
More informationIB Physics - Astronomy
Solar System Our Solar System has eight planets. The picture below shows their relative sizes, but NOT their relative distances. A planet orbits the sun, and has gravitationally cleared its orbital area
More informationThe Mystery of Dark Matter
The Mystery of Dark Matter Maxim Perelstein, LEPP/Cornell U. CIPT Fall Workshop, Ithaca NY, September 28 2013 Introduction Last Fall workshop focused on physics of the very small - elementary particles
More informationFirst: Some Physics. Tides on the Earth. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath. 1.
Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath First: Some Physics 1. Tides 2. Degeneracy Pressure Concept 1: How does gravity cause tides? R F tides
More informationANSWER KEY. Stars, Galaxies, and the Universe. Telescopes Guided Reading and Study. Characteristics of Stars Guided Reading and Study
Stars, Galaxies, a the Universe Stars, Galaxies, and the Universe Telescopes Use Target Reading Skills Check student definitions for accuracy. 1. Electromagneticradiationisenergythatcan travel through
More informationthe nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes
the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes The spectral lines of stars tell us their approximate composition Remember last year in Physics?
More informationGravity simplest. fusion
Gravity simplest fusion The life of a star has a complex relationship with gravity: 1. Gravity is what brings the original dust together to make a star 2. Gravity wants to crush the star Gravity pulls
More informationRecall what you know about the Big Bang.
What is this? Recall what you know about the Big Bang. Most of the normal matter in the universe is made of what elements? Where do we find most of this normal matter? Interstellar medium (ISM) The universe
More informationCosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE
Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE Cosmology Cosmology is the study of the universe; its nature, origin and evolution. General Relativity is the mathematical basis of cosmology from which
More informationThe Birth Of Stars. How do stars form from the interstellar medium Where does star formation take place How do we induce star formation
Goals: The Birth Of Stars How do stars form from the interstellar medium Where does star formation take place How do we induce star formation Interstellar Medium Gas and dust between stars is the interstellar
More informationClusters and constellations
Astrophysics Clusters and constellations Star clusters are groups of stars that are connected by a significant gravitational force ands move around tougher as the galaxy rotates. The motion of the Sun
More informationLarge Scale Structure
Large Scale Structure Measuring Distance in Universe-- a ladder of steps, building from nearby Redshift distance Redshift = z = (λ observed - λ rest )/ λ rest Every part of a distant spectrum has same
More informationIt is possible for a couple of elliptical galaxies to collide and become a spiral and for two spiral galaxies to collide and form an elliptical.
7/16 Ellipticals: 1. Very little gas and dust an no star formation. 2. Composed of old stars. 3. Masses range from hundreds of thousands to 10's of trillions of solar masses. 4. Sizes range from 3000 ly
More informationHomework #9. Chapter 19 questions are for PRACTICE ONLY they will not factor into your Homework #9 grade, but will help you prepare for Exams #4/#5.
Homework #9 Due Wednesday, April 25, 11:59PM Covers Chapters 18 and 17 Estimated time to complete: 40 minutes Read chapters, review notes before starting Last homework of the semester Chapter 19 questions
More information3/6/12! Astro 358/Spring 2012! Galaxies and the Universe! Dark Matter in Spiral Galaxies. Dark Matter in Galaxies!
3/6/12 Astro 358/Spring 2012 Galaxies and the Universe Dark Matter in Galaxies Figures + Tables for Lectures (Feb 16-Mar 6) Dark Matter in Spiral Galaxies Flat rotation curve of Milky Way at large radii
More informationThe Stars. Chapter 14
The Stars Chapter 14 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star s nuclear fuel is depleted, the star must burn out. Chapter Outline
More informationNotes for Wednesday, July 16; Sample questions start on page 2 7/16/2008
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate
More informationStars and Galaxies 1
Stars and Galaxies 1 Characteristics of Stars 2 Star - body of gases that gives off great amounts of radiant energy as light and heat 3 Most stars look white but are actually different colors Antares -
More informationStars and Galaxies. Evolution of Stars
Stars and Galaxies Evolution of Stars What do you think? Read the two statements below and decide whether you agree or disagree with them. Place an A in the Before column if you agree with the statement
More informationChapter 11 Review. 1) Light from distant stars that must pass through dust arrives bluer than when it left its star. 1)
Chapter 11 Review TRUE/FALSE. Write 'T' if the statement is true and 'F' if the statement is false. 1) Light from distant stars that must pass through dust arrives bluer than when it left its star. 1)
More informationASTR Midterm 1 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 1 Phil Armitage, Bruce Ferguson FIRST MID-TERM EXAM FEBRUARY 16 th 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More informationL = 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?
Fall 2016 Astronomy - Test 3 Test form B Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form B on the answer sheet. Write your name above as well.
More informationL = 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
Fall 2016 Astronomy - Test 3 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as well.
More informationChapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs
Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White
More informationThe Milky Way Galaxy
The Milky Way Galaxy A. Expert - I have done a lot of reading in this area already. B. Above Average - I have learned some information about this topic. C. Moderate - I know a little about this topic.
More informationOur View of the Milky Way. 23. The Milky Way Galaxy
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
More informationPhysics HW Set 3 Spring 2015
1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.
More informationIntroduction and Fundamental Observations
Notes for Cosmology course, fall 2005 Introduction and Fundamental Observations Prelude Cosmology is the study of the universe taken as a whole ruthless simplification necessary (e.g. homogeneity)! Cosmology
More informationTAKE A LOOK 2. Identify This star is in the last stage of its life cycle. What is that stage?
CHAPTER 15 2 SECTION Stars, Galaxies, and the Universe The Life Cycle of Stars BEFORE YOU READ After you read this section, you should be able to answer these questions: How do stars change over time?
More informationAST1100 Lecture Notes
AST1100 Lecture Notes 4 Stellar orbits and dark matter 1 Using Kepler s laws for stars orbiting the center of a galaxy We will now use Kepler s laws of gravitation on much larger scales. We will study
More informationDark Side of the Universe: dark matter in the galaxy and cosmos
Utah State University DigitalCommons@USU Public Talks Astrophysics 8-1-2008 Dark Side of the Universe: dark matter in the galaxy and cosmos Shane L. Larson Utah State University Follow this and additional
More informationHow Do Stars Appear from Earth?
How Do Stars Appear from Earth? Magnitude: the brightness a star appears to have from Earth Apparent Magnitude depends on 2 things: (actual intrinsic brightness) The color of a star is related to its temperature:
More informationThey developed a graph, called the H-R diagram, that relates the temperature of a star to its absolute magnitude.
Ejnar Hertzsprung and Henry Russell noticed that stars with higher temperatures and large sizes also have brighter absolute magnitudes the actual amount of light given off by a star. (also referred to
More informationFinding Black Holes Left Behind by Single Stars
Finding Black Holes Left Behind by Single Stars Finding Black Holes "Yesterday upon the stair I met a man who wasn't there. He wasn't there again today. I wish that man would go away." Hughes Mearns (1875-1965)
More informationSupernovae, Neutron Stars, Pulsars, and Black Holes
Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier
More informationNSCI 314 LIFE IN THE COSMOS
NSCI 314 LIFE IN THE COSMOS 2 BASIC ASTRONOMY, AND STARS AND THEIR EVOLUTION Dr. Karen Kolehmainen Department of Physics CSUSB COURSE WEBPAGE: http://physics.csusb.edu/~karen MOTIONS IN THE SOLAR SYSTEM
More informationA100 Exploring the Universe: Black holes. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: Black holes Martin D. Weinberg UMass Astronomy weinberg@astro.umass.edu October 30, 2014 Read: S2, S3, Chap 18 10/30/14 slide 1 Sizes of s The solar neighborhood visualized!
More informationIntroduction. The Mystery of our universe today, is Dark Matter. Dark Matter is the heart of our
Introduction The Mystery of our universe today, is Dark Matter. Dark Matter is the heart of our galaxy, and it keeps the planets and stars from flying away or moving positions. Dark Matter is the pitch
More informationLecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli
Lecture PowerPoints Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching
More information10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure
10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds
More informationThe Formation of Stars
The Formation of Stars A World of Dust The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky. We are interested
More informationDiscussion Review Test #2. Units 12-19: (1) (2) (3) (4) (5) (6)
Discussion Review Test #2 Units 12-19: (1) (2) (3) (4) (5) (6) (7) (8) (9) Galileo used his observations of the changing phases of Venus to demonstrate that a. the sun moves around the Earth b. the universe
More informationStellar Astronomy Sample Questions for Exam 4
Stellar Astronomy Sample Questions for Exam 4 Chapter 15 1. Emission nebulas emit light because a) they absorb high energy radiation (mostly UV) from nearby bright hot stars and re-emit it in visible wavelengths.
More informationAstronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 22 Neutron Stars and Black Holes MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) In a neutron star, the core
More informationChapter 14 The Milky Way Galaxy
Chapter 14 The Milky Way Galaxy Spiral Galaxy M81 - similar to our Milky Way Galaxy Our Parent Galaxy A galaxy is a giant collection of stellar and interstellar matter held together by gravity Billions
More informationChapter 14: The Bizarre Stellar Graveyard
Lecture Outline Chapter 14: The Bizarre Stellar Graveyard 14.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf?
More informationLec 9: Stellar Evolution and DeathBirth and. Why do stars leave main sequence? What conditions are required for elements. Text
1 Astr 102 Lec 9: Stellar Evolution and DeathBirth and Evolution Why do stars leave main sequence? What conditions are required for elements Text besides Hydrogen to fuse, and why? How do stars die: white
More informationLecture 25: Cosmology: The end of the Universe, Dark Matter, and Dark Energy. Astronomy 111 Wednesday November 29, 2017
Lecture 25: Cosmology: The end of the Universe, Dark Matter, and Dark Energy Astronomy 111 Wednesday November 29, 2017 Reminders Online homework #11 due Monday at 3pm One more lecture after today Monday
More information