Lecture 24: Cosmology: The First Three Minutes. Astronomy 111 Monday November 27, 2017
|
|
- Ashlie Booth
- 5 years ago
- Views:
Transcription
1 Lecture 24: Cosmology: The First Three Minutes Astronomy 111 Monday November 27, 2017
2 Reminders Last star party of the semester tomorrow night! Online homework #11 due Monday at 3pm
3 The first three minutes The First Three Minutes: A Modern View of the Origin of the Universe by Steven Weinberg
4 The Big Bang s hot past Today: Universe is low-density and very cold (2.7 K) Steadily expanding ~15 Gyr Ago: Universe was smaller, denser, & hotter Expanding at a somewhat faster rate How far back can we go?
5 Early (expanding) Universe Average temperature decreases with expansion.
6 Loosing & binding Binding Energy: Energy needed to unbind (break up) matter. Binding Temperature: Temperature equivalent to the binding energy. Matter at this temperature melts (unbinds) Example: In massive stars, nuclei melt at T~10 Billion K.
7 Typical sizes & binding energies Binding Size Energy Atoms 10 m 10 3 K Nuclei 10 m K p & n 10 m K Quarks 10 m K
8 Fundamental forces of nature Gravitation: Long-Range Electromagnetic Force: Long-Range, stronger than gravity Weak Force: Range <10 7 meters, 10 2 gravity Strong Force: Range <10 meters, 10 gravity
9 Unification of the forces Electroweak Force: EM & Weak forces unify at high energies (10 15 K) Verified in particle accelerator experiments. Grand Unified Theory (GUTs): Strong & Electroweak forces unified. Predicted, but no experimental basis (yet)
10 Dreams of a final theory What about Gravity? Gravity should unify with the GUTs force at very high energies. Much higher than in any possible accelerator. However, these energies could occur in the early Universe. Problem: We have no quantum theory of Gravity!
11 The cosmic timeline Physics gives us a framework within which to describe the Big Bang from the earliest phases to the present. Particle accelerators probe matter at states similar to some of these early phases. Astronomers look for evidence in the present Universe (e.g., Cosmic Background, primordial deuterium & helium, dark energy)
12 LHC ASTR111 Lecture 24
13 LHC instrument, ATLAS ASTR111 Lecture 24
14 Planck epoch Before t=10 3 sec: All 4 forces unified into a single Superforce 1 force rules all of physics Can t say much else, since we don t yet have a quantum theory of gravity to guide us.
15 Planck epoch t<10-43 sec T>10 32 K No theory of quantum gravity All forces may have been unified
16 Grand unification epoch At t=10 3 sec, T=10 32 K (???): Gravity separates from the Superforce Strong & Electroweak Forces still unified. 2 forces rule physics: Gravity & GUTs Universe is a soup of quarks, antiquarks & photons.
17 Grand unification epoch <t<10-38 sec >T>10 29 K Gravity becomes distinct from other forces Era ends when strong & electroweak forces decouple; inflation?
18 Inflationary epoch t=10 3 sec (?), T=10 27 K (?): Strong force separates from GUTs force EM & Weak forces still unified 3 forces rule physics: Gravity, Strong, and Electroweak forces Rapid separation triggers a rapid inflation of the Universe
19 Inflationary epoch <t<10-20 sec >T>10 15 K Gravity, strong, & electroweak forces are distinct. Era ends when electrostatic & weak forces decouple.
20 The inflationary Universe Universe grows by a factor of between 10 3 and seconds! Expansion rate greatly slows after this brief burst of inflation. Helps to explain why the universe is so very smooth on large scales.
21 Four forces at last t=10 2 sec, T=10 15 K: Electroweak separates into EM & Weak forces All forces are now separate 4 forces rule physics: Gravity, Strong, Weak & Electromagnetic Conditions becoming right for free matter to begin to exist separate from photons.
22 Four forces at last ASTR111 Lecture 24
23 Quark freeze-out At t=10 6 sec, T=10 13 K: Free quarks combine into hadrons (primarily protons & neutrons) Particle-antiparticle pairs & photons in equilibrium: p n p n
24 Nucleon freeze-out At t=0.01 sec, T=10 11 K protons & neutrons decouple from photons and exist as free particles. electrons & positrons in equilibrium with photons neutrinos & nucleons in equilibrium Free neutrons are stable during this epoch.
25 Freeze-out As universe cools, particles and anti-particles annihilate, but fortunately for us there are slightly more particles:
26 Freeze-out <t<0.001 sec >T>10 12 K Amount of matter & antimatter nearly equal About 1 extra proton for every 10 9 protonantiproton pairs. ASTR111 Lecture 24 Inequality very important!
27 Neutrino decoupling At t=1 sec, T=10 10 K neutrinos decouple from matter stream out into space freely cosmic neutrino background (not yet observed) Free neutrons are no longer stable: Decay into protons, electrons & neutrinos Left with about 1 neutron for every 7 protons
28 Epoch of nucleosynthesis t~3 min, T=10 9 K: Fusion of protons & remaining free neutrons: Formation of 2 H (Deuterium) & 4 He End up with ~75% H, 25% He Traces of D, Li, Be, B We cannot observe this directly, but we can look for the products of these events.
29 Epoch of nucleosynthesis s<t<3 min >T>10 9 K Begins when matter annihilates remaining antimatter. Nuclei begin to fuse. Helium nuclei formed at ~3 minutes.
30 Epoch of nuclei 3 min<t<380,000 yrs, 10 9 >T>3000 K Universe cools to leave Hydrogen and Helium nuclei
31 Epoch of nuclei ~3 min<t<380,000 yrs 10 9 >T>3000 K Universe becomes too cool for photons to break helium apart (free-streaming)
32 Epoch of recombination t=380,000 yr T=3000 K: Electrons & nuclei combine into neutral atoms Universe becomes transparent Photons stream out into space Origin of the Cosmic Background Radiation Earliest we can see back directly using light.
33
34 Recombination ASTR111 Lecture 24
35 Epoch of recombination 380,000 yrs <t<10 9 yrs 3000>T>30 K Atoms formed. Cosmic background radiation released, Universe becomes transparent to electrons (Surface of last scattering)
36 Epoch of galaxies Galaxy formation: t=10 9 yrs, T~30 K Quasars. First generation of stars. First metals (heavy elements) from first supernovae. Present: t~10 10 yrs, T=2.726 K Galaxies, stars, planets, us... Lots of metals from many generations of supernovae of massive stars.
37 Cosmic timeline ASTR111 Lecture 24
38 What about the beginning? Our physics can not yet probe earlier than the end of the Planck epoch (t=10 3 sec). Some would say we have problems back before the Electroweak epoch (t=10 2 sec). This will be the astrophysics of the 21 st Century (or maybe the 22 nd )
39 Summary: Physics of the early Universe Informed by experimental & theoretical physics The cosmic timeline: Observations go back to t~3 minutes Reasonably firm physics back to t~10 6 sec Speculative back before t~10 2 sec Present theories stop at t~10 3 sec
40
Lecture 36: The First Three Minutes Readings: Sections 29-1, 29-2, and 29-4 (29-3)
Lecture 36: The First Three Minutes Readings: Sections 29-1, 29-2, and 29-4 (29-3) Key Ideas Physics of the Early Universe Informed by experimental & theoretical physics Later stages confirmed by observations
More informationLab Monday optional: review for Quiz 3. Lab Tuesday optional: review for Quiz 3.
Announcements SEIs! Quiz 3 Friday. Lab Monday optional: review for Quiz 3. Lab Tuesday optional: review for Quiz 3. Lecture today, Wednesday, next Monday. Final Labs Monday & Tuesday next week. Quiz 3
More informationASTR 1120 General Astronomy: Stars & Galaxies. OUR Universe: Accelerating Universe
ASTR 1120 General Astronomy: Stars & Galaxies FINAL: Saturday, Dec 12th, 7:30pm, HERE ALTERNATE FINAL: Monday, Dec 7th, 5:30pm in Muenzinger E131 Last OBSERVING session, Tue, Dec.8th, 7pm Please check
More informationASTR 101 General Astronomy: Stars & Galaxies
ASTR 101 General Astronomy: Stars & Galaxies ANNOUNCEMENTS FINAL EXAM: THURSDAY, May 14 th, 11:15am Last Astronomy public talk, May 8 th (up to 3% Extra class credit (see Blackboard announcement for details)
More informationEarly (Expanding) Universe. Average temperature decreases with expansion.
Early (Expanding) Universe Average temperature decreases with expansion. Particles & Anti-Particles Very short wavelength photons collide and form electron-positron pairs. E=mc 2 electron=matter positron=antimatter
More informationChapter 22: Cosmology - Back to the Beginning of Time
Chapter 22: Cosmology - Back to the Beginning of Time Expansion of Universe implies dense, hot start: Big Bang Future of universe depends on the total amount of dark and normal matter Amount of matter
More informationA100 Exploring the Universe Big Bang Theory and the Early Universe. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe and the Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu December 02, 2014 Read: Chap 23 12/04/14 slide 1 Assignment on Chaps 22 23, at the end of next week,
More informationChapter 22 Back to the Beginning of Time
Chapter 22 Back to the Beginning of Time Expansion of Universe implies dense, hot start: Big Bang Back to the Big Bang The early Universe was both dense and hot. Equivalent mass density of radiation (E=mc
More informationAstr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic
Astr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic Inflation Galaxy Formation 1 Chapter 24: #3 Chapter
More informationChapter 27 The Early Universe Pearson Education, Inc.
Chapter 27 The Early Universe Units of Chapter 27 27.1 Back to the Big Bang 27.2 The Evolution of the Universe More on Fundamental Forces 27.3 The Formation of Nuclei and Atoms 27.4 The Inflationary Universe
More informationJohn Ellison University of California, Riverside. Quarknet 2008 at UCR
Overview of Particle Physics John Ellison University of California, Riverside Quarknet 2008 at UCR 1 Particle Physics What is it? Study of the elementary constituents of matter And the fundamental forces
More informationThe Big Bang The Beginning of Time
The Big Bang The Beginning of Time What were conditions like in the early universe? The early universe must have been extremely hot and dense Photons converted into particle-antiparticle pairs and vice-versa
More informationLecture #25: Plan. Cosmology. The early Universe (cont d) The fate of our Universe The Great Unanswered Questions
Lecture #25: Plan Cosmology The early Universe (cont d) The fate of our Universe The Great Unanswered Questions Announcements Course evaluations: CourseEvalUM.umd.edu Review sheet #3 was emailed to you
More informationASTR 101 General Astronomy: Stars & Galaxies
ASTR 101 General Astronomy: Stars & Galaxies ANNOUNCEMENTS MIDTERM III: Tuesday, Nov 24 th Midterm alternate day: Fri, Nov 20th, 11am, ESS 450 At LAST: In the very Beginning BIG BANG: beginning of Time
More informationInflationary Universe and. Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation
Inflationary Universe and Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation Survey questions 1. The iclickers used in class encouraged
More informationSurvey questions. Inflationary Universe and. Survey Questions. Survey questions. Survey questions
Inflationary Universe and Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation Survey questions 1. The iclickers used in class encouraged
More informationChapter 27: The Early Universe
Chapter 27: The Early Universe The plan: 1. A brief survey of the entire history of the big bang universe. 2. A more detailed discussion of each phase, or epoch, from the Planck era through particle production,
More informationA100H Exploring the Universe: Big Bang Theory. Martin D. Weinberg UMass Astronomy
A100H Exploring the : Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 21, 2016 Read: Chap 23 04/26/16 slide 1 Early Final Exam: Friday 29 Apr at 10:30 am 12:30 pm, here! Emphasizes
More informationThe first 400,000 years
The first 400,000 years All about the Big Bang Temperature Chronology of the Big Bang The Cosmic Microwave Background (CMB) The VERY early universe Our Evolving Universe 1 Temperature and the Big Bang
More informationChapter 23 The Beginning of Time. Agenda. Presentation Tips. What were conditions like in the early universe? 23.1 The Big Bang.
Chapter 23 The Beginning of Time Agenda Announce: Observation April 19 Thursday 8pm APS Meeting April 17 no class (instead Fate of the Universe tutorial Presentation Tips Ch. 23 Presentation Tips Limit
More informationThe Beginning of the Universe 8/11/09. Astronomy 101
The Beginning of the Universe 8/11/09 Astronomy 101 Astronomy Picture of the Day Astronomy 101 Outline for Today Astronomy Picture of the Day Return Lab 11 Astro News Q&A Session Dark Energy Cosmic Microwave
More informationEarlier in time, all the matter must have been squeezed more tightly together and a lot hotter AT R=0 have the Big Bang
Re-cap from last lecture Discovery of the CMB- logic From Hubble s observations, we know the Universe is expanding This can be understood theoretically in terms of solutions of GR equations Earlier in
More informationOUSSEP Final Week. If we run out of time you can look at uploaded slides Pearson Education, Inc.
OUSSEP Final Week Last week hopefully read Holiday-Week 23rd November Lecture notes Hand in your Hubble Deep Field Reports today! (If not today then in my mail box @ International College.) Today we will
More informationHot Big Bang model: early Universe and history of matter
Hot Big Bang model: early Universe and history of matter nitial soup with elementary particles and radiation in thermal equilibrium. adiation dominated era (recall energy density grows faster than matter
More informationThe Big Bang Theory, General Timeline. The Planck Era. (Big Bang To 10^-35 Seconds) Inflationary Model Added. (10^-35 to 10^-33 Of A Second)
The Big Bang Theory, General Timeline The Planck Era. (Big Bang To 10^-35 Seconds) The time from the exact moment of the Big Bang until 10^-35 of a second later is referred to as the Planck Era. While
More informationPlasma Universe. The origin of CMB
Plasma Universe As we go back in time, temperature goes up. T=2.73(1+z) K At z~1100, T~3000 K About the same temperature as M-dwarfs Ionization of hydrogen atoms H + photon! p + e - Inverse process: recombination
More informationChapter 22 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Birth of the Universe Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Birth of the Universe 22.1 The Big Bang Theory What were conditions like in the early universe? How did the early universe change with time?
More information2. The evolution and structure of the universe is governed by General Relativity (GR).
7/11 Chapter 12 Cosmology Cosmology is the study of the origin, evolution, and structure of the universe. We start with two assumptions: 1. Cosmological Principle: On a large enough scale (large compared
More informationAstro-2: History of the Universe. Lecture 12; May
Astro-2: History of the Universe Lecture 12; May 23 2013 Previously on astro-2 The four fundamental interactions are? Strong, weak, electromagnetic and gravity. We think they are unified at high energies,
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 informationTuesday, Thursday 2:30-3:45 pm. Astronomy 100. Tom Burbine
Astronomy 100 Tuesday, Thursday 2:30-3:45 pm Tom Burbine tburbine@mtholyoke.edu www.xanga.com/astronomy100 Schedule Today (end and beginning of the universe) May 3 (Does Life Exist Elsewhere in the Universe)
More informationBig Bang, Black Holes, No Math
ASTR/PHYS 109 Dr. David Toback Lecture 19 1 Was due Today L19 Reading: (Unit 4) Unit 5: Assigned today Pre-Lecture Reading Questions (PLRQ) Unit 3 (Original or Revision) and Unit 4 Let us know if you think
More informationDEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS
DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS TSOKOS OPTION E-6 GALAXIES Introductory Video: The Big Bang Theory Objectives Understand the Hubble classification scheme of galaxies and describe the
More informationExploring the Early Universe. Chapter Twenty-Nine. Guiding Questions. The Isotropy Problem
Exploring the Early Universe Chapter Twenty-Nine Guiding Questions 1. Has the universe always expanded as it does today, or might it have suddenly inflated? 2. How did the fundamental forces of nature
More informationCosmology. Big Bang and Inflation
Cosmology Big Bang and Inflation What is the Universe? Everything we can know about is part of the universe. Everything we do know about is part of the universe. Everything! The Universe is expanding If
More informationLecture 17: the CMB and BBN
Lecture 17: the CMB and BBN As with all course material (including homework, exams), these lecture notes are not be reproduced, redistributed, or sold in any form. Peering out/back into the Universe As
More informationThe Expanding Universe
Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe
More informationLecture 19 Big Bang Nucleosynthesis
Lecture 19 Big Bang Nucleosynthesis As with all course material (including homework, exams), these lecture notes are not be reproduced, redistributed, or sold in any form. The CMB as seen by the WMAP satellite.!2
More informationOne of elements driving cosmological evolution is the presence of radiation (photons) Early universe
The Frontier Matter and Antimatter One of elements driving cosmological evolution is the presence of radiation (photons) Early universe Matter and antimatter But we live in universe full of matter -- where
More informationChapter 22 Lecture. The Cosmic Perspective. Seventh Edition. The Birth of the Universe Pearson Education, Inc.
Chapter 22 Lecture The Cosmic Perspective Seventh Edition The Birth of the Universe The Birth of the Universe 22.1 The Big Bang Theory Our goals for learning: What were conditions like in the early universe?
More informationClass 18 The early universe and nucleosynthesis
Class 18 The early universe and nucleosynthesis ch 12 of book Why did Gamov and Peebles suggest hot big band model? If the early Universe was hot (full of energy), a lot of features of the current universe
More informationMass (Energy) in the Universe:
Mass (Energy) in the Universe: smooth (vacuum) clumping Parameters of our Universe present values H = (71±4)km/s/Mpc = 1.0±0.0 m = 0.7±0.0 incl. b = 0.044±0.004 and < 0.014 photons r = 4.9-5 dark energy
More informationHubble s Law. Our goals for learning. What is Hubble s Law? How do distance measurements tell us the age of the universe?
Hubble s Law Our goals for learning What is Hubble s Law? How do distance measurements tell us the age of the universe? How does the universe s expansion affect our distance measurements? We measure speeds
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 informationWhat forms AGN Jets? Magnetic fields are ferociously twisted in the disk.
What forms AGN Jets? Magnetic fields are ferociously twisted in the disk. Charged particles are pulled out of the disk and accelerated like a sling-shot. Particles are bound to the magnetic fields, focussed
More informationRapid Inflation of the Early Universe. 27. Exploring the Early Universe. The Isotropy Problem. Possible Causes of Cosmic Inflation
27. Exploring the Early Universe Rapid inflation of the early Universe Mass & energy formed during inflation Most matter & antimatter annihilated each other Neutrinos & helium are primordial fireball relics
More informationThe Universe: What We Know and What we Don t. Fundamental Physics Cosmology Elementary Particle Physics
The Universe: What We Know and What we Don t Fundamental Physics Cosmology Elementary Particle Physics 1 Cosmology Study of the universe at the largest scale How big is the universe? Where What Are did
More informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
More informationCosmology: Building the Universe.
Cosmology: Building the Universe. The term has several different meanings. We are interested in physical cosmology - the study of the origin and development of the physical universe, and all the structure
More informationMatter vs. Antimatter in the Big Bang. E = mc 2
Matter vs. Antimatter in the Big Bang Threshold temperatures If a particle encounters its corresponding antiparticle, the two will annihilate: particle + antiparticle ---> radiation * Correspondingly,
More informationGalaxy A has a redshift of 0.3. Galaxy B has a redshift of 0.6. From this information and the existence of the Hubble Law you can conclude that
Galaxy A has a redshift of 0.3. Galaxy B has a redshift of 0.6. From this information and the existence of the Hubble Law you can conclude that A) Galaxy B is two times further away than Galaxy A. B) Galaxy
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter 17-2 Cosmology ³ The study of the origins, structure, and evolution of the universe ³ Key moments: ² Einstein General Theory of Relativity
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter. Olber s Paradox. Cosmology. Olber s Paradox. Assumptions 4/20/18
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter Cosmology ³The study of the origins, structure, and evolution of the universe ³Key moments: ²Einstein General Theory of Relativity ²Hubble
More informationThe Early Universe. 1. Inflation Theory: The early universe expanded enormously in a brief instance in time.
The Early Universe The Early Universe 1. Inflation Theory: The early universe expanded enormously in a brief instance in time. 2. The fundamental forces change during the first second after the big bang.
More informationPlanetarium/Observing: the clock is ticking! Don t forget to fill out your Planetarium/ Observing impression online.
Announcements HW #5 Due Wed, Dec. 10th. Planetarium/Observing: the clock is ticking! Don t forget to fill out your Planetarium/ Observing impression online. NOTE: Planetarium: Large dome you sit inside.
More information4 The Big Bang, the genesis of the Universe, the origin of the microwave background
4 The Big Bang, the genesis of the Universe, the origin of the microwave background a(t) = 0 The origin of the universe: a(t) = 0 Big Bang coined by Fred Hoyle he calculated the ratio of elements created
More informationWhat is the 'cosmological principle'?
What is the 'cosmological principle'? Modern cosmology always starts from this basic assumption the Universe is homogeneous and isotropic. This idea seems strange there's empty space between me and the
More informationLecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741
Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals
More informationHubble's Law. H o = 71 km/s / Mpc. The further a galaxy is away, the faster it s moving away from us. V = H 0 D. Modern Data.
Cosmology Cosmology is the study of the origin and evolution of the Universe, addressing the grandest issues: How "big" is the Universe? Does it have an "edge"? What is its large-scale structure? How did
More informationTimeline 5/4/17. Our Schedule and Topics
ASTR 1040: Stars & Galaxies Cosmic Web Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 30 Thur 4 May 2017 zeus.colorado.edu/astr1040-toomre Our Schedule and Topics Final Exam on Wed May 10,
More informationImplications of the Hubble Law: - it is not static, unchanging - Universe had a beginning!! - could not have been expanding forever HUBBLE LAW:
Cosmology and the Evolution of the Universe Edwin Hubble, 1929: -almost all galaxies have a redshift -moving away from us -greater distance greater redshift Implications of the Hubble Law: - Universe is
More informationCosmology and the Evolution of the Universe. Implications of the Hubble Law: - Universe is changing (getting bigger!) - it is not static, unchanging
Cosmology and the Evolution of the Edwin Hubble, 1929: -almost all galaxies have a redshift -moving away from us -exceptions in Local Group -with distance measurements - found a relationship greater distance
More informationThe Early Universe and the Big Bang
The Early Universe and the Big Bang Class 24 Prof J. Kenney June 28, 2018 Final Exam: Friday June 29 at 2-5pm in Watson A48 What the Final Exam will emphasize: Classroom lectures 10-24 (starting FRI June
More informationAy1 Lecture 18. The Early Universe and the Cosmic Microwave Background
Ay1 Lecture 18 The Early Universe and the Cosmic Microwave Background 18.1 Basic Ideas, and the Cosmic Microwave background The Key Ideas Pushing backward in time towards the Big Bang, the universe was
More informationi>clicker Quiz #14 Which of the following statements is TRUE?
i>clicker Quiz #14 Which of the following statements is TRUE? A. Hubble s discovery that most distant galaxies are receding from us tells us that we are at the center of the Universe B. The Universe started
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,
More informationIntroduction to Cosmology
Introduction to Cosmology Subir Sarkar CERN Summer training Programme, 22-28 July 2008 Seeing the edge of the Universe: From speculation to science Constructing the Universe: The history of the Universe:
More informationHomework 6 Name: Due Date: June 9, 2008
Homework 6 Name: Due Date: June 9, 2008 1. Where in the universe does the general expansion occur? A) everywhere in the universe, including our local space upon Earth, the solar system, our galaxy and
More informationPhysics 133: Extragalactic Astronomy and Cosmology. Week 8
Physics 133: Extragalactic Astronomy and Cosmology Week 8 Outline for Week 8 Primordial Nucleosynthesis Successes of the standard Big Bang model Olbers paradox/age of the Universe Hubble s law CMB Chemical/Physical
More informationAnnouncements. Homework. Set 8now open. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site.
Homework. Set 8now. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site. Review for Final. In class on Thursday. Course Evaluation. https://rateyourclass.msu.edu /
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 informationCosmology. An Analogy 11/28/2010. Cosmology Study of the origin, evolution and future of the Universe
Cosmology Cosmology Study of the origin, evolution and future of the Universe Obler s Paradox If the Universe is infinite why is the sky dark at night? Newtonian Universe The Universe is infinite and unchanging
More informationLecture 32: Astronomy 101
Lecture 32: Evidence for the Big Bang Astronomy 101 The Three Pillars of the Big Bang Threefundamental pieces of evidence: Expansion of the Universe: Explains Hubble s Law Primordial Nucleosynthesis: Formation
More informationa)! 0-10 miles b)! miles c)! miles d)! miles
How far away from this classroom will you be for Thanksgiving? a)! 0-10 miles b)! 10-100 miles c)! 100-1000 miles d)! 1000+ miles This Class (Lecture 33): The Early Universe HW 11 due on Dec 5 th Music:
More informationWhat is the evidence that Big Bang really occurred
What is the evidence that Big Bang really occurred Hubble expansion of galaxies Microwave Background Abundance of light elements but perhaps most fundamentally... Darkness of the night sky!! The very darkness
More informationOrigin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean?
Origin of the Universe - 2 ASTR 2120 Sarazin What does it all mean? Fundamental Questions in Cosmology 1. Why did the Big Bang occur? 2. Why is the Universe old? 3. Why is the Universe made of matter?
More informationToday. Last homework Due next time FINAL EXAM: 8:00 AM TUE Dec. 14 Course Evaluations Open. Modern Cosmology. Big Bang Nucleosynthesis.
Today Modern Cosmology Big Bang Nucleosynthesis Dark Matter Dark Energy Last homework Due next time FINAL EXAM: 8:00 AM TUE Dec. 14 Course Evaluations Open Elements of Modern Cosmology 1.Expanding Universe
More informationBIG BANG SUMMARY NOTES
BIG BANG SUMMARY NOTES BIG BANG THEORY Studies of red-shifts of distant galaxies show that the universe is expanding. This and other observations has led to the Big Bang Theory The Big Bang Theory claims
More informationAssignments. Read all (secs ) of DocOnotes-cosmology. HW7 due today; accepted till Thurs. w/ 5% penalty
Assignments Read all (secs. 25-29) of DocOnotes-cosmology. HW7 due today; accepted till Thurs. w/ 5% penalty Term project due last day of class, Tues. May 17 Final Exam Thurs. May 19, 3:30 p.m. here Olber
More informationAstronomy 122 Final Exam
Astronomy 122 Final Exam This Class (Lecture 28): The Beginning is the End. HW11 due Wednesday In this classroom, May 6 th from 1:30-4:30pm Multiple choice 70 questions. Can bring one sheet of notes Can
More informationAgenda. Chapter 17. Cosmology. Cosmology. Observations of the Universe. Observations of the Universe
Agenda Chapter 17 3/17/09 Measure Solar Altitude is it really 2pm? Announce: Observation: Tue March 24 Test 2: Tue March 24 Online stuff due by Test 2 Ch. 17 Cosmology Labwork: Hubble s Law & Large Scale
More informationCosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation
Cosmology Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Energy density versus scale factor z=1/a-1 Early times,
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 informationAstro-2: History of the Universe
Astro-2: History of the Universe Lecture 13; May 30 2013 Previously on astro-2 Energy and mass are equivalent through Einstein s equation and can be converted into each other (pair production and annihilations)
More informationKatsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy
11/14/12 Katsushi Arisaka 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Seven Phases of Cosmic Evolution 11/14/12 Katsushi Arisaka
More informationChapter 17 Cosmology
Chapter 17 Cosmology Over one thousand galaxies visible The Universe on the Largest Scales No evidence of structure on a scale larger than 200 Mpc On very large scales, the universe appears to be: Homogenous
More informationChapter 18. Cosmology in the 21 st Century
Chapter 18 Cosmology in the 21 st Century Guidepost This chapter marks a watershed in our study of astronomy. Since Chapter 1, our discussion has focused on learning to understand the universe. Our outward
More informationI V E R S U N. The Hot Big Bang I T Y T H E O F E. Andrew Liddle R G. Image: NASA/WMAP Science Team
The Hot Big Bang Andrew Liddle T H E O F E U N D I I V E R S N U B R G I T Y H Image: NASA/WMAP Science Team The Standard Model The discovery of the Higgs particle completes the Standard Model of Particle
More informationUnity in the Whole Structure
Cosmology II Unity in the Whole Structure How is it possible by any methods of observation yet known to the astronomer to learn anything about the universe as a whole? It is possible only because the universe,
More informationPart 1: Protons to heavy elements!
Cosmic Evolution Part 1: Protons to heavy elements Big Bang occurred 13.8 Billion yrs ago (13.8 x 10 9 yr) Only fundamental particles existed for first few minutes Name Proton Neutron Electron Photon Neutrino
More informationThe slides with white background you need to know. The slides with blue background just have some cool information.
The slides with white background you need to know. The slides with blue background just have some cool information. The Big Bang cosmology the study of the origin, properties, processes, and evolution
More informationASTR 200 : Lecture 33. Structure formation & Cosmic nuceleosynthesis
ASTR 200 : Lecture 33 Structure formation & Cosmic nuceleosynthesis 1 At the time of decoupling, the CMB tells us that the universe was very uniform, but that there were 10-5 fluctuations Known because
More informationCosmology. Chapter 18. Cosmology. Observations of the Universe. Observations of the Universe. Motion of Galaxies. Cosmology
Cosmology Chapter 18 Cosmology Cosmology is the study of the structure and evolution of the Universe as a whole How big is the Universe? What shape is it? How old is it? How did it form? What will happen
More informationParticles in the Early Universe
Particles in the Early Universe David Morrissey Saturday Morning Physics, October 16, 2010 Using Little Stuff to Explain Big Stuff David Morrissey Saturday Morning Physics, October 16, 2010 Can we explain
More informationAn Introduction to Particle Physics
An Introduction to Particle Physics The Universe started with a Big Bang The Universe started with a Big Bang What is our Universe made of? Particle physics aims to understand Elementary (fundamental)
More informationPrimordial (Big Bang) Nucleosynthesis
Primordial (Big Bang) Nucleosynthesis H Li Be Which elements? He METALS - 1942: Gamow suggests a Big Bang origin of the elements. - 1948: Alpher, Bethe & Gamow: all elements are synthesized minutes after
More informationLecture 2: The First Second origin of neutrons and protons
Lecture 2: The First Second origin of neutrons and protons Hot Big Bang Expanding and cooling Soup of free particles + anti-particles Symmetry breaking Soup of free quarks Quarks confined into neutrons
More informationAstronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006
Astronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006 Information Makeup quiz Wednesday, May 31, 5-6PM, Planetarium Review Session, Monday, June 5 6PM, Planetarium Cosmology Study of the universe
More informationLecture 3: Big Bang Nucleosynthesis The First Three Minutes Last time:
Lecture 3: Big Bang Nucleosynthesis The First Three Minutes Last time: particle anti-particle soup --> quark soup --> neutron-proton soup p / n ratio at onset of 2 D formation Today: Form 2 D and 4 He
More information