History of the Universe

Slides:



Advertisements
Similar presentations
Chapter 18: Cosmology For a humorous approach to quarks, check out the Jefferson Lab’s game.  In Looking for the Top Quark, each player receives six quarks.
Advertisements

Notes 30.4 The Big Bang Theory
Major Epochs in the Early Universe t3x10 5 years: Universe matter dominated Why? Let R be the scale length.
Dark Matter, Dark Energy, and the Fate of the Universe.
The Fate of the Universe. The cosmological principle The simplest universes is: Homogenous – the same everywhere you go Isotropic – the same in all directions.
Chapter 20 Dark Matter, Dark Energy, and the Fate of the Universe.
BIG BANG. EVIDENCE FOR BIG BANG Hot Big Bang Model: The universe began expanding a finite time ago from a very dense, very hot initial state. Dense Dense.
Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 10. Inflation.
Cosmological Structure Formation A Short Course
Cosmology Astronomy 315 Professor Lee Carkner Lecture 22 "In the beginning the Universe was created. This has made a lot of people very angry and been.
The Dark Side of the Universe Scott Watson Dept. of Physics Brown University
The Birth Of Our Universe The Big Bang And Inflation
Cosmology Astronomy 315 Professor Lee Carkner Lecture 22 "In the beginning the Universe was created. This has made a lot of people very angry and been.
Physics 133: Extragalactic Astronomy ad Cosmology Lecture 6; January
Cosmology Astronomy 315 Professor Lee Carkner Lecture 24.
Galaxy Evolution 1) Density fluctuations in the primordial matter 2) galaxies grew by repeated merging of smaller objects - evidence: galaxies at large.
© 2010 Pearson Education, Inc. Chapter 23 The Beginning of Time.
ASTR100 (Spring 2008) Introduction to Astronomy The Case for Dark Matter Prof. D.C. Richardson Sections
Galaxies and Cosmology 5 points, vt-2007 Teacher: Göran Östlin Lecture 12.
Types of Galaxies Elliptical: Spiral: Irregular:.
Inflation, Expansion, Acceleration Two observed properties of the Universe, homogeneity and isotropy, constitute the Cosmological Principle Manifest in.
Chapter 30 Section 4 Handout
The Big Bang Astrophysics Lesson 18. Learning Objectives To know:-  What is the big bang theory  What is the evidence supporting it including:-  Cosmological.
17.3 The Big Bang and Inflation 17.4 Observing the Big Bang for yourself Our Goals for Learning What aspects of the universe were originally unexplained.
Pop-quiz #21 Which of the following statements is TRUE? A.Black holes can emit particles and thereby lose mass — this is called Hawking radiation B.John.
Hubble’s Law Our goals for learning What is Hubble’s Law?
Cosmology: The Study of the Universe as a Whole Physics 360 Geol 360 Astronomy John Swez.
Cosmology The Origin, Evolution, and Destiny of the Universe.
Why is the universe lumpy? Tuesday, February 19.
© 2010 Pearson Education, Inc. Chapter 23 The Beginning of Time.
COSMOLOGY SL - summary. STRUCTURES Structure  Solar system  Galaxy  Local group  Cluster  Super-cluster Cosmological principle  Homogeneity – no.
Expansion of the Universe Natural consequence of the basic field equations of the General Theory of Relativity (GTR) When GTR was first developed in the.
Astrophysics ASTR3415: Homework 4, Q.2. Suppose there existed Velman cosmologists who were observing the CMBR when the light we now see from the supernova.
2 pt 3 pt 4 pt 5pt 1 pt 2 pt 3 pt 4 pt 5 pt 1 pt 2pt 3 pt 4pt 5 pt 1pt 2pt 3 pt 4 pt 5 pt 1 pt 2 pt 3 pt 4pt 5 pt 1pt.
10B The Big Bang Where do we come from, where are we going?
The Life of the Universe From Beginning to End.
The Beginning of Time: Evidence for the Big Bang & the Theory of Inflation.
Astro-2: History of the Universe Lecture 10; May
General Relativity and Cosmology The End of Absolute Space Cosmological Principle Black Holes CBMR and Big Bang.
Cosmology (Chapter 14) NASA. Student Learning Objectives Describe the Big Bang theory Analyze possible fates of our universe.
Homework for today was WORKBOOK EXERCISE: “Expansion of the Universe” (pg in workbook)
1 Cosmic Microwave Background Radiation (CMBR) Relic of the Big Bang ( “ afterglow ” of initial fireball) predicted in late 1940s Discovered by Penzias.
Universe Tenth Edition Chapter 25 Cosmology: The Origin and Evolution of the Universe Roger Freedman Robert Geller William Kaufmann III.
The Fate of the Universe What property determines the ultimate fate of the universe?
The Universe Through Time: The Big Bang. The Universe Through Time: The Curvature of Space.
The Fate of the Universe. The fate depends on the rate of expansion and the density Density greater than critical value – gravity will halt expansion.
Stars, Galaxies, and the Universe Section 4 Section 4: The Big Bang Theory Preview Key Ideas Hubble’s Observations A Theory Emerges Big Bang Theory Universal.
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.
THE BIG BANG THEORY. HOW IT ALL BEGAN Scientists hypothesize that approximately 13.7 billion years ago, a rapid expansion created the universe, producing.
The Size and Shape of the Universe. The Uniform Temperature of the Early Universe The brighter and darker spots in the microwave background correspond.
Chapter 23 The Beginning of Time
Chapter 30 Section 4 Big Bang Theory.
Alternative to Big Bang theory: Steady State Cosmology
Introduction To Modern Astronomy II
Where do we come from, where are we going?
Section 4: The Big Bang Theory
MLSC 550: Modern Astronomy
Types of Galaxies Elliptical: Spiral: Irregular:.
Our Universe What it is like, how it started, how it evolved to its current state, and how it will end.
Expansion of the Universe
The Big Bang and the Expansion of the Universe
History of the Universe
Sci Formation of the Universe
The Last Epoch.
Dark Matter, Dark Energy, and the Fate of the Universe
Homework #10 is due tonight, 9:00 pm.
Cosmology: The Origin and Evolution of the Universe
COSMOLOGY Prospects in Theoretical Physics Institute for Advance Study
Dark Energy.
Recombination t = 380 ky T = 4000 K
Presentation transcript:

History of the Universe How did the universe evolve so uniformly? Why is the CMBR temperature the same everywhere ? When and how did matter form ? Why are the H and He abundances the same everywhere (except for He produced in stars) ? Why is the expansion accelerating? Is the universe open or closed ?

Fluctuations and Large-Scale Structure Disturbances in the early universe grow in time; their size determines large-scale structure and properties such as the curvature of the universe.

“Hot spots” in the early universe as we see them today: Indicators of the curvature of the Universe

Uniformity and Isotropy of CMBR Why is the temperature of CMBR the same everywhere? The extremely uniform background radiation everywhere in the Universe presents a problem since different parts of the Universe may have been out of touch (even by light) from each other, i.e. outside each other’s event horizons

Observable Universe

Early to Present Universe (Flat?)

Temperature Evolution of the Universe Holds nucleus together Charged particles

Temporal Evolution of the Universe

History of forces and particles in the Universe

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2025 SlidePlayer.com. Inc. All rights reserved.