The Big Bang Or… The Standard Model. Precepts of the standard model The laws of Physics are the same throughout the Universe. The Universe is expanding.

Slides:



Advertisements
Similar presentations
Objectives: 1. relate the cosmological principle to isotropy and homgeneity of the universe. 2. understand how Hubble’s law is used to map the universe,
Advertisements

Major Epochs in the Early Universe t3x10 5 years: Universe matter dominated Why? Let R be the scale length.
The Expanding Universe!
A Scientific History of the Universe. How do we predict the conditions of the early universe? What are the different eras in the early universe? What.
Chapter 17 The Beginning of Time
Chapter 17: The Birth of the Universe
ORIGIN OF THE UNIVERSE P In the beginning, God created the heaven and the earth; and the earth was without form and void; and darkness was upon the face.
Cosmology The Origin and Future of the Universe Part 2 From the Big Bang to Today.
La teoria del big bang y la formacion del Universo.
Big Bang …..was actually very small and quiet. Atoms are mostly empty space.
Age, Evolution, and Size of the Cosmos Szydagis and Lunin.
Early Universe Chapter 38. Reminders Complete last Mallard-based reading quiz before class on Thursday (Ch 39). I will be sending out last weekly reflection.
Astronomy 100 Tuesday, Thursday 2:30 - 3:45 pm Tom Burbine
Advances in contemporary physics and astronomy --- our current understanding of the Universe Lecture 5: Evolution of Early Universe April 30 th, 2003.
© 2010 Pearson Education, Inc. Chapter 23 The Beginning of Time.
Do your course evaluations.
Introductory Video: The Big Bang Theory Objectives  Understand the Hubble classification scheme of galaxies and describe the structure of the Milky.
Evolution of the Universe (continued)
The Big Bang Or… The Standard Model. Precepts of the standard model The laws of Physics are the same throughout the Universe. The Universe is expanding.
The Big Bang Astrophysics Lesson 18. Learning Objectives To know:-  What is the big bang theory  What is the evidence supporting it including:-  Cosmological.
ASTR Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture23]
History of the Universe. If the universe was 1 year old...
The Evolution of the Universe Nicola Loaring. The Big Bang According to scientists the Universe began ~15 billion years ago in a hot Big Bang. At creation.
Big Bang timeline. Big Bang Timeline 13.7 billion years ago – Before the Big Bang, the universe was a hot point ( ) of pure energy : Tremendous levels.
Hubble’s Law Our goals for learning What is Hubble’s Law?
Exploring the Early Universe Chapter Twenty-Nine.
Intro to Cosmology! OR What is our Universe?. The Latest High Resolution Image of the Cosmic Microwave Background Radiation Low Energy RegionHigh Energy.
Happyphysics.com Physics Lecture Resources Prof. Mineesh Gulati Head-Physics Wing Happy Model Hr. Sec. School, Udhampur, J&K Website: happyphysics.com.
© 2010 Pearson Education, Inc. Chapter 23 The Beginning of Time.
AS2001 / 2101 Chemical Evolution of the Universe Keith Horne Room 315A
AS2001 Chemical Evolution of the Universe Keith Horne 315a
Today: “Nucleosynthesis… another phase change in early universe… and why is the Universe so Flat?” HW for next time: Onion, “the nucleus and forces of.
Cosmology, Cosmology I & II Fall Cosmology, Cosmology I & II  Cosmology I:  Cosmology II: 
BIG BANG TIMELINE FILL IN YOUR MISSING DATA. THE BIG BANG 0 to seconds Temperature- theorized to be infinite Infinitely small, Infinitely Dense,
The Big Bang Or… The Standard Model.
THE BIG BANG Theory… How did the universe begin?.
The Life of the Universe From Beginning to End.
Chapter 17 The Beginning of Time. Running the Expansion Backward Temperature of the Universe from the Big Bang to the present (10 10 years ~ 3 x
The Beginning of Time: Evidence for the Big Bang & the Theory of Inflation.
The Universe Characteristics –Expanding (Hubble’s Law) –Finite age –Cool now, hotter long ago –Composition 70% H, 28% He, 2% the rest – Why? –Most matter.
Chapter 18: Chapter 18: Cosmology. WHAT DO YOU THINK? What does the universe encompass? Is the universe expanding, fixed in size, or contracting? Will.
Goal: To understand the history of the universe especially the beginning Objectives: 1)To learn about the beginning of the Big bang! 2)To explore the Big.
Cosmology -- the Origin and Structure of the Universe Cosmological Principle – the Universe appears the same from all directions. There is no preferred.
Universe Tenth Edition Chapter 26 Exploring the Early Universe Roger Freedman Robert Geller William Kaufmann III.
Cosmology That part of astronomy which deals with the nature of the universe as a whole.
Option D. 3. Universe was born around 13.8 billion years ago in process called Big Bang In the beginning, all matter & energy in the entire universe was.
Discovering the Universe Eighth Edition Discovering the Universe Eighth Edition Neil F. Comins William J. Kaufmann III CHAPTER 18 Cosmology Cosmology.
Astrophysics – final topics Cosmology Universe. Jeans Criterion Coldest spots in the galaxy: T ~ 10 K Composition: Mainly molecular hydrogen 1% dust EGGs.
ORIGIN OF THE UNIVERSE In the beginning, God created the heaven and the earth; and the earth was without form and void; and darkness was upon the face.
Lecture 24: The Epochs of the Universe Astronomy 1143 – Spring 2014.
Important Stuff (Section 3) The Final Exam is Monday, December 19, 1:30 pm – 3:30 pm The Final Exam room is Physics 150 Bring 2 pencils and a photo-id.
Chapter 19: The Beginning of Time A Hot Early Universe The Story of Creation Evidence for the Big Bang Inflation Did the BB really happen?
© 2017 Pearson Education, Inc.
Harrison B. Prosper Florida State University YSP
Chapter 23 The Beginning of Time
Alternative to Big Bang theory: Steady State Cosmology
Lectures on galaxies and cosmology
Universe! Early Universe.
The Big Bang The Big Bang
Big Bang: timeline.
Introduction To Modern Astronomy II
The Beginning of Time (Birth Of The Universe)
Cosmology Chapter 15 Great Idea:
Early Universe.
Did someone monkey with the laws of nature ? Unit 1.1
Early Universe.
The Big Bang The Big Bang
The Big Bang Or… The Standard Model.
Cosmology.
Learning Goals: 4. Complex Knowledge: demonstrations of learning that go aboveand above and beyond what was explicitly taught. 3. Knowledge: meeting.
Presentation transcript:

The Big Bang Or… The Standard Model

Precepts of the standard model The laws of Physics are the same throughout the Universe. The Universe is expanding The Universe is isotropic and homogeneous General relativity works. The early Universe was hotter than it is today The Universe is evolving. The cosmological principle.

A bit of history Einstein’s General relativity predicts that the Universe is either expanding or contracting 1920s Hubble discovers the expansion of the Universe. 1940s Gamow et al work on a Big Bang model: If space is expanding, then it was once small If it was small, it was hot. (Adiabatic expansion cools) If it was once hot, it should be a little warm now.

They (Gamow) predicted that we should still be able to see radiation from the young Universe. (This is known as the cosmic microwave background radiation or CMBR) The radiation should have a Wien temperature of about 5 K Display a black body curve Be the same in all directions A bit of history... Nobody paid any attention to these predictions

1965 Arno Penzias and Richard Wilson are having “noise” problems with their radio telescope: 7.35 cm radiation is everywhere. At first they think it is their equipment But it’s coming from “out there” A bit of history...

1989 The Cosmic Background Explorer (COBE) spacecraft measures the CMBR. The radiation is isotropic It has a Wien temperature of K It is exactly black body as predicted by the big bang: (error bars, put λmax in notes) A bit of history...

1992 The Cosmic Background Explorer (COBE) measures miniscule fluctuations (anisotropies) in the CMBR. The anisotropies are exactly what the big bang model predicts from the Heisenberg uncertainty of the early Universe: - (Smoot and the “eye of God”) A bit of history...

Spherical Harmonics. - the ringing of the universe Spring 2000, Boomerang measures primordial sound waves: A bit of history...

1) the universe was 13.7 billion years old, plus or minus about 200 million years, 2) it is composed of 4% matter, 22% dark matter, and 74% dark energy (later) 3) the Hubble Constant is 71.0(km/sec)/MPc +/- 2.5, not 50 or 100 as some researchers had suggested, and 4) the universe is flat (similar to what the BOOMERANG craft had seen). As of 2003/6 The WMAP Probe:

The Standard Model Bang Now Thermal Energy decreases (Allows creation of things with less and less mass) Like condensation (particle accelerators)

The Standard Model Bang Now Basic concepts: Adiabatic expansion Stretching of radiation Matter becoming energy, Energy becoming matter Matter as “condensed” energy Wien’s Law/ ”Temp”/ energy per photon

Types of Particles Gauge Bosons Leptons Hadrons (made of quarks) Masses Heavier particles decay into lighter…

Put this in your notes: Key Photon energy thresholds: 2x938 MeV ≈ 2 GeV – energy to create the lightest Hadron. (proton) 2x0.511 MeV ≈ 1 MeV – energy to create the lightest Lepton (electron) 1.3 eV – energy to ionize atoms (plasma vs not plasma) Calculate the Wien Temperature of each of these energies. E = hf = hc/ = (6.626E-34 Js)(3.00E8 m/s)/ λ max (metres) = 2.90 x m / K T (Kelvin) 1 eV = 1.602x J 1 MeV = 1x10 6 eV

Put this in your notes: Key Photon energy thresholds: 2x938 MeV ≈ 2 GeV – energy to create the lightest Hadron. (proton) E = hf = hc/, T = 2.90 x mK

Put this in your notes: Key Photon energy thresholds: 2x0.511 MeV ≈ 1 MeV – energy to create the lightest Lepton (electron) E = hf = hc/, T = 2.90 x mK

Put this in your notes: Key Photon energy thresholds: 1.3 eV – energy to ionize atoms (plasma vs not plasma) E = hf = hc/, T = 2.90 x mK

The Standard Model Before seconds: General Relativity doesn’t work Don’t yet have a quantum theory of gravity We think the four forces of nature were unified. (Um… Gravity, Electromagnetic, Weak Nuclear, and Strong Nuclear)

The Standard Model seconds to seconds: Gravity has “condensed” out No distinction between fundamental particles.

The Standard Model seconds to seconds: Strong Nuclear Separate Quarks are confined Hadron era (Protons and Neutrons are Hadrons) Energy of photons… Roughly equal Matter and Anti matter being created and destroyed. Slight imbalance of Matter (1 in 10 9 )

The Standard Model seconds to 10 seconds: Photon Energy drops below mass of Hadrons Hadron matter annihilates Hadron anti matter Lepton era (electrons, positrons, neutrinos) (there are also photons around) Lepton eat lepton universe

The Standard Model 10 seconds to.38 x 10 6 years: Thermal Energy drops below mass of Leptons Lepton matter annihilates Lepton anti matter Slight imbalance of Matter persists to this day (1 in 10 9 ) Radiation era (neutrinos, photons)

The Standard Model.38 x 10 6 years to Present: Thermal energy drops below binding energy of atomic electrons Atoms are born Photons de-couple from matter (To become CMBR) Expansion of the Universe stretches out radiation Universe is now matter dominated. Soon after atoms form, stars and galaxies form as well.

The Standard Model About 2 or 3 minutes after the Big Bang, fusion occurs. 1 H, 2 H, 3 H, 4 He…maybe some Lithium…are created (No A = 5 or 8) BBN theory predicts that 75% of matter be Hydrogen, and 25% Helium. This is what we see today. Stars forge heavy elements later. Older stars should have fewer heavy elements than new ones. This is what we see today. Meanwhile back at the ranch: