Unity in the Whole Structure Evolution of the Universe from 13 to 4 Billion Years Ago Prof Dr Harold Geller hgeller gmu edu http physics gmu edu hgeller Department of Physics and Astronomy George Mason University 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 vast though it is shows certain characteristics of a unified and bounded whole science shows unity in the whole structure and diversity only in details Simon Newcomb 1906 The Big Bang Begats What I m Going to Talk About The Big Bang Theory of the Formation of the Universe Radiation Matter and the Physical Laws Kirchoff s Spectroscopic Laws Planck s Radiation Curves Stefan Boltzmann Law Newton s Law of Motion Maxwell s Equations for Electromagnetism Hubble s Law Einstein s General Theory of Relativity Bohr s Atom Wien s Law Kepler s Laws of Planetary Motion Newton s Law of Universal Gravitation Doppler Effect Einstein s Special Theory of Relativity Gamow s Big Bang The Formation of Galaxies and Stars The Nebular Condensation Theory and the Formation of the Solar System The Formation of the Earth The Precursors of the Formation of Life Some Basic Physics Kirchoff s Spectral Laws Continuous Spectrum any body ideal blackbody that is at a temperature above 0 K Emission Spectrum any low pressure gas that you place a high voltage across Absorption Spectrum Macrocosmos Quantum Fluctuation Radiation Electron Positron Higgs Fields Inflation Cosmos Universe Strong Force Proton Nuclear Fusion Beta Radioactivity Gas Electric Charge Rocks Life Field Cosmic Background Radiation Particles Particle Anti particle Interactions False Vacuum Spontaneous Symmetry Breaking Big Bang Quarks Neutron Alpha Radioactivity Atom Gravity Magnetism Air Humans Bohr s Atom Best described the workings of the Hydrogen atom one proton and one electron around the proton moving in orbits that are discretized quantized so that no intermediate orbits are allowed Absorption Emission any low pressure gas placed between a blackbody and the observer 1 Planck s Radiation Curves Wien s Law A way to depict frequency inverse of wavelength versus intensity Peak wavelength is inversely proportional to the temperature of the blackbody Cooler Body Peak Wavelength Hotter Body Intensity Intensity Frequency Frequency Kepler s Laws Stefan Boltzmann Law Energy radiated by blackbody is proportional to the temperature to the 4th power Kepler s First Law of Planetary Motion planets orbit sun in an ellipse with sun at one focus Kepler s Second Law of Planetary Motion Energyvs Temperature 60000 planets sweep out equal areas in equal times 50000 travel faster when closer slower when farther Energy E T4 40000 Kepler s Third Law of Planetary Motion 30000 20000 10000 0 0 2 4 6 8 10 12 14 Temperature Newton s Laws I Newton s First Law of Motion body at rest tends to stay at rest and body in uniform motion will stay in straight line uniform motion unless acted upon by an outside force Newton s Second Law of Motion the acceleration of a body is proportional to the force being applied 16 orbital period squared is proportional to semimajor axis cubed P2 a3 Newton s Laws II Newton s Third Law of Motion for every force there is an equal and opposite force action and reaction Newton s Law of Gravitational Attraction force is proportional to masses and inversely proportional to the distance squared F G m M r2 F ma 2 Doppler Shift A change in measured frequency caused by the motion of the observer or the source classical example of pitch of train coming towards you and moving away Maxwell s Electromagnetism Electricity according to Gauss relates electricity to electric charge Faraday s Law relates electric fields to magnetic fields Magnetism according to Gauss relates magnetism to electricity Ampere Maxwell Law relates magnetic field to electricity Einstein s Relativity Theories Special Theory of Relativity speed of light constant in all reference frames time dilation and simultaneity length and mass addition of velocities General Theory of Relativity Hubble s Law The further away a galaxy is the greater its recessional velocity and the greater its spectral red shift Principle of Equivalence curvature of space time v H0d There is a simple linear relationship between the distance a galaxy is from the Earth and the redshift of that galaxy which is a measure of the speed with which a galaxy is moving away from the Earth The value of the Hubble constant H0 is not known with certainty but best value today is approximately 67 km s Mpc 3 Hubble s Conculsion From Hubble s Law we can calculate a time in the past when universe was a point Big bang occurred about 13 15 billion years ago big bang formally proposed by Gamow based upon such evidence Big bang theory progenitors existed in looser manner In The Beginning In the beginning God created the particles and the antiparticles Now the temperature was high and the particles and the antiparticles were in equilibrium And God said Let there be light and He separated the photons from the particles and antiparticles God called the photons bosons and the particles and antiparticles He called fermions And there was pair production and there was photon creation the first 10 43 seconds Eric Schulman from A Briefer History of Time The Littlest of Physics Space Time Matter and Forces Types of Matter Quarks Baryons protons neutrons Electrons Leptons electrons neutrinos muons Types of Forces Gamow s Big Bang and Hoyle s Steady State Steady State Universe universe looks same and will look same continuous creation Big Bang Universe universe began in big bang or ylem single point of creation Details of the Big Bang The littlest of physics The Big Bang ensuing Cosmic Eras The Vacuum Era The Planck Epoch and The Inflationary Epoch The Radiation Era Light and Baryons The Electroweak Epoch and The Strong Epoch Decoupling and the creation of matter The Matter Era Transition to matter Galaxy Formation Epoch and Stellar Epoch The Degenerate Dark Era Dead Star Epoch and Black Hole Epoch Whither the future Back to the Beginning The universe began as an infinitely dense cosmic singularity which began its expansion in the event called the Big Bang which can be described as the beginning of time During the first 10 43 second after the Big Bang the universe was too dense to be described by the known laws of physics gravity electromagnetism strong weak 4 The Vacuum Era