Lecture 18 : Where does matter come from? The structure of matter
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1 Lecture 18 : Where does matter come from? The structure of matter Structure of atoms; the elements The Standard Model for Particle Physics Timeline for the Hot Big Bang 11/11/13 1 I: THE STRUCTURE OF MATTER Atoms are made up of Nucleus (very tiny but contains most off mass) Electrons (orbit around the nucleus) Atom held together by (electromagnetic) attraction between positively-charged nucleus and negatively-charged electrons. 11/11/13 2 1
2 Atomic nuclei The nucleus is itself made up of: Protons, p (positively charged) Neutrons, n (neutral; no charge) Collectively, these particles are known as baryons p is slightly less massive than n (0.1% difference) Protons and neutrons bound together by the strong nuclear force (exchange of gluons ) 11/11/13 3 Elements & isotopes Number of protons determines the element: Hydrogen 1 proton Helium 2 protons Lithium 3 protons Beryllium 4 protons Boron 5 protons Carbon 6 proton Number of neutrons determines the isotope e.g., for hydrogen (1 proton), there are three isotopes Normal Hydrogen (H or p) no neutrons Deuterium (d) 1 neutron Tritium (t) 2 neutrons 11/11/13 4 2
3 Standard model of particle physics [Discussion on board] 11/11/ /11/13 6 3
4 II : Threshold temperature Universe started off very hot and cooled as it expanded; the temperature characterizing the radiation goes as The average energy of the photons is proportional to the temperature of the radiation k B is called Boltzmann s constant (has the value of k B = J/K) 11/11/13 7 At early times, when the Universe was dense and hot, the photons had enormous energy they were able to interact and produce particle/anti-particle pairs. For a given kind of particle (e.g., electrons or protons) we can define the threshold temperature. Definition : Threshold Temperature of a particle species is that temperature at which the typical energy of a pair of photons is just enough to create a particle/anti-particle pair T thres = mc 2 k B 11/11/13 8 4
5 Different particles with different masses have different threshold temperatures Protons : T K Electrons : T K Above the threshold temperature Continual creation/destruction of particles and anti-particles (equilibrium) Below threshold temperature Can no longer create pairs Particles and anti-particles annihilate Small residual of particles (matter) left over 11/11/13 9 III : TIMELINE FOR THE BIG BANG The Big Bang! (t=0) The Planck Epoch (t<10-43 s) All fundamental forces are coupled Very difficult to describe the universe at this time something completely outside of our experience. Full theory of Quantum Cosmology needed to describe this period of the Universe s life Such a theory doesn t yet exist 5
6 End of the Planck Epoch (t=10-43 s) Gravity decouples from other forces Classical General Relativity starts to describe gravity very well Gravitons cease their interactions with other particles start free streaming through space Produces a background of gravitational waves (almost completely redshifted away in present day) The Unified Epoch (t= s) Universe is homogeneous soup of elementary particles Two forces operate Gravity (described by GR) All other forces (described by so-called Grand Unified Theories; GUT) Baryogenesis Slight asymmetry between particle & antiparticle Get more matter than antimatter by 1 part in 10 9 Same as ratio of number of baryons to CMB photons today This produces the matter dominance that we have today! At end of epoch, GUT force splits into Strong and Electroweak force. Inflation!!! [More later] 6
7 The quark epoch ( s) Universe consists of soup of Quarks Gluons Electroweak forces particles Photons Other more exotic particles Electroweak force splits at about t=10-11 s Quark epoch ends with quark-hadron phase transition quarks pull themselves together into particles called hadrons (baryons are a subclass of this). Hadron Epoch (t= s) Universe contains a soup of protons, neutrons, photons, W & Z particles + exotics Matter/anti-matter asymmetry from GUT era gives baryon/anti-baryon asymmetry. End of epoch given when temperature falls below proton threshold temperature 7
8 Lepton Epoch (t= s) Abundant production of electron/positron pairs Equilibrium between protons and neutrons Epoch ended when temperature falls below electron threshold temperature. Proton/Neutron ratio frozen in at this point. 8
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