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From Subatomic Particles to the Cosmos (Particle Physics Today) Mark Oreglia The Enrico Fermi Institute The University of Chicago Outline: Particle and Forces Recent Cosmology Synthesis The New Tools 18 May 2006 M. Oreglia/ Linda Hall Library 1 Particle Physicists are concerned with the very small: 18 May 2006 M. Oreglia/ Linda Hall Library 2 Atoms can be imaged • With the best electron microscopes we can make very believable images of atoms • For smaller objects we use similar instruments … but do not create such a graphic image 18 May 2006 STM image of nickel atoms in crystal M. Oreglia/ Linda Hall Library 3 Accelerators: 1890-now! • Thompson’s electron tube is the basis for the discovery of the electron, the TV picture tube, … and all current accelerators 18 May 2006 M. Oreglia/ Linda Hall Library 4 Discovery of The Nucleus α particle Rutherford 1909 Led to new model of atom α particle size: Nucleus Fly = Cathedral Atom nucleus ‘like a fly in a cathedral’ electron 18 May 2006 M. Oreglia/ Linda Hall Library 5 Scattering = Diffraction • The pattern of scattered radiation tells you about the structure it is scattering off Water wave diffracting as it passes through a slit 18 May 2006 M. Oreglia/ Linda Hall Library 6 The Elementary Particles • So, from 1890 to 1990 we established a hierarchy of: – non-composite (i.e., elementary) types of matter – 4 distinct force carriers that allow matter to interact – Plus the antimatter 18 May 2006 M. Oreglia/ Linda Hall Library 7 The 4 Known Forces •The forces are characterized by their very different strengths • STRONG: affects the quarks; manifested in alpha radioactivity; holds nucleus together • strength 1, but only at short distances • EM: affects quarks and charged leptons; holds atom together • strength 1/100 • WEAK: affects quarks and leptons; evident in beta radioactivity • strength 1/10000 • GRAVITY: affects all(?) • strength 10-38!!! 18 May 2006 M. Oreglia/ Linda Hall Library 8 Common Matter: quarks + leptons • QUARKS: combine in pairs or triplets to form larger objects called hadrons: – qqq ~ baryons (p = uud; n = udd, etc) – qq ~ mesons (pion = u + anti-u) • LEPTONS: the family consisting of: – the electron and her heavier partners (muon, tau) • Hundreds of muons are passing through your body every second … the cosmic rays – The electrically neutral partners (neutrinos) • Even more neutrinos are bombarding you • And their antimatter counterparts – A basic symmetry of nature! 18 May 2006 M. Oreglia/ Linda Hall Library 9 How we know • Years of experiments with particle accelerators – Bring electrons or protons to high energy and let them scatter off the objects we want to study … or let them break the target apart into the ultimate constituents – A basic law of nature tells us that the probe particle has to have higher energy to image smaller targets: resolution ~ 1/E De Broglie 18 May 2006 M. Oreglia/ Linda Hall Library 10 More than mere classification • By 1970 we had a really good theory of the particles and forces … so good, we call it the “Standard Model” – Specific mathematics describing the ways quarks and leptons interact via strong, EM and weak forces; predictive and testable! 18 May 2006 M. Oreglia/ Linda Hall Library 11 Einstein’s Dream Partially Realized • The SM theory succeeded in unifying 2 of the forces: EM+Weak into a single theory 18 May 2006 M. Oreglia/ Linda Hall Library 12 The Problem with Theories • Predictions are a nuisance – you’ve gotta verify them! – The Standard Model unified EM+Weak by introducing a new particle field nobody has seen yet … the celebrated Higgs Boson • This “field” is the entity which could give mass to all the matter particles Peter Higgs (not a boson (Thanks to Prof. David Miller) 18 May 2006 M. Oreglia/ Linda Hall Library 13 Higgs Boson, where art thou? • Searching for the Higgs Boson has become the #1 priority in particle physics • Searches in the 1990’s hinted at its existence just outside the reach of current accelerators 18 May 2006 M. Oreglia/ Linda Hall Library 14 We expect to see it soon We expect to see it in 2008 or 2009 when the new “LHC” accelerator comes online at the CERN laboratory in Geneva, Switzerland … … more on that later 18 May 2006 M. Oreglia/ Linda Hall Library 15 Theories mean more theories • Despite the success of the SM, it opened a Pandora’s box of esoteric problems, such as: – Where do all the parameters come from? – How do they get their particular values – Why don’t we have a theory of gravity!!! • So we expand on the theory – Invent new particles (eg, supersymmetry) purely on the basis of mathematical aesthetics – Invent new theories (strings) purely on the basis of mathematical aesthetics • Job of accelerators: see if new particles exist 18 May 2006 M. Oreglia/ Linda Hall Library 16 Meanwhile, in a Gaxaxy Far Away • Enter a noteworthy astronomer from Marshfield: Edwin Hubble Riess, Press, Kirshner 1996 Slope is equal to 1/t, where t is the amount of time the expansion has been occurring Thus, t = 1.5 billion years ← 1 Mpsc = roughly earth to α-Centuri 18 May 2006 M. Oreglia/ Linda Hall Library 17 Hubble Expansion implies Big Bang • All objects in the cosmos are moving away from each other – Not exactly like an explosion…if you go to any reference point, the rest of the universe appears to be receding from you in the same way we see it – Visualize galaxies as proteins in a lump of bread dough as it rises, expanding in all directions Slice from Sloan Digital Sky Survey • The universe appears the same in all directions and in all regions … “homogeneous and isotropic” … this is the clincher: space itself is stretching … consequence of how gravity distorts space 18 May 2006 M. Oreglia/ Linda Hall Library 18 How We Know • It is only fairly recently that we can make reliable surveys of the space around us • Digital processing and automation of telescopes permits us to make billions of measurements • The speed of distance objects is measured using the Doppler Shift of the spectrum Here is what a spectrum looks like from sources moving away or towards you v = c x (wavelength shift) / (wavelength) Hubble: if you know v, you know distance 18 May 2006 M. Oreglia/ Linda Hall Library 19 Global Cooling • If space is stretching, then it used to be smaller – That means things were closer together (denser) at earlier times, likewise the energy density … and therefore the temperature increases as we go back in time – Here is where we can start interpreting the picture in terms of chemistry and particles • First an ultra hot universe so energetic that only the most elementary particles existed • As it expands, it cools; particles “condense” and form atoms, molecules, suns, planets, galaxies 18 May 2006 M. Oreglia/ Linda Hall Library 20 Cosmological Fine Print • The Big Bang did not occur at a single point in space as an "explosion." It is better thought of as the simultaneous appearance of space everywhere in the universe. That region of space that is within our present horizon was indeed no bigger than a point in the past. Nevertheless, if all of space both inside and outside our horizon is infinite now, it was born infinite. If it is closed and finite, then it was born with zero volume and grew from that. In neither case is there a "center of expansion" - a point from which the universe is expanding away from. • By definition, the universe encompasses all of space and time as we know it, so it is beyond the realm of the Big Bang model to postulate what the universe is expanding into. In either the open or closed universe, the only "edge" to space-time occurs at the Big Bang, so it is not logically necessary to consider this question. • It is beyond the realm of the Big Bang Model to say what gave rise to the Big Bang… where the stuff came from, etc 18 May 2006 M. Oreglia/ Linda Hall Library 21 18 May 2006 M. Oreglia/ Linda Hall Library 22 The evolving universe • 10 -43 sec, size = 10 -30 today, temp = 10 32 Kelvin • 10 -35 sec, size = 10 -26 today, temp = 10 28 Kelvin • 10 -12 sec, size = 10 -15 today, temp = 10 15 Kelvin • 10 -6 sec, size = 10 -12 today, temp = 10 12 Kelvin • 10 sec, size = 10 -9 today, temp = 10 9 Kelvin • 3.7×10 5 years, size = 10 -3 today, temp = 3×10 3 Kelvin • 10 8 years, size = 10 -1 today, temp = 30 Kelvin • 9×10 9 years, size = 5×10 -1 today, temp = 6 Kelvin • 13.7×10 9 years, size = 10 0 today, temp = 2.74 Kelvin – The Planck era. Quantum gravity is important; current theories are inadequate. We can't get any closer to the Big Bang at earlier times – Inflation. A temporary period of domination by a form of dark energy at an ultrahigh energy scale. A speculative theory. – Electroweak phase transition. At high temperatures, electromagnetism is unified with the weak interactions; now they become distinct. – Quark-gluon phase transition. Quarks and gluons become bound into the protons and neutrons we see today. – Primordial nucleosynthesis. Universe cools to a point where protons and neutrons combine to form light atomic nuclei, primarily Helium, Deuterium, and Lithium. – Recombination. Universe cools to a point where electrons can combine with nuclei to form atoms; becomes transparent. CMB is a snapshot of this era. – The dark ages. Ripples in the density gradually assemble into stars and galaxies. – Sun and Earth form. From the existence of heavy elements in the Solar System, we know that the Sun is a second-generation star, formed about five billion yrs ago. 18 May 2006 M. Oreglia/ Linda Hall Library 23 Nucleosynthesis in the early Universe • The predicted abundance of deuterium, helium and lithium depends on the density of ordinary matter in the early universe • About 24% of the ordinary matter in the universe is helium produced in the Big Bang – in very good agreement with observations and is another major triumph for the Big Bang theory • In order for the predicted yields of the other light elements to come out in agreement with observations, the overall density of the ordinary matter must be roughly 4% of the critical density (… next slide) 18 May 2006 M. Oreglia/ Linda Hall Library 24 Amount of Matter affects Outcome • The stretching of the universe is a balance of outward forces and gravitational attraction • Thus, the total amount of gravitating stuff determines the kind of evolution • Critical density is a unique point 18 May 2006 M. Oreglia/ Linda Hall Library 25 Open, Flat, or Closed? • The amount of matter, and the fractions of different types of matter, determine whether the universe expands forever or eventually collapses – Radiation: composed of massless or nearly massless particles that move at the speed of light. Known examples include photons (light) and neutrinos. This form of matter is characterized by having a large positive pressure. – Baryonic matter: this is "ordinary matter" composed primarily of protons, neutrons and electrons. This form of matter has essentially no pressure of cosmological importance. – Pure Energy … like Einstein’s cosmological constant 18 May 2006 M. Oreglia/ Linda Hall Library 26 Einstein’s “big mistake” • The expanding nature of the Big Bang theory derives from Einstein’s general theory of relativity • Einstein originally wrote an equation for how space must expand under relativity: acceleration = - const/6R2 + 1/3 R Λ The “cosmological” constant was a term Einstein inserted on aesthetic grounds – to stop the expansion !!! He later called it his greatest mistake. (we now think it does indeed exist … an energy sea) 18 May 2006 M. Oreglia/ Linda Hall Library 27 Luminous Matter • Most of the larger collections of matter in the universe emit detectable radiation, from x-rays to radio frequencies • But most of the photons in the universe are actually not emitted by stars, gas, or any other object in the contemporary universe. Rather, they are the lowenergy photons left over from the Big Bang. This relic radiation is primarily in the microwave region of the spectrum, and is known as the Cosmic Microwave Background (CMB). Photons from the CMB pervade space, providing a background buzz that serves as a constant reminder of the hot, dense state in which our universe began 18 May 2006 M. Oreglia/ Linda Hall Library 28 The Cosmic Microwave Background • At startling discovery in 1965: we are bathed in a sea of photons equivalent to those emitted by an object at temp=2.7 Kelvin •Blackbody radiation: 18 May 2006 M. Oreglia/ Linda Hall Library 29 Why Isotropic Photons? • The Cosmic Microwave Background (CMB) strongly supports the Big Bang model – These would be the photons created from particle collisions after the density of matter became so dilute the photons were not being absorbed any longer – It therefore makes sense they should be coming uniformly from all directions (more or less) – They were created about 370,000 yr after the Big Bang, when the universe had a temperature of 3,700 K (we see the photons redshifted to 2.7 K) – These photons came from the “surface of last scattering” – the edge of the visible universe 18 May 2006 M. Oreglia/ Linda Hall Library 30 In pictures: • So, we see a consistent model where as the universe expands the fractions of different types of matter evolve 18 May 2006 M. Oreglia/ Linda Hall Library 31 The Latest Measurements • In recent years we have been able to perform very precise studies of the CMB – Space probes and Antarctic telescopes – Can see small variations in the CMB (10-5 level) 18 May 2006 M. Oreglia/ Linda Hall Library 32 The CMB Fluctuations • Here’s a plot of the amount of graininess at different distance scales • The first peak results from the interplay between gravity and acoustic shock • As the universe cooled, matter collected preferentially in certain areas … like acoustic nodes • the scale plot fits beautifully to a theory … which gives the parameters •… and a problem 18 May 2006 M. Oreglia/ Linda Hall Library 33 Meanwhile, stargazers had a problem Not Newton Newton 18 May 2006 • 1990s: Vera Rubin and others measured the rotation speed of visible objects in galaxies and clusters • The results were not consistent with what we’d expect for a mass concentration in the center • There is a LOT of “dark” matter everywhere M. Oreglia/ Linda Hall Library 34 Another Indication of DM • This is supported by images made using x-rays • X-rays are coming from reqions of space where we did not expect there to be much matter 18 May 2006 M. Oreglia/ Linda Hall Library 35 Gravitational Lensing • Further evidence of some forms of Dark Matter are evident through telescopes • Light from some visible objects is distorted by the gravitational field of very heavy compact objects which are invisible (emit no visible light) 18 May 2006 M. Oreglia/ Linda Hall Library 36 Finally, Hubble redux: 18 May 2006 M. Oreglia/ Linda Hall Library 37 The expansion is accelerating! 18 May 2006 M. Oreglia/ Linda Hall Library 38 All the pieces fit! • When you assemble all the experimental evidence, the picture is consistent: – Flat universe – Accelerated expansion • Implies backgrnd E • What causes it? – Consistent with inflation • But a surprising measurement of the matter … 18 May 2006 M. Oreglia/ Linda Hall Library 39 The Embarassing Bottom Line 1. So 5/6ths of the matter is in a form unknown to us 2. Even worse: 74% of the energy in the universe is not in any of our theories!!! • We might already have a solution for #1 18 May 2006 M. Oreglia/ Linda Hall Library 40 Particle Physics Might Have a Solution • For a long time, particle physicists have felt that there should be partners of the currently known particles – This family of supersymmetric partners would provide a simple solution to some problems in the Standard Model theory – If they exist, they could have just the right qualities to be a candidate for the Dark Matter! – To solve the theory problems, some of them would have to have masses which the next generation of accelerators could see – Another theory posits Extra Dimensions • Suddenly particle physicists are popular again! 18 May 2006 M. Oreglia/ Linda Hall Library 41 SUSY • SuperSymmetry is an idea that has been around for decades • To solve some mathematical glitches in the Standard Model, propose the existence of a mirror family of partners to the current ones – The sparticles have oppposite properties of the particles, causing mathematical cancellations in the theory – The sparticles would have larger masses • And the sparticles could have the right properties to be the Dark Matter!!! 18 May 2006 M. Oreglia/ Linda Hall Library 42 2007: the Large Hadron Collider • To reach the energies needed to create SUSY particles, we need an accelerator capable of reaching the 1,000,000,000,000 volt range … the “TeV” range, or Terascale – We tried to build the SSC in Texas, but it became too expensive, so we are constructing a cheaper version in Geneva, Switzerland … the LHC – LHC will collide protons head-on, permitting them to sometimes annihilate into any particles … providing the products have masses satisfying mc2 is less than the collision energy • Online by end of 2007 18 May 2006 M. Oreglia/ Linda Hall Library 43 At 7.5xEFermilab, LHC is big! 18 May 2006 M. Oreglia/ Linda Hall Library 44 LHC Parameters • The protons are going so fast, it is difficult to build magnets that can bend them sharply – hence the large radius (27 km circumference) – Need 1232 magnets, each 14 m long ($300k ea) • Because the collision products have high energies, large detectors are required – Need lots of material to absorb energetic particles – Millions of electronic channels to measure the collisions – HUGE data rate – using GRID computing network 18 May 2006 M. Oreglia/ Linda Hall Library 45 The ATLAS Detector 18 May 2006 M. Oreglia/ Linda Hall Library 46 It will be in place next year 18 May 2006 M. Oreglia/ Linda Hall Library 47 Expect to see the new particles! • The energy and rate of LHC protons should produce the particles we are seeing hints of in earlier experiments and cosmology 18 May 2006 M. Oreglia/ Linda Hall Library 48 And After LHC? 18 May 2006 M. Oreglia/ Linda Hall Library 49 The ILC !!! • The International Linear Collider – Being planned now for construction next decade – A truly international project – By colliding electrons instead of protons, it will be much better than LHC for pinning down the properties of the new particles … and better at discovering some types of new particles Its been in the press recently and getting a lot of attention in Washington Also: realization that the US has fallen behind in scientific funding 18 May 2006 M. Oreglia/ Linda Hall Library 50 Epilogue • I hope I have convinced you: – We are in a new scientific revolution – Major discoveries will thrill us in the next few years • While the results are fascinating in and of themselves, we all benefit from this research in many ways – Education and cutting-edge technical training – Development of new industrial processes – … what the future brings…who knows! • Thank you, and the Linda Hall Library, for this opportunity! 18 May 2006 M. 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