Origins of particle physics

Within the lifetime of my grandparents, there lived distinguished scientists who did not believe in atoms. Within the lifetime of my children, there lived distinguished scientists who did not believe in quarks. Although we can trace the notion of fundamental constituents of matter – minimal parts – to the ancients, the experimental reality of the atom is a profoundly modern achievement. The experimental reality of the quark is more modern still.

Through the end of the nineteenth century, controversy seethed over whether atoms were real material bodies or merely convenient computational fictions. The law of multiple proportions, the indivisibility of the elements, and the kinetic theory of gases supported the notion of real atoms, but a reasonable person could resist because no one had ever seen an atom. One of the founders of physical chemistry, Wilhelm Ostwald, wrote influential chemistry textbooks that made no use of atoms. The physicist, philosopher, and psychologist Ernst Mach likened “artificial and hypothetical atoms and molecules” to algebraic symbols – tokens, devoid of physical reality – that could be manipulated to answer questions about Nature.

What is a superfluid?

The word “superfluid” was coined to describe a qualitatively different state of a fluid that can occur at low temperatures, in which the resistance to flow is identically zero, so that flow round a closed path lasts for ever – a persistent current. Superfluidity can occur either for uncharged particles such as helium atoms or for charged particles such as the electrons in a metal. In the latter case the flow constitutes an electric current and we have a superconductor. Since an electric current is accompanied by a magnetic field, it is much easier to demonstrate the presence of a persistent current in a superconductor than in a neutral superfluid.

In this chapter I shall describe the properties of superfluids, starting with the simplest and working up to more complicated examples. But in this introductory section I shall depart from the historical order even further by turning to the last page of the detective story so as to catch a glimpse of the conclusion from almost a century of experimental and theoretical research; we shall then have an idea of where we are heading.

The conclusion is that superfluidity is more than just flow without resistance. It is an example of a transition to a more ordered state as the temperature is lowered, like the transition to ferromagnetism. At such a transition new macroscopically measurable quantities appear: in the case of a ferromagnet, the spontaneous magnetization. Such new measurable quantities are known as the order parameter of the low-temperature phase. The new quantities in the case of a superfluid are more subtle and more surprising: the amplitude and phase of the de Broglie wave associated with the motion of the superfluid particles. A superfluid can therefore exhibit quantummechanical effects on a macroscopic scale.

Introduction

This chapter describes remarkable new experiments that have been made possible through recent advances in laser cooling of atoms. Cooling of atoms in a gas by laser light is in itself surprising and this technique is important in a range of applications. In particular the experiments described here take atoms that have been laser cooled and then use other methods to reach even lower temperatures, at which wonderful and fascinating quantum effects occur. As well as revealing new phenomena, these experiments explore the deep analogies between the roles played by light waves in lasers and matter waves. These techniques are widely accessible and enable skilled researchers in laboratories all over the world to explore exciting new physics. The key physics and techniques of laser cooling are described in depth in Chapter 6.

What is “temperature”?

We use the words “cold” and “hot” every day; for example to refer to the temperature of the air outside. But what do “cold” and “hot” mean for the air’s molecules? Broadly speaking, we can say that atoms in a hot gas move faster than those in a cold gas and that cooling, by taking energy out of the gas, slows the atoms down. In this description of the gas as a collection of atoms behaving like billiard balls, or little hard spheres, the lowest possible temperature occurs when the atoms stop moving but, as we shall see, this picture does not give an accurate description at very low energies, for which quantum effects become important. In this chapter we will look at the fascinating properties of atomic gases cooled to temperatures within one millionth of a degree Kelvin from absolute zero. We shall use the term “ultra-cold” to refer to such extremely low temperatures that have only recently been achieved in experiments on atomic gases. The techniques used to cool liquids and solids have a longer history and have made available a different set of possibilities (see Chapter 8). Note that most of this chapter refers to gases in which the individual particles are atoms, but the general statements about temperature scales apply equally well to gases of molecules, e.g. air, whose major constituents, oxygen and nitrogen, exist as diatomic molecules.

The attraction of gravity

Gravity attracts. It attracts every body in the Universe to every other, and it has attracted the interest of physicists for centuries. It was the first fundamental force to be understood mathematically in Isaac Newton’s action-at-a-distance theory, it is a center of current attention in Albert Einstein’s general relativity theory, and it promises to be the last force to be fully understood and integrated with the rest of physics.

After centuries of success, Newton’s theory was finally replaced by Einstein’s theory, which describes gravity at a deeper level as due to curvature of spacetime. General relativity is widely considered to be the most elegant physical theory and one of the most profound. It has allowed the study and understanding of gravitational phenomena ranging from laboratory scale to the cosmological scale – the entire Universe; but many mysteries remain, especially in cosmology.

An impressive understanding of the other fundamental forces of nature, electromagnetism and the weak and strong nuclear forces, is now embodied in the Standard Model of elementary particles. However, these other forces are understood in terms of quantum field theory and are not geometric in the manner of general relativity, so gravity remains apart. Many physicists believe that the final phase of understanding gravity will be to include quantum effects and form a union of general relativity and the Standard Model. We would then understand all the forces and spacetime on a fundamental quantum level. This is proving to be quite a task.

Introduction

Electromagnetic interactions play a central role in low-energy physics, chemistry, and biology. They are responsible for the cohesion of atoms and molecules and are at the origin of the emission and absorption of light by such systems. They can be described in terms of absorptions and emissions of photons by charged particles or by systems of charged particles like atoms and molecules. Photons are the energy quanta associated with a light beam. Since the discoveries of Planck and Einstein at the beginning of the last century, we know that a plane light wave with frequency ν, propagating along a direction defined by the unit vector u, can also be considered as a beam of photons with energy E = hν and linear momentum p = (hν/c)u. We shall see later on that these photons also have an angular momentum along u depending on the polarization of the associated light wave.

Conservation laws are very useful for understanding the consequences of atom–photon interactions. They express that the total energy, the total linear momentum, and the total angular momentum are conserved when the atom emits or absorbs a photon. Consider for example the conservation of the total energy. Quantum mechanics tells us that the energy of an atom cannot take any value. It is quantized, the possible values of the energy forming a discrete set Ea, Eb, Ec, . . . In an emission process, the atom goes from an upper energy level Eb to a lower one Ea and emits a photon with energy hν. Conservation of the total energy requiresThe energy lost by the atom on going from Eb to Ea is carried away by the photon.

Introduction

Ever since physics came into existence as a scientific discipline, it has been mainly concerned with identifying a minimal set of fundamental laws connecting a minimal number of different constituents, under the more or less implicit assumption that knowledge of these rules were a sufficient condition for explaining the world we live in. Such a program has had remarkable success, to the extent that processes occurring on scales that range from that of elementary particles up to those of stellar evolution can nowadays be satisfactorily described. Nevertheless, it has meanwhile become clear that the inverse approach is a source of unexpected richness and can hardly be included with the original microscopic equations. The existence of different phases of matter (gas, liquid, solid, and plasma, together with perhaps glasses, granular materials, and Bose–Einstein condensates) provides the most striking evidence that the adjustment of a parameter (e.g. temperature) can dramatically change the organization of the system.

Moreover, not only can the same set of microscopic laws give rise to different structures, but also the converse is true: different systems can, for example, converge toward the same crystalline configuration. One of the basic ingredients that makes the connection between different levels of description complex, though very intriguing, is the presence of nonlinearities. As long as each atom deviates slightly from its equilibrium position, the equations of motion can be linearized and the dynamics thereby decomposed into the sum of independent evolutions of so-called normal modes. In some cases, especially when disorder is present, such a decomposition cannot be easily performed (and very interesting physics can indeed arise, e.g. Anderson localization) but is, at least in principle, feasible.

Introduction

The atomic nature of matter is well documented and appreciated. Solids are made from regular (in the case of crystals) or irregular (for the example of glasses) arrangements of atoms. Nature finds a way to produce various materials by combining constituent atoms into a macroscopic substance.

Imagine the following hypothetical experiment. Suppose that one builds up, for example, a crystal of silicon by starting with a single atom and adding atoms to make a small number of unit cells, repeating the process until a large enough crystallite has formed. A fundamental question is the following: at what stage in this process, i.e. at what size of the crystallite, will it approximately acquire the “bulk” properties? The precise answer to this question may well depend on what exactly one intends to do with the crystal.

While this may sound like a purely thought experiment, remarkable modern fabrication methods are close to being able to achieve this, using at least two independent approaches. Molecular-beam epitaxy (Figure 12.1) is able to grow high-quality crystalline layers one by one with remarkable control. Atomic-resolution methods are already able to deposit atoms selectively on some surfaces (Figure 12.2).

How it all began

In 1935, a decade after the invention of quantum theory by Heisenberg (1925) and Schrödinger (1926), three papers appeared, setting the stage for a new concept, quantum entanglement. The previous decade had already seen momentous discussions on the meaning of the new theory, for example by Niels Bohr (see his contribution to Albert Einstein: Philosopher-Scientist in Further reading); but these new papers opened up the gates for a new, very deep philosophical debate about the nature of reality, about the role of knowledge, and about their relation. Since the 1970s, it has become possible for experimenters to observe entanglement directly in the laboratory and thus test the counter-intuitive predictions of quantum mechanics whose confirmation today is beyond reasonable doubt. Since the 1990s, the conceptual and experimental developments have led to new concepts in information technology, including such topics as quantum cryptography, quantum teleportation, and quantum computation, in which entanglement plays a key role.

In the first of the three papers, Einstein, Podolsky, and Rosen (EPR) realized that, if two particles had interacted in their past, their properties will remain connected in the future in a novel way, namely, observation on one determines the quantum state of the other, no matter how far away. Their conclusion was that quantum mechanics is incomplete and they expressed their belief that a more complete theory may be found. Niels Bohr replied that the two systems may never be considered independent of each other, and observation on one changes the possible predictions on the other. Finally, Erwin Schrödinger, in the paper which also proposed his famous cat paradox, coined the term “entanglement” (in German Verschränkung) for the new situation and he called it “not one, but the essential trait of the new theory, the one which forces a complete departure from all classical concepts.”

Introduction

The application of basic physics ideas to the study of biological molecules is one of the major growth areas of modern physics, and emphasizes well how physics principles ultimately underpin the whole of Nature. This chapter focuses on the collective properties of biological molecules showing examples of hierarchical structures, and, in some instances, how structure and dynamics enable biological function. In addition, supramolecular biophysics casts a wide web with contributions to a broad range of fields. Among them are, in medicine and genetics, the design of carriers of large pieces of DNA containing genes for gene therapy and for characterizing chromosome structure and function; in molecular neurosciences, elucidating the structure and dynamics of the nerve-cell cytoskeleton; and in molecular cell biology, characterizing the forces responsible for condensation of DNA in vivo, to name a few. Concepts and new materials emerging from research in the field continue to have a large impact in industries as diverse as cosmetics and optoelectronics. A separate branch of biophysics dealing with the properties of single molecules is not described here due to space limitations and the availability of excellent reviews published in the past few years.

If one looks at research in biophysics over the last few decades one finds that a large part has been dedicated to studies of the structure and phase behavior of biological membranes. Membranes of living organisms are astoundingly complex structures, with the lipid bilayer containing membrane-protein inclusions and carbohydrate-chain decorations as shown in a cartoon of a section of the plasma membrane of a eukaryotic cell, which separates the interior contents of the cell from the region outside of the cell (Figure 16.1). The common lipids in membranes are amphiphilic molecules, meaning that the molecules contain both hydrophilic (“water-liking”) polar head groups and hydrophobic (“water-avoiding”) double tail hydrocarbon chains. Plasma membranes contain a large number of distinct membrane-associated proteins, which may traverse the lipid bilayer, be partially inserted into the bilayer, or interact with the membrane but not penetrate the bilayer.

Introduction

Computation is an operation on symbols. We tend to perceive symbols as abstract entities, such as numbers or letters from a given alphabet. However, symbols are always represented by selected properties of physical objects. The binary string

1. 10011011010011010110101101

may represent an abstract concept, such as the number 40 711 597, but the binary symbols 0 and 1 have also a physical existence of their own. It could be ink on paper (this is most likely to be how you see them when you are reading these words), glowing pixels on a computer screen (this is how I see them now when I am writing these words), or different charges or voltages (this is how my word processor sees them). If symbols are physical objects and if computation is an operation on symbols then computation is a physical process. Thus any computation can be viewed in terms of physical experiments, which produce outputs that depend on initial preparations called inputs. This sentence may sound very innocuous but its consequences are anything but trivial!

On the atomic scale matter obeys the rules of quantum mechanics, which are quite different from the classical rules that determine the properties of conventional computers. Today’s advanced lithographic techniques can etch logic gates and wires less than a micrometer across onto the surfaces of silicon chips. Soon they will yield even smaller parts and inevitably reach a point at which logic gates are so small that they are made out of only a handful of atoms. So, if computers are to become smaller in the future, new, quantum technology must replace or supplement what we have now. The point is, however, that quantum technology can offer much more than cramming more and more bits onto silicon and multiplying the clock-speed of microprocessors. It can support an entirely new kind of computation, known as quantum computation, with qualitatively new algorithms based on quantum principles.

What is the future of astronomy education worldwide? How can astronomers and astronomy educators ensure that the future will be a positive one? A few years ago, one of us was invited to write an article on the topic of the first question (Percy, 1996). The article also addressed the second question, but it ended as follows:

Fortunately, many of the characteristics of this “alternate future” do not appear to be developing – yet. But there are negative developments. Belief in pseudosciences, such as astrology, creationism, and space aliens, is widespread, and is not decreasing, as both Jayant Narlikar, and John Percy and Jay Pasachoff, have explained. Astronomical misconceptions, of many kinds, continue to abound. Astronomy is poorly taught, if it is taught at all, in many schools. The scientific enterprise appears to be maintained by a small fraction of the population.

An overview of IAU Commission 46: “Astronomy Education and Development”

The International Astronomical Union (IAU) is a union of professional astronomers who produce a large number of new astronomical results and make the frontiers of astronomy expand. However, the union cannot stand by itself but needs much support from governments as well as from the public. Therefore, the IAU established Commission 46 through the vigorous efforts of E. Schatzman, and others. In 1967 it was originally called “Teaching of Astronomy” and was renamed in 2000 “Astronomy Education and Development,” with a much wider scope of activities, in order to cover from the level of beginners to that of doctoral and post-doctoral students. Table 21.1 gives a list of its presidents; they are well distributed internationally.

There are currently nine “program groups,” as shown in Table 21.2. Because of limited budgetary resources, it is difficult for the IAU to cover all the possible fields to promote our Commission's goals.

Introduction

Scientists occasionally lament the low public interest in science and the falling level of scientific literacy in the public. However, public surveys continually demonstrate that public interest is high, and although we might not be happy with the current level of scientific literacy, it is, if anything, on the rise (albeit marginally).

In the classical study by Durant and Evans (1989), more than 80 per cent of the respondents professed (a high or moderate) interest in science. A survey in Norway by Eide and Ottosen (1994) found that “as many as 37 per cent of the readers regularly read science articles presented in newspapers.” Other researchers using various indicators report significantly higher self-reported interest in science, although there is a strong subject dependency.

Recently, Eurobarometer (European Commission 2001), the survey carried out on behalf of the European Commission in the 15 member-states of the European Union (later augmented by a similar survey in those countries that since joined the Union), looked at attitudes towards and knowledge about science.

While the Dipper may rule the sky of spring and early summer, different stars and new opportunities await the sky's watchers in late summer and fall.

High in the western sky is the “Summer Triangle” of Vega, Deneb, and Altair, leading their respective constellations of Lyra the Harp, Cygnus the Swan, and Aquila the Eagle. To the east of the Triangle flies the square of Pegasus, the winged horse. I have never thought this asterism looks much like a horse, let alone the kind that flies, but its four bright stars do resemble a baseball diamond. You can easily spot home plate and the bases, while the Milky Way to the north represents the fans in the stadium. A little further to the east is Andromeda the Princess, and Perseus.

We now focus on Beta Persei. In 1603, Johann Bayer published a star atlas in which stars in the different constellations were given Greek letters in approximate order of brightness. Many stars are numbered instead, according to John Flamsteed's 1725 catalog, which used increasing numbers from west to east in each constellation.

Beta Persei, the demon star of mythology, is more commonly known as Algol, the star that winks! Every 2.9 days, or 69 hours, Algol drops in brightness by a full magnitude for about ten hours. It is one of the finest examples of a celestial event: a star that is not just there, but is visibly doing something for all to see.