Gravity from the Ground Up by Schutz, Bernard -- Read -- Imperial Library of Trantor

Index

Cover Half Title Title Page Copyright Dedication Contents Preface Background: what you need to know before you start 1. Gravity on Earth: the inescapable force

Galileo: the beginnings of the science of gravity The acceleration of gravity is uniform Trajectories of cannonballs Galileo: the first relativist

2. And then came Newton: gravity takes center stage

The second law: weight and mass The third law, and its loophole Preview: Newton’s gravity Action at a distance The new equivalence principle The gravitational redshift of light Gravity slows time Summing up

3. Satellites: what goes up doesn’t always come down

Taking motion apart Acceleration, and how to change your weight Getting into orbit

4. The Solar System: a triumph for Newtonian gravity

How to invent Newton’s law for the acceleration of gravity The orbits of the planets described by Newton’s law of gravity What is the value of G? Kepler’s laws The Sun has a little orbit of its own Geostationary satellites The gravitational attraction of spherical objects Playing with the orbit program Black holes before 1800 Light is deflected by the Sun’s gravity

5. Tides and tidal forces: the real signature of gravity

Tidal forces in free fall Ocean tides Tides from the Sun Spring and neap tides What the tidal forces do to the oceans, the Earth, and the Moon Tides elsewhere in astronomy Jupiter gives Mercury’s story another twist Triumph of Newtonian gravity: the prediction of Neptune Tiny flaw of Newtonian gravity: Mercury’s perihelion motion

6. Interplanetary travel: the cosmic roller-coaster

Getting away from the Earth Plain old momentum, and how rockets use it Energy, and how planets never lose it Getting to another planet The principle of the slingshot Using Jupiter to reach the outer planets Slinging towards the Sun Force and energy: how to change the energy of a body Time and energy

7. Atmospheres: keeping planets covered

In the beginning . . . . . . was the greenhouse . . . . . . and then came Darwin The ones that get away The Earth’s atmosphere Pressure beats gravity: Archimedes buoys up balloons Pressure beats gravity again: Bernoulli lifts airplanes Helium balloons and the equivalence principle Absolute zero: the coldest temperature of all Why there is a coldest temperature: the random nature of heat The ideal gas An atmosphere at constant temperature The Earth’s atmosphere The atmospheres of other planets Quantum theory and absolute zero

8. Gravity in the Sun: keeping the heat on

Sunburn shows that light comes in packets, called photons A gas made of photons Einstein in 1905 Gravity keeps the Sun round The Sun is one big atmosphere The Standard Model of the Sun The structure of the Sun How photons randomly ‘walk’ through the Sun Rotation keeps the Sun going around Solar seismology: the ringing Sun

9. Reaching for the stars: the emptiness of outer space

Leaping out of the Solar System How far away are the stars? How bright are stars? Astronomers’ units for brightness Standard candles: using brightness to measure distance

10. The colors of stars: why they are black (bodies)

The colors of stars Why stars are black bodies The color of a black body Relation between color and temperature: greenhouses again Spectral lines: the fingerprint of a star How big stars are: color and distance tell us the size But why are stars as hot as they are, and no hotter? Looking ahead

11. Stars at work: factories for the Universe

Star light, star bright . . . . . . first star I see tonight Cooking up the elements The solar neutrino problem Life came from the stars, but would you have bet on it?

12. Birth to death: the life cycle of the stars

Starbirth The gravitational thermostat The main sequence Giants Degenerate stars: what happens when the nuclear fire goes out The Chandrasekhar mass: white dwarfs can’t get too heavy Neutron stars Fire or ice: supernova or white dwarf Death by disintegration What is left behind: cinders and seeds

13. Binary stars: tidal forces on a huge scale

Looking at binaries The orbit of a binary Planetary perturbations Tidal forces in binary systems Accretion disks in binaries Compact-object binaries Fun with the three-body problem

14. Galaxies: atoms in the Universe

Globular clusters: minigalaxies within galaxies Describing galaxies Galaxies are speeding apart Measuring the Universe: the distances between galaxies Most of the Universe is missing! Gangs of galaxies The missing mass Radio galaxies: the monster is a giant black hole Quasars: feeding the monster Galaxy formation: how did it all start? Did it all start?

15. Physics at speed: Einstein stands on Galileo’s shoulders

Fast motion means relativity Relativity is special The Michelson-Morley experiment: light presents a puzzle Michelson’s interferometer: the relativity instrument Special relativity: general consequences The extra inertia of pressure Conclusions

16. Relating to Einstein: logic and experiment in relativity

Nothing can travel faster than light Light cannot be made to stand still Clocks run slower when they move The length of an object contracts along its motion Loss of simultaneity The mass of an object increases with its speed Energy is equivalent to mass Photons have zero rest-mass Consistency of relativity: the twin paradox saves the world Relativity and the real world

17. Spacetime geometry: finding out what is not relative

Gravity in general relativity is . . . . . . geometry Spacetime: time and space are inseparable Relativity of time in the spacetime diagram Time dethroned . . . . . . and the metric reigns supreme! The geometry of relativity Proper measures of time and distance Equivalence principle: the road to curvature . . . . . . is a geodesic The equivalence principle: spacetime is smooth

18. Einstein’s gravity: Einstein climbs onto Newton’s shoulders

Driving from Atlanta to Alaska, or from Cape Town to Cairo Dimpled and wiggly: describing any surface Newtonian gravity as the curvature of time Do the planets follow the geodesics of this time-curvature? How to define the conserved energy of a particle The deflection of light: space has to be curved, too Space curvature is a critical test of general relativity How Einstein knew he was right: Mercury’s orbital precession Weak gravity, strong gravity

19. Einstein’s recipe: fashioning the geometry of gravity

Einstein’s kitchen: the ingredients Einstein’s kitchen: the active gravitational mass comes first Einstein’s kitchen: the recipe for curving time Einstein’s kitchen: the recipe for curving space Einstein’s kitchen: the recipe for gravitomagnetism The geometry of gravitomagnetism Gyroscopes, Lense, Thirring, and Mach The cosmological constant: making use of negative pressure The big picture: all the field equations The search for simplicity General relativity Looking ahead

20. Neutron stars: laboratories of strong gravity

Nuclear pudding: the density of a neutron star It takes a whole star to do the work of 100 neutrons What would a neutron star look like? Where should astronomers look for neutron stars? Pulsars: neutron stars that advertise themselves The mystery of the way pulsars emit radiation The rotation rate of pulsars and how it changes Puzzles about the rotation of pulsars Pulsars in binary systems X-ray binary neutron stars Gamma-ray bursts: deaths of neutron stars? The relativistic structure of a neutron star The relation of mass to radius for neutron stars Neutron stars as physics labs

21. Black holes: gravity’s one-way street

The first black hole What black holes can do – to photons The gravitational redshift Danger: horizon! Getting away from it all Singularities, naked or otherwise What black holes can do . . . to orbits Making a black hole: the bigger, the easier Inside the black hole Disturbed black holes Limits on the possible The uniqueness of the black hole Spinning black holes drag everything with them The naked truth about fast black holes Mining the energy reservoir of a spinning black hole Accretion onto black holes The signature of the supermassive black hole in MCG-6-30-15 Wormholes: space and time tubes Hawking radiation: black holes are truly black bodies Black hole entropy: a link to nineteenth century physics Black hole entropy: a link to twenty-first century physics

22. Gravitational waves: gravity speaks

Gravitational waves are inevitable Transverse waves of tidal acceleration How gravitational waves act on matter Early confusion: are gravitational waves real? How gravitational waves are created Strength of gravitational waves Gravitational waves carry energy, lots of energy The Binary Pulsar: a Nobel-Prize laboratory Gravitational waves from binary systems Listening to black holes Gravitational collapse and pulsars Gravitational waves from the Big Bang: the Big Prize Catching the waves Michelson returns: the relativity instrument searches for waves LISA: catching gravitational waves in space

23. Gravitational lenses: bringing the Universe into focus

Pretty obvious, really, . . . . . . but not always easy How a gravitational lens works Why images get brighter Making multiple images: getting caustic about light The Einstein ring MACHOs grab the light The third image: the ghost in a mirror Lensing shows us the true size of quasars Weak lensing reveals strong gravity

24. Cosmology: the study of everything

What is “everything”? Copernican principle: “everything” is the same “everywhere” The Hubble expansion and the Big Bang The accelerating Universe Was there a Big Bang? Looking back nearly to the beginning Cosmic microwave background: echo of the Big Bang The rest frame of the Universe Big Crunch or Big Freeze: what happens next? Cosmology according to Newton Cosmology according to Einstein Evolving the Universe The cosmological scale-factor What is the cosmological expansion: does space itself expand? The age of the Universe

25. The Big Bang: the seed from which we grew

Physical cosmology: everything but the first nanosecond The expansion of the quark soup and its radiation The laws of physics prefer matter over anti-matter The Universe becomes ordinary Making helium: first steps toward life Does it correspond to reality? Three and only three neutrinos: a triumph for Big Bang physics From nuclei to atoms: the Universe goes transparent The evolution of structure Ghosts of the dark matter What is the dark matter?

26. Einstein’s Universe: the geometry of cosmology

Cosmology could be complicated . . . . . . but in fact it is simple (fortunately!) Gravity is geometry: what is the geometry of the Universe? Friedmann’s model universes What the Universe looks like

27. Ask the Universe: cosmic questions at the frontiers of gravity

The puzzle of the slightly lumpy Universe Einstein’s “big blunder” The cosmological constant in particle physics Inflation: a concept waiting for a theory Inflation power: the active vacuum Inflating the Universe Inflation put to the test Is inflation still going on? Is Einstein’s law of gravity simply wrong? Cosmic defects Cosmic rays Quantum gravity: the end of general relativity A Universe for life: the Anthropic Principle Causality in quantum gravity: we are all quantized The quantization of time? Time for the twenty-first century

Appendix Glossary Index

← Prev
Back
Next →

← Prev
Back
Next →