MICHAEL ANDRIESSEN • PETER PENTLAND
RICHARD GAUT • BRUCE McKAY • JILL TACON
Third edition published 2008 by John Wiley & Sons Australia, Ltd 42 McDougall Street, Milton, Qld 4064 Typeset in 10.5/12pt New Baskerville
© Michael Andriessen, Peter Pentland, Richard Gaut, Bruce McKay, Jillian Tacon and Upgrade Business Systems (Ric Morante) 2008 First edition published 2001
© Michael Andriessen, Peter Pentland, Richard Gaut and Bruce McKay 2001
Second edition published 2003
© Michael Andriessen, Peter Pentland, Richard Gaut, Bruce McKay and Jillian Tacon 2003
The moral rights of the authors have been asserted. National Library of Australia
Cataloguing-in-Publication data
Title: Physics 2 HSC course/Michael Andriessen ... [et al.].
Edition: 3rd ed.
ISBN: 978 0 7314 0823 8 (pbk.)
Notes: Includes index.
Target audience: For secondary school age. Subjects: Physics — Textbooks. Other authors/contributors: Andriessen, Michael.
Dewey number: 530
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CONTENTS
Preface viiiAbout eBookPLUS ix Syllabus grid x Acknowledgements xvi
Chapter 1: Earth‘s gravitational field 2
1.1 The Earth’s gravity 31.2 Weight 6
1.3 Gravitational potential energy 7 Summary 10
Questions 10
Practical activities 11
Chapter 2: Launching into space 13
2.1 Projectile motion 14 2.2 Escape velocity 23 2.3 Lift-off 24 Summary 33 Questions 33 Practical activities 35Chapter 3: Orbiting and re-entry 38
3.1 In orbit 393.2 Re-entry 50 Summary 56 Questions 56
Practical activities 58
Chapter 4: Gravity in the solar system 60
4.1 The Law of Universal Gravitation 614.2 Gravitational fields 65 4.3 The slingshot effect 66 Summary 70
Questions 70
Chapter 5: Space and time 71
5.1 The aether model 725.2 Special relativity 74
5.3 Consequences of special relativity 77 Summary 93
Questions 93
Practical activities 96
Chapter 6: The motor effect and DC electric motors 100
6.1 The motor effect 1036.2 Forces between two parallel conductors 105 6.3 Torque 107 6.4 DC electric motors 109 Summary 116 Questions 116 Practical activities 120
HSC CORE MODULE
Space
HSC CORE MODULE
Motors and
generators
iv
Chapter 7: Generating electricity
122
7.1 The discoveries of Michael Faraday 123 7.2 Electromagnetic induction 126 7.3 Generating a potential difference 127 7.4 Lenz’s law 128
7.5 Eddy currents 131
Summary 134
Questions 134
Practical activities 137
Chapter 8: Generators and power distribution
139
8.1 Generators 140
8.2 Electric power generating stations 146 8.3 Transformers 148
8.4 Power distribution 151 8.5 Electricity and society 156
Summary 157
Questions 157
Practical activities 160
Chapter 9: AC electric motors
163
9.1 Main features of an AC motor 164 9.2 Energy transformations and transfers 169
Summary 171
Questions 171
Practical activities 172
Chapter 10: Cathode rays and
the development of television
174
10.1 The discovery of cathode rays 175
10.2 Effect of electric fields on cathode rays 177 10.3 Effect of magnetic fields on cathode rays 182
10.4 Determining the charge-to-mass ratio of cathode rays 183 10.5 Cathode rays — waves or particles? 184
10.6 Applications of cathode rays 186
Summary 189
Questions 189
Practical activities 191
Chapter 11: The photoelectric
effect and black body radiation
193
11.1 Maxwell’s theory of electromagnetic waves 194 11.2 Heinrich Hertz and experiments with radio waves 196 11.3 The black body problem and the ultraviolet catastrophe 199 11.4 What do we mean by ‘classical physics’ and ‘quantum theory’? 202 11.5 The photoelectric effect 202
Summary 209 Questions 209 Practical activities 211
HSC CORE MODULE
From ideas to
implementation
v
Chapter 12: The development
and application of transistors
212
12.1 Conductors, insulators and semiconductors 213 12.2 Band structures in semiconductors 216 12.3 Doping and band structure 219 12.4 Thermionic devices 220 12.5 Solid state devices 222
12.6 Thermionic versus solid state devices 224 12.7 Invention of the transistor 225
12.8 Integrated circuits 227 Summary 230 Questions 230 Practical activities 231
Chapter 13: Superconductivity
232
13.1 Interference 233 13.2 Diffraction 235 13.3 X-ray diffraction 235 13.4 Bragg’s experiment 23813.5 The crystal lattice structure of metals 239 13.6 Superconductivity 240
13.7 How is superconductivity explained? 243
Summary 251
Questions 251
Practical activities 253
Chapter 14: Looking and seeing
256
14.1 Galileo’s telescopes 25714.2 Atmospheric absorption of the electromagnetic spectrum 258 14.3 Telescopes 261
14.4 Seeing 265
14.5 Modern methods to improve telescope performance 265
Summary 270
Questions 270
Practical activities 272
Chapter 15: Astronomical measurement
274
15.1 Astrometry 275 15.2 Spectroscopy 279 15.3 Photometry 289 Summary 299 Questions 299 Practical activities 302Chapter 16: Binaries and variables
305
16.1 Binaries 306 16.2 Variables 312 Summary 316 Questions 316 Practical activities 318HSC OPTION MODULE
Astrophysics
vi
Chapter 17: Star lives
320
17.1 Star birth 32117.2 Main sequence star life 324
17.3 Star life after the main sequence 327 17.4 Star death 332
Summary 336
Questions 336
Practical activities 338
Chapter 18: The use of ultrasound in medicine
340
18.1 What type of sound is ultrasound? 34118.2 Using ultrasound to detect structure inside the body 343 18.3 Producing and detecting ultrasound: the piezoelectric effect 347 18.4 Gathering and using information in an ultrasound scan 348 18.5 Using ultrasound to examine blood flow 352
Summary 358
Questions 358
Chapter 19: Electromagnetic
radiation as a diagnostic tool
361
19.1 X-rays in medical diagnosis 36219.2 CT scans in medical diagnosis 368 19.3 Endoscopes in medical diagnosis 373
Summary 378
Questions 378
Practical activities 380
Chapter 20: Radioactivity as a diagnostic tool
381
20.1 Radioactivity and the use of radioisotopes 38220.2 Positron emission tomography (PET) 392 20.3 Imaging methods working together 394
Summary 396
Questions 396
Chapter 21: Magnetic resonance
imaging as a diagnostic tool
398
21.1 The patient and the image using MRI 39921.2 The MRI machine: effect on atoms in the patient 402 21.3 Medical uses of MRI 410
21.4 Comparison of the main imaging techniques 412
Summary 415
Questions 415
Chapter 22: The atomic models of Rutherford and Bohr
418
22.1 The Rutherford model of the atom 41922.2 Bohr’s model of the atom 423 22.3 Bohr’s postulates 427
22.4 Mathematics of the Rutherford and Bohr models 429 22.5 Limitations of the Bohr model of the atom 434
Summary 435 Questions 435 Practical activities 437
HSC OPTION MODULE
Medical physics
HSC OPTION MODULE
From quanta
to quarks
vii
Chapter 23: Development of quantum mechanics
440
23.1 Diffraction 44123.2 Steps towards a complete quantum theory model of the atom 444
Summary 452
Questions 452
Chapter 24: Probing the nucleus
453
24.1 Discoveries pre-dating the nucleus 454 24.2 Discovery of the neutron 45824.3 Discovery of the neutrino 461 24.4 The strong nuclear force 466
24.5 Mass defect and binding energy of the nucleus 468
Summary 472
Questions 472
Chapter 25: Nuclear fission
and other uses of nuclear physics
474
25.1 Energy from the nucleus 47525.2 The discovery of nuclear fission 476 25.3 The development of the atom bomb 480 25.4 Nuclear fission reactors 484
25.5 Medical and industrial applications of radioisotopes 489 25.6 Neutron scattering 492
Summary 493
Questions 493
Chapter 26: Quarks and the
Standard Model of particle physics
495
26.1 Instruments used by particle physicists 496 26.2 The Standard Model of particle physics 503Summary 516
Questions 516
Practical activities 518 Glossary 521
Appendix 1: Formulae and data sheet 526 Appendix 2: Periodic table 528
Appendix 3: Key words for examination questions 529 Answers to numerical questions 531
viii
PREFACE
This third edition of Physics 2: HSC Course is revised and updated to meet all the requirements of the amended Stage 6 Physics Syllabus for Year 12 students in New South Wales. Written by a team of experienced Physics teachers, Physics 2 offers a complete resource with coverage of the three core modules as well as three option modules: Quanta to Quarks, Astro-physics and Medical Physics. An additional option topic, The Age of Silicon, is available online.
Physics 2 features:
• full-colour, high-quality, detailed illustrations to enhance students’ understanding of Physics concepts
• clearly written explanations and sample problems
• interest boxes focusing on up-to-date information, current research and new discoveries
• practical activities at the end of each chapter to support the syllabus investigations
• key terms highlighted and defined in the context of the chapters and in a complete glossary
• chapter reviews that provide a summary and a range of problem-solving and descriptive questions.
Next generation teaching and learning
This title features eBookPLUS: an electronic version of the textbook and a complementary set of targeted digital resources. These flexible and engaging ICT activities are available online at the JacarandaPLUS website (www.jacplus.com.au).
eBookPLUS icons within the text direct students to the online resources, which include:
• eModelling: Excel spreadsheets that provide examples of numerical and algebraic modelling
• eLessons: Video and animations that reinforce study by bringing key concepts to life
• Interactivities: Interactive study activities that enhance student under-standing of key concepts through hands-on experience
• Weblinks: HTML links to other useful support material on the internet.
eBookplus
ix
Next generation teaching and learning
About eBookPLUS
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x
SYLLABUS GRID
Core module: SPACE (chapters 1–5, pages 1–98)
1. The Earth has a gravitational field that exerts a force on objects both on it and around it
Students learn to:
• define weight as the force on an object due to a gravitational field • explain that a change in gravitational potential energy is related to work
done
• define gravitational potential energy as the work done to move an object from a very large distance away to a point in a gravitational field
page 8 7 7–9
Students:
• perform an investigation and gather information to determine a value for acceleration due to gravity using pendulum motion or computer- assisted technology and identify reasons for possible variations from the value
9.8 m s−2
• gather secondary information to predict the value of acceleration due to gravity on other planets
• analyse information using the expression F = mg to determine the weight force for a body on Earth and for the same body on other planets
page 11 5, 10, 12 6, 10, 12
2. Many factors have to be taken into account to achieve a successful rocket launch, maintain a stable orbit and return to Earth
Students learn to:
• describe the trajectory of an object undergoing projectile motion within the Earth’s gravitational field in terms of horizontal and vertical components
• describe Galileo’s analysis of projectile motion • explain the concept of escape velocity in terms of the:
– gravitational constant – mass and radius of the planet
• outline Newton’s concept of escape velocity
• identify why the term ‘g forces’ is used to explain the forces acting on an astronaut during launch
• discuss the effect of the Earth’s orbital motion and its rotational motion on the launch of a rocket
• analyse the changing acceleration of a rocket during launch in terms of the:
– Law of Conservation of Momentum – forces experienced by astronauts
• analyse the forces involved in uniform circular motion for a range of objects, including satellites orbiting the Earth
• compare qualitatively low Earth and geo-stationary orbits • define the term orbital velocity and the quantitative and qualitative
relationship between orbital velocity, the gravitational constant, mass of the central body, mass of the satellite and the radius of the orbit using Kepler’s Law of Periods
• account for the orbital decay of satellites in low Earth orbit
• discuss issues associated with safe re-entry into the Earth’s atmosphere and landing on the Earth’s surface
• identify that there is an optimum angle for safe re-entry for a manned spacecraft into the Earth’s atmosphere and the consequences of failing to achieve this angle
page 14–23 14 23–4 23 26–31 31–2 25, 26–7 (see also 36–7) 39–41 47–8 41–4 49–50 50–5 51 Students:
• solve problems and analyse information to calculate the actual velocity of a projectile from its horizontal and vertical components using:
vx 2 = ux2 v = u + at vy 2 = uy2 + 2ay∆y ∆x = uxt ∆y = uyt + ayt 2
• perform a first-hand investigation, gather information and analyse data to calculate initial and final velocity, maximum height reached, range and time of flight of a projectile for a range of situations by using simulations, data loggers and computer analysis
• identify data sources, gather, analyse and present information on the contribution of one of the following to the development of space exploration: Tsiolkovsky, Oberth, Goddard, Esnault-Pelterie, O’Neill or von Braun
• solve problems and analyse information to calculate the centripetal force acting on a satellite undergoing uniform circular motion about the Earth using
• solve problems and analyse information using:
page 19–22, 33–4 35 32 40–1, 56, 58–9 42–4, 56–7
3. The Solar System is held together by gravity
Students learn to:
• describe a gravitational field in the region surrounding a massive object in terms of its effects on other masses in it
• define Newton’s Law of Universal Gravitation
• discuss the importance of Newton’s Law of Universal Gravitation in understanding and calculating the motion of satellites
• identify that a slingshot effect can be provided by planets for space probes page 65–6 61–2 62–5 66–9 Students:
• present information and use available evidence to discuss the factors affecting the strength of the gravitational force
• solve problems and analyse information using
page 61–4, 70 61–2, 70
4. Current and emerging understanding about time and space has been dependent upon earlier models of the transmission of light
Students learn to:
• outline the features of the aether model for the transmission of light • describe and evaluate the Michelson-Morley attempt to measure the
relative velocity of the Earth through the aether
• discuss the role of the Michelson-Morley experiments in making determinations about competing theories
• outline the nature of inertial frames of reference • discuss the principle of relativity
• describe the significance of Einstein’s assumption of the constancy of the speed of light
• identify that if c is constant then space and time become relative • discuss the concept that length standards are defined in terms of time in
contrast to the original metre standard
page 72 72–4 74 74–5 74–5 75–6 76 77 Students:
• gather and process information to interpret the results of the Michelson-Morley experiment
• perform an investigation to help distinguish between non-inertial and inertial frames of reference
• analyse and interpret some of Einstein’s thought experiments involving mirrors and trains and discuss the relationship between thought and reality
• analyse information to discuss the relationship between theory and the evidence supporting it, using Einstein’s predictions based on relativity that were made many years before evidence was available to support it
(continued) page 96–7 97–8 75–6, 77–8 80–1 Ep Gm1m2 r ---– = 1 2 ---F mv 2 r ---= r3 T2 --- GM 4π2 ---= F Gm1m2 d2 ---= F Gm1m2 d ---=
xi
Core module: MOTORS AND GENERATORS (chapters 6–9, pages 101–72)
• explain qualitatively and quantitatively the consequence of special relativity in relation to:
– the relativity of simultaneity
– the equivalence between mass and energy – length contraction
– time dilation – mass dilation
• discuss the implications of mass increase, time dilation and length contraction for space travel
77–8 88–9 81–4 78–9 85–8 89–92
• solve problems and analyse information using:
89, 95 84, 94–5 81, 94–5 88, 95
1. Motors use the effect of forces on current-carrying conductors in magnetic fields
Students learn to:
• discuss the effect on the magnitude of the force on a current-carrying conductor of variations in:
– the strength of the magnetic field in which it is located – the magnitude of the current in the conductor – the length of the conductor in the external magnetic field – the angle between the direction of the external magnetic field and
the direction of the length of the conductor
• describe qualitatively and quantitatively the force between long parallel current-carrying conductors:
• define torque as the turning moment of a force using: τ = Fd • identify that the motor effect is due to the force acting on a
current-carrying conductor in a magnetic field
• describe the forces experienced by a current-carrying loop in a magnetic field and describe the net result of the forces
• describe the main features of a DC electric motor and the role of each feature
• identify that the required magnetic fields in DC motors can be produced either by current-carrying coils or permanent magnets
page 104–5 105–7 107–8 104–5 102–3 109–11 109–11, 112 Students:
• solve problems using:
• perform a first-hand investigation to demonstrate the motor effect • solve problems and analyse information about the force on
current-carrying conductors in magnetic fields using
• solve problems and analyse information about simple motors using: • identify data sources, gather and process information to qualitatively
describe the application of the motor effect in: – the galvanometer – the loudspeaker page 107, 117–19 120 105, 117–19 114, 118–19, 121 114–15
2. The relative motion between a conductor and magnetic field is used to generate an electrical voltage
Students learn to:
• outline Michael Faraday’s discovery of the generation of an electric current by a moving magnet
• define magnetic field strength B as magnetic flux density
• describe the concept of magnetic flux in terms of magnetic flux density and surface area
• describe generated potential difference as the rate of change of magnetic flux through a circuit
• account for Lenz’s Law in terms of conservation of energy and relate it to the production of back emf in motors
• explain that, in electric motors, back emf opposes the supply emf • explain the production of eddy currents in terms of Lenz’s Law
page 123–6 126 126–7 127–8 128–30 129–30 131–2 Students:
• perform an investigation to model the generation of an electric current by moving a magnet in a coil or a coil near a magnet
• plan, choose equipment or resources for, and perform a first-hand investigation to predict and verify the effect on a generated electric current when:
– the distance between the coil and the magnet is varied – the strength of the magnet is varied
– the relative motion between the coil and the magnet is varied • gather, analyse and present information to explain how induction is used
in cooktops in electric ranges
• gather secondary information to identify how eddy currents have been utilised in electromagnetic braking
page 137–8 137–8 133 132
3. Generators are used to provide large-scale power production
Students learn to:
• describe the main components of a generator • compare the structure and function of a generator to an
electric motor
• describe the differences between AC and DC generators • discuss the energy losses that occur as energy is fed through
transmission lines from the generator to the consumer • assess the effects of the development of AC generators on society
and the environment
page 140–1 141, 109, 164–5 142–5 151–4 147–8, 156 Students:
• plan, choose equipment or resources for, and perform a first-hand investigation to demonstrate the production of an alternating current • gather secondary information to discuss advantages and disadvantages of
AC and DC generators and relate these to their use
• analyse secondary information on the competition between Westinghouse and Edison to supply electricity to cities
• gather and analyse information to identify how transmission lines are: – insulated from supporting structures
– protected from lightning strikes
page 160–1 160 147–8 154–5
4. Transformers allow generated power to be either increased or decreased before it is used
Students learn to:
• describe the purpose of transformers in electrical circuits • compare step-up and step-down transformers
• identify the relationship between the ratio of the number of turns in the primary and secondary coils and the ratio of primary to secondary voltage
• explain why voltage transformations are related to conservation of energy
• explain the role of transformers in electricity sub-stations
• discuss why some electrical appliances in the home that are connected to the mains domestic power supply use a transformer
• discuss the impact of the development of transformers on society
page 148–9 149 149–50 149–50 154 148–9, 153 152–3, 156 Students:
• perform an investigation to model the structure of a transformer to demonstrate how secondary voltage is produced
• solve problems and analyse information about transformers using: • gather, analyse and use available evidence to discuss how difficulties of
heating caused by eddy currents in transformers may be overcome • gather and analyse secondary information to discuss the need for
transformers in the transfer of electrical energy from a power station to its point of use page 160–1 150–1 151 152–4, 162 E= mc2 lv l0 1 v 2 c2 ---– = tv t0 1 v 2 c2 ---– ---= mv m0 1 v 2 c2 ---– ---= F l -- kI1I2 d ---= F l -- kI1I2 d ---= F =BIlsinθ τ = nBIAcosθ Vp Vs --- np ns ---=
xii
Core module: FROM IDEAS TO IMPLEMENTATION (chapters 10–13, pages 173–254)
5. Motors are used in industries and the home usually to convert electrical energy into more useful forms of energy
Students learn to:
• describe the main features of an AC electric motor
page 164–9
Students:
• perform an investigation to demonstrate the principle of an AC induction motor
• gather, process and analyse information to identify some of the energy transfers and transformations involving the conversion of electrical energy into more useful forms in the home and industry
page 172 169–70
1. Increased understanding of cathode rays led to the development of television
Students learn to:
• explain why the apparent inconsistent behaviour of cathode rays caused debate as to whether they were charged particles or electromagnetic waves
• explain that cathode ray tubes allowed the manipulation of a stream of charged particles
• identify that moving charged particles in a magnetic field experience a force
• identify that charged plates produce an electric field
• describe quantitatively the force acting on a charge moving through a magnetic field
• discuss qualitatively the electric field strength due to a point charge, positive and negative charges and oppositely charged parallel plates • describe quantitatively the electric field due to oppositely charged
parallel plates
• outline Thomson’s experiment to measure the charge : mass ratio of an electron
• outline the role of:
– electrodes in the electron gun – the deflection plates or coils
– the fluorescent screen in the cathode ray tube of conventional TV displays and oscilloscopes
page 184–5 175–6 182 177–9 182 177–9 177–9 183 186–8 Students:
• perform an investigation and gather first-hand information to observe the occurrence of different striation patterns for different pressures in discharge tubes
• perform an investigation to demonstrate and identify properties of cathode rays using discharge tubes:
– containing a Maltese cross – containing electric plates – with a fluorescent display screen – containing a glass wheel
– analyse the information gathered to determine the sign of the charge on cathode rays
• solve problems and analyse information using: and page 191 192 178, 181, 182, 189–90
2. The reconceptualisation of the model of light led to an understanding of the photoelectric effect and black body radiation
Students learn to:
• describe Hertz’s observation of the effect of a radio wave on a receiver and the photoelectric effect he produced but failed to investigate • outline qualitatively Hertz’s experiments in measuring the speed of
radio waves and how they relate to light waves
• identify Planck’s hypothesis that radiation emitted and absorbed by the walls of a black body cavity is quantised
• identify Einstein’s contribution to quantum theory and its relation to black body radiation
• explain the particle model of light in terms of photons with particular energy and frequency
• identify the relationships between photon energy, frequency, speed of
light and wavelength: E = hf and c = f λ
page 196–8, 202–3 196–8 199–201 205 204 201– 5 Students:
• perform an investigation to demonstrate the production and reception of radio waves
• identify data sources, gather, process and analyse information and use available evidence to assess Einstein’s contribution to quantum theory and its relation to black body radiation
• identify data sources and gather, process and present information to summarise the use of the photoelectric effect in:
– solar cells – photocells
• solve problems and analyse information using:
E = hf and c = f λ
• process information to discuss Einstein and Planck’s differing views about whether science research is removed from social and political forces
page 211 205–6 207–8 201, 209–10 206
3. Limitations of past technologies and increased research into the structure of the atom resulted in the invention of transistors
Students learn to:
• identify that some electrons in solids are shared between atoms and move freely
• describe the difference between conductors, insulators and semi- conductors in terms of band structures and relative electrical resistance • identify absences of electrons in a nearly full band as holes, and
recognise that both electrons and holes help to carry current • compare qualitatively the relative number of free electrons that can drift
from atom to atom in conductors, semiconductors and insulators • identify that the use of germanium in early transistors is related to lack
of ability to produce other materials of suitable purity • describe how ‘doping’ a semiconductor can change its electrical
properties
• identify differences in p- and n-type semiconductors in terms of the relative number of negative charge carriers and positive holes • describe differences between solid state and thermionic devices and
discuss why solid state devices replaced thermionic devices
page 213–14 213–20 216–17, 219–20 213–15 218–19 217, 219–20 219–20 220–5 Students:
• perform an investigation to model the behaviour of semiconductors, including the creation of a hole or positive charge on the atom that has lost the electron and the movement of electrons and holes in opposite directions when an electric field is applied across the semiconductor • gather, process and present secondary information to discuss how
shortcomings in available communication technology led to an increased knowledge of the properties of materials with particular reference to the invention of the transistor
• identify data sources, gather, process, analyse information and use available evidence to assess the impact of the invention of transistors on society with particular reference to their use in microchips and microprocessors
page 230, 231 225–6, 231 225–8
4. Investigations into the electrical properties of particular metals at different temperatures led to the identification of superconductivity and the exploration of possible applications
Students learn to:
• outline the methods used by the Braggs to determine crystal structure • identify that metals possess a crystal lattice structure
• describe conduction in metals as a free movement of electrons unimpeded by the lattice
• identify that resistance in metals is increased by the presence of impurities and scattering of electrons by lattice vibrations • describe the occurrence in superconductors below their critical
temperature of a population of electron pairs unaffected by electrical resistance
• discuss the BCS theory
• discuss the advantages of using superconductors and identify limitations to their use page 236–9 239 240 240 243–6 243–4 240–2, 246–50 Students:
• process information to identify some of the metals, metal alloys and compounds that have been identified as exhibiting the property of superconductivity and their critical temperatures
• perform an investigation to demonstrate magnetic levitation • analyse information to explain why a magnet is able to hover above a
superconducting material that has reached the temperature at which it is superconducting
• gather and process information to describe how superconductors and the effects of magnetic fields have been applied to develop a maglev train • process information to discuss possible applications of superconductivity
and the effects of those applications on computers, generators and motors and transmission of electricity through power grids
page 241–2 253–4 240–1, 245 248–9 246–8 F = qvBsinθ f = qvBsinθ F =qE E V d ---=
xiii
Option module: ASTROPHYSICS (chapters 14–17, pages 255–338)
1. Our understanding of celestial objects depends upon observations made from Earth or space near the Earth
Students learn to:
• discuss Galileo’s use of the telescope to identify features of the Moon • discuss why some wavebands can be more easily detected from space • define the terms ‘resolution’ and ‘sensitivity’ of telescopes
• discuss the problems associated with ground-based astronomy in terms of resolution and absorption of radiation and atmospheric distortion • outline methods by which the resolution and/or sensitivity of
ground-based systems can be improved, including: – adaptive optics – interferometry – active optics page 257–8 258–60 262–4 265 265–8 Students:
• identify data sources, plan, choose equipment or resources for, and perform an investigation to demonstrate why it is desirable for telescopes to have a large diameter objective lens or mirror in terms of both sensitivity and resolution
page 272
2. Careful measurement of a celestial object’s position, in the sky, (astrometry) may be used to determine its distance
Students learn to:
• define the terms parallax, parsec, light-year
• explain how trigonometric parallax can be used to determine the distance to stars
• discuss the limitations of trigonometric parallax measurements
page 275–6 275–7 277–8
Students:
• solve problems and analyse information to calculate the distance to a star given its trigonometric parallax using:
• gather and process information to determine the relative limits to trigonometric parallax distance determinations using recent ground-based and space-ground-based telescopes
page 277, 299–300 302–3
3. Spectroscopy is a vital tool for astronomers and provides a wealth of information
Students learn to:
• account for the production of emission and absorption spectra and compare these with a continuous black body spectrum
• describe the technology needed to measure astronomical spectra • identify the general types of spectra produced by stars, emission
nebulae, galaxies and quasars
• describe the key features of stellar spectra and describe how these are used to classify stars
• describe how spectra can provide information on surface temperature, rotational and translational velocity, density and chemical composition of stars page 280–2 279–80 285 286–7 288–9 Students:
• perform a first-hand investigation to examine a variety of spectra produced by discharge tubes, reflected sunlight, or incandescent filaments
• analyse information to predict the surface temperature of a star from its intensity/wavelength graph
page 303 300, refer 281–2
4. Photometric measurements can be used for determining distance and comparing objects
Students learn to:
• define absolute and apparent magnitude
• explain how the concept of magnitude can be used to determine the distance to a celestial object
• outline spectroscopic parallax
• explain how two-colour values (i.e. colour index, B-V) are obtained and why they are useful
• describe the advantages of photoelectric technologies over photographic methods for photometry
page 291 291–2 293–5 293–7 298 Students:
• solve problems and analyse information using:
M = m − 5 log
and =
to calculate the absolute or apparent magnitude of stars using data and a reference star
• perform an investigation to demonstrate the use of filters for photometric measurements
• identify data sources, gather, process and present information to assess the impact of improvements in measurement technologies on our understanding of celestial objects
page 291, 292, 293, 294–5, 300–1 303–4 289, 298
5. The study of binary and variable stars reveals vital information about stars
Students learn to:
• describe binary stars in terms of the means of their detection: visual, eclipsing, spectroscopic and astrometric
• explain the importance of binary stars in determining stellar masses • classify variable stars as either intrinsic or extrinsic and periodic or
non-periodic
• explain the importance of the period-luminosity relationship for determining the distance of cepheids
page 306–10 306–8 312–314 315 Students:
• perform an investigation to model the light curves of eclipsing binaries using computer simulation
• solve problems and analyse information by applying:
m1 + m2 =
page 318–19 308, 318
6. Stars evolve and eventually ‘die’
Students learn to:
• describe the processes involved in stellar formation
• outline the key stages in a star’s life in terms of the physical processes involved
• describe the types of nuclear reactions involved in Main Sequence and post-Main Sequence stars
• discuss the synthesis of elements in stars by fusion
• explain how the age of a globular cluster can be determined from its zero-age main sequence plot for an H–R diagram
• explain the concept of star death in relation to: – planetary nebula – supernovae – white dwarfs – neutron stars/pulsars – black holes page 321–4 321–34, 335 324–8, 331 332 329–30 332–3 Students:
• present information by plotting Hertzsprung–Russell diagrams for: nearby or brightest stars; stars in a young open cluster; stars in a globular cluster
• analyse information from an H–R diagram and use available evidence to determine the characteristics of a star and its evolutionary stage • present information by plotting on an H–R diagram the pathways of stars
of 1, 5 and 10 solar masses during their life cycle
page 330 335, 338 335 d 1 p ---= d 10 --- IA IB --- 100mB–mA 5 ---4π2r3 Gπ2
---xiv
Option module: MEDICAL PHYSICS (chapters 18–21, pages 339–416)
1. The properties of ultrasound waves can be used as diagnostic tools
Students learn to:
• identify the differences between ultrasound and sound in normal hearing range
• describe the piezoelectric effect and the effect of using an alternating potential difference with a piezoelectric crystal
• define acoustic impedance:
and identify that different materials have different acoustic impedances • describe how the principles of acoustic impedance and reflection and
refraction are applied to ultrasound
• define the ratio of reflected to initial intensity as:
• identify that the greater the difference in acoustic impedance between two materials, the greater is the reflected proportion of the incident pulse
• describe the situations in which A scans, B scans, and phase and sector scans would be used and the reasons for the use of each
• describe the Doppler effect in sound waves and how it is used in ultrasonics to obtain flow characteristics of blood moving through the heart
• outline some cardiac problems that can be detected through the use of the Doppler effect
page 341–2 347 344–5 344–6 345–6 345–6 348–51 352–5 354–5 Students:
• solve problems and analyse information to calculate the acoustic impedance of a range of materials, including bone, muscle, soft tissue, fat, blood and air and explain the types of tissues that ultrasound can be used to examine
• gather secondary information to observe at least two ultrasound images of body organs
• identify data sources and gather information to observe the flow of blood through the heart from a Doppler ultrasound video image
• identify data sources, gather, process and analyse information to describe how ultrasound is used to measure bone density
• solve problems and analyse information using: and page 345, 358 344, 350, 355–6 355, 360 351–2 344–6, 358–9
2. The physical properties of electromagnetic radiation can be used as diagnostic tools
Students learn to:
• describe how X-rays are currently produced
• compare the differences between ‘soft’ and ‘hard’ X-rays • explain how a computed axial tomography (CT) scan is produced • describe circumstances where a CT scan would be a superior diagnostic
tool compared to either X-rays or ultrasound
• explain how an endoscope works in relation to total internal reflection • discuss differences between the role of coherent and incoherent
bundles of fibres in an endoscope • explain how an endoscope is used in:
– observing internal organs
– obtaining tissue samples of internal organs for further testing
page 362–3 366 368–70 371–7 373–7 375 376–7 Students:
• gather information to observe at least one image of a fracture on an X-ray film and X-ray images of other body parts
• gather secondary information to observe a CT scan image and compare the information provided by CT scans to that provided by an X-ray image for the same body part
• perform a first-hand investigation to demonstrate the transfer of light by optical fibres
• gather secondary information to observe internal organs from images produced by an endoscope page 361, 367, 368 371–2, 377 380 377, 379
3. Radioactivity can be used as a diagnostic tool
Students learn to:
• outline properties of radioactive isotopes and their half lives that are used to obtain scans of organs
• describe how radioactive isotopes may be metabolised by the body to bind or accumulate in the target organ
• identify that, during decay of specific radioactive nuclei, positrons are given off
• discuss the interaction of electrons and positrons resulting in the production of gamma rays
• describe how the positron emission tomography (PET) technique is used for diagnosis
page 382–4 384, 385 392–3 392 393–5 Students:
• perform an investigation to compare an image of bone scan with an X-ray image
• gather and process secondary information to compare a scanned image of at least one healthy body part or organ with a scanned image of its diseased counterpart
page 390, 397 388, 390, 391
4. The magnetic field produced by nuclear particles can be used as a diagnostic tool
Students learn to:
• identify that the nuclei of certain atoms and molecules behave as small magnets
• identify that protons and neutrons in the nucleus have properties of spin and describe how net spin is obtained
• explain that the behaviour of nuclei with a net spin, particularly hydrogen, is related to the magnetic field they produce
• describe the changes that occur in the orientation of the magnetic axis of nuclei before and after the application of a strong magnetic field • define precessing and relate the frequency of the precessing to the composition of the nuclei and the strength of the applied external magnetic field
• discuss the effect of subjecting precessing nuclei to pulses of radio waves • explain that the amplitude of the signal given out when precessing
nuclei relax is related to the number of nuclei present • explain that large differences would occur in the relaxation time
between tissue containing hydrogen-bound water molecules and tissues containing other molecules
page 399–400 400–1 400–1 403–4 404–5 405–8 408–9 409–10 Students:
• perform an investigation to observe images from magnetic resonance image (MRI) scans, including a comparison of healthy and damaged tissue
• identify data sources, gather, process and present information using available evidence to explain why MRI scans can be used to: – detect cancerous tissues
– identify areas of high blood flow
– distinguish between grey and white matter in the brain
• gather and process secondary information to identify the function of the electromagnet, radio frequency oscillator, radio receiver and computer in the MRI equipment
• identify data sources, gather and process information to compare the advantages and disadvantages of X-rays, CT scans, PET scans and MRI scans
• gather, analyse information and use available evidence to assess the impact of medical applications of physics on society
page 408, 410, 411, 414 410–13 402 412–13, 415 415 Z =ρv Ir I0 ---- [Z2–Z1] 2 Z2+Z1 [ ]2 ---= Z =ρv Ir I0 ---- Z2–Z1 [ ]2 Z2+Z1 [ ]2 ---=
xv
Option module: From QUANTA TO QUARKS (chapters 22–26, pages 417–520)
1. Problems with the Rutherford model of the atom led to the search for a model that would better explain the observed phenomena
Students learn to:
• discuss the structure of the Rutherford model of the atom, the existence of the nucleus and electron orbits
• analyse the significance of the hydrogen spectrum in the development of Bohr’s model of the atom
• define Bohr’s postulates
• discuss Planck’s contribution to the concept of quantised energy • describe how Bohr’s postulates led to the development of a
mathematical model to account for the existence of the hydrogen spectrum:
• discuss the limitations of the Bohr model of the hydrogen atom
page 421–3 424 427–8 423 429–33 434 Students:
• perform a first-hand investigation to observe the visible components of the hydrogen spectrum
• process and present diagrammatic information to illustrate Bohr’s explanation of the Balmer series
• solve problems and analyse information using:
• analyse secondary information to identify the difficulties with the Rutherford–Bohr model, including its inability to completely explain: – the spectra of larger atoms
– the relative intensity of spectral lines – the existence of hyperfine spectral lines – the Zeeman effect
page 437–9 433–4 425, 435 434
2. The limitations of classical physics gave birth to quantum physics
Students learn to:
• describe the impact of de Broglie’s proposal that any kind of particle has both wave and particle properties
• define diffraction and identify that interference occurs between waves that have been diffracted
• describe the confirmation of de Broglie’s proposal by Davisson and Germer
• explain the stability of the electron orbits in the Bohr atom using de Broglie’s hypothesis page 444–6 441–3 446 446–7 Students:
• solve problems and analyse information using:
• gather, process, analyse and present information and use available evidence to assess the contributions made by Heisenberg and Pauli to the development of atomic theory
page 445, 452 448–51
3. The work of Chadwick and Fermi in producing artificial transmutations led to practical applications of nuclear physics
Students learn to:
• define the components of the nucleus (protons and neutrons) as nucleons and contrast their properties
• discuss the importance of conservation laws to Chadwick’s discovery of the neutron
• define the term ‘transmutation’
• describe nuclear transmutations due to natural radioactivity • describe Fermi’s initial experimental observation of nuclear fission • discuss Pauli’s suggestion of the existence of the neutrino and relate it to
the need to account for the energy distribution of electrons emitted in ß-decay
• evaluate the relative contributions of electrostatic and gravitational forces between nucleons
• account for the need for the strong nuclear force and describe its properties
• explain the concept of a mass defect using Einstein’s equivalence between mass and energy
• describe Fermi’s demonstration of a controlled nuclear chain reaction in 1942
• compare requirements for controlled and uncontrolled nuclear chain reactions page 457 460 456 456 476–8 461–5 467 467–8 468–70 481–2 482–7 Students:
• perform a first-hand investigation or gather secondary information to observe radiation emitted from a nucleus using a Wilson cloud chamber or similar detection device
• solve problems and analyse information to calculate the mass defect and energy released in natural transmutation and fission reactions
page 518–20 470–1, 473, 494
4. An understanding of the nucleus has led to large science projects and many applications
Students learn to:
• explain the basic principles of a fission reactor
• describe some medical and industrial applications of radioisotopes • describe how neutron scattering is used as a probe by referring to the
properties of neutrons
• identify ways by which physicists continue to develop their
understanding of matter, using accelerators as a probe to investigate the structure of matter
• discuss the key features and components of the standard model of matter, including quarks and leptons
page 484–8 489–91 492 496–502 503–13 Students:
• gather, process and analyse information to assess the significance of the Manhattan Project to society
• identify data sources, and gather, process and analyse information to describe the use of:
– a named isotope in medicine – a named isotope in agriculture – a named isotope in engineering
page 480–4 489–91 1 λ --- R 1 nf2 --- 1 ni2 ---– = 1 λ --- R 1 nf2 --- 1 ni2 ---– = λ h mv ---=
xvi
ACKNOWLEDGEMENTS
The authors would like to thank the following people fortheir support during the writing of this book: Michael Andriessen gives special thanks to Christine, Sam and Luke for their understanding and patience; Peter Pentland wishes especially to thank his wife Helen Kennedy for her contin-uing support; Bruce McKay is indebted to close friend and former colleague Barry Mott for his valuable advice; Richard Gaut thanks Stephen and Greta for their helpful suggestions and feedback; Jill Tacon wishes to thank Dr Manjula Sharma and Dr Joe Khachan from the University of Sydney for their valuable advice and Lee Collins from Westmead Hospital for his expert assistance. Yoka McCallum’s contribution and encouragement is also appreciated, and thanks must go to Dean Bunn for his permission to adapt some practical activi-ties and other material from Physics for a Modern World. The authors and publisher are grateful to the following indi-viduals and organisations for their permission to reproduce photographs and other copyright material.
Images
• © Alan Bean/Novaspace Galleries: 2.2 • AIP Emilio Segrè Visual Achives, W.F. Meggers Collection: 22.8 • © ANSTO: 20.3,
20.4/Gentech® generator courtesy of ANSTO • Otto Rogge/ ANTPhoto.com.au: 11.21 • Bhathal, R., Astronomy for the HSC, Kangaroo Press 1993, p. 47. Reproduced by permission of Ragbir Bhathal: 17.12(a–c) • © Black & Decker: 9.1 • © Boeing: 3.9 • The Royal Institution, London, UK/ Bridgeman Art Library: 7.1 • Courtesy of Brookhaven National Laboratory: 26.8(a, b) • Cavendish Laborator y, Cambridge University: 10.1 • © University of Queensland, Centre for Magnetic Resonance: 21.15(a–c) • Chicago Historical Society, Birth of the Atomic Age, Painting by Gary Sheahan, 1957: 25.5 • © Corbis Australia/Australian Picture Library: 13.1; 18.16/ Belt/Corbis/Annie Griffiths; 8.17/Corbis; 8.15, 8.16, 11.2,
11.5, 11.12, 23.11, 23.12, 23.13, 23.14, 23.15/Corbis/Bettman;
21.14(d)/Corbis/Howard Sochurek; 7.4/Corbis/Hulton-Deutsch Collection • © CERN: 26.2 • © CFHT, 1996 Used with permission: 14.17 • Adapted from Physics in Medical Diagnosis, Chapman & Hall 1997, p. 213 fig. 5.23. Reproduced with permission of the author Dr Trevor A Delchar: 18.14(a) • © Digital Stock/Corbis Corporation: page 99; 2.4, 13.18 • © Digital Vision: 2.1 • © Dorling Kindersley: 6.1 • Image courtesy of Elaine Collin: 19.19 • © Corbis/Greg Smith:
11.22 • Image courtesy of the European Space Agency © ESA:
14.13, 15.6 • Courtesy of EMI Archives: 19.10 • Fermilab National Accelerator Laborator y: 26.1, 26.7, 26.10 • Dave Finley, National Radio Astronomy Observatory, courtesy Associated Universities, Inc., and the National Science Foundation: 14.14 • © Fundamental Photographs, New York: 15.8(a); 15.14, 22.9,
23.6/Wabash Instrument Corp.; 23.2(a)/Ken Kay • © Getty Images/ Hulton Archive: 14.2, 22.2, 23.8 • David Grabham: 19.7,
21.14(c), 21.18(a, b) • Medical Physics by J Pope, p. 81, fig 4.13 Reprinted by permission of Harcourt Education Ltd: 21.13 • Reprinted by permission of HarperCollins Publishers Ltd. © Illingworth 1994: 15.21, 16.10 • Terry Herter: 16.15, 16.16 • Adapted and reproduced from Martin Hollins, Medical Physics, 2nd edition, Nelson Thornes 2001, pp. 114, 122, 127, 100, 101, 186, 197: 18.6, 18.17, 19.6, 19.16, 19.17, 20.7(b), 21.6 • ‘The Fermion Particles’ and ‘The Boson Force Carriers’, From Quarks to the Cosmos: Tools of Discovery by Leon M Lederman and David N Schramm. © 1989, 1995 Scientific American Librar y. Reprinted by permission of Henry Holt and Company, LLC: table 26.4 • Courtesy of Hologic: 18.11 • © www.imageaddict.com.au: 14.8,
14.10 • ImageState: 10.5 • Kamioka Observatory, ICRR (Institute for Cosmic Ray Research), The University of Tokyo: 24.1 • IEE Review March 2001, Vol 47, 102, p 42. Reproduced with permission of IET. www.theiet.org: 13.25 • Jared Schneidman Design:
12.24 • JAS Photography/John Sowden: 2.3 • Kenneth Krane,
Modern Physics 2nd edition, 1996, p. 24. Used by permission of John Wiley & Sons, Inc.: 5.4 • Resnick, R, Introduction to Special Relativity, figures 1.4 and 1.6, John Wiley & Sons Inc., © 1968: 5.5 • Halliday et al., Fundamentals of Physics Extended, 5th edition, John Wiley & Sons, Inc. 1997, figures 37.27 (b, c and d), 43.3, 37.22, 43.6. Used by permission of John Wiley & Sons, Inc.: 13.9,
13.12, 22.5, 22.12, 24.15 • Webster, J G (ed), Medical
Instrumentation, 3rd edition, 1998, p. 559, adapted and used by permission of John Wiley & Sons, Inc.: 20.7(a) • Adapted from ‘The Particle Adventure’, produced by the Particle Data Group, Lawrence Berkeley National Laborator y: 26.3, 26.4 • Bruce McKay: 13.4, 22.1, 23.2(b, c), 26.11 • David Malin Images:
15.1 • Mary Evans Picture Library: 14.3 • Cambridge Encyclopedia of Astronomy, ed. by Dr Simon Mitton, Jonathon Cape, 1977, © Cambridge University. Reproduced with pemission of Simon Mitton: 15.8(b), 17.13 • Barbara Mochejska (Copernicus Astronomical Center), Andrew Szentgyorgyi
(Harvard-Smithsonian Center for Astrophysics), F. L. Whipple Obser vatory:
17.11(b) • NASA: 2.28, 3.1/MSFC, 3.6, 3.8, 4.8/NSSDC, 14.1/ STSCI, 14.7, 17.3/NOAO, 17.16/The Hubble Heritage Team,
17.18(a)/ESA/ASU/J Hester and A Loll, 17.18(b)/CXC/ASU/ J Hester et al. • © Newspix: 20.13/Jody D’Arcy, 25.2 • © Moriel NessAiver: 21.2 • © Department of Nuclear Medicine, The Queen Elizabeth Hospital, South Australia: 20.7(d) • De Jong et al., Heinmann Physics Two, p. 237. Reproduced with permission from Pearson Education Australia: 13.2 • Adapted from David Heffernan, Physics Contexts 2, Pearson Education Australia 2002, p. 315. Reproduced with permission of Pearson Education Australia: 18.8 • Peter Pentland: 9.9 • © Philips Medical Systems: 18.3(b), 19.11 • © Photodisc, Inc.: pages 1, 173, 255,
339, 417; 1.1, 4.1, 8.1, 8.24(a, b), 10.22, 11.19, 17.1, 18.1, 18.3(c),
19.9(a), 20.15(a), 21.17, 25.1 • photolibrary.com: 9.4/Tom Marexchal, 13.26(b)/Photo Researchers Inc., 17.11(a)/John Chumack; 18.15(a, b), 19.14, 20.9, 21.1, 21.3, 21.14(a, b), 23.1/ Phototake; 19.8/Phototake Science; 19.9(b), 20.14/Phototake Science/Science Ltd; 20.1/Phototake Science/ISM
• photolibrary.com/Science Photo Librar y: 4.2, 5.1, 7.2, 14.5,
15.22, 19.1, 22.7; 3.11/NASA; 10.26(b)/Peter Apraham; 11.1,
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12.25(a) • © Greg Pitt: 20.7(c) • Science Museum/Science & Society Picture Library: 24.8 • Reprinted from Medical Physics, 1978, John Wiley & Sons Inc. with permission from the authors, John R Cameron and James G Skofronick © 1992: 19.5(a, b) • Peter Storer: 8.22 • Sudbury Neutrino Observatory/R Chambers:
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• Extracts from Physics Stage 6 Syllabus © Board of Studies NSW, 2002 (pages x–xv) • Data and formulae sheets from Physics Higher School Certificate Examination © Board of Studies NSW (pages 526–7) • Higher School Certificate Assessment Support Document © Board of Studies NSW, 1999 (key words, pages 529–30)
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SPACE
HSC C
ORE
MODUL
E
Chapter 1
Earth’s gravitational field
Chapter 2
Launching into space
Chapter 3
Orbiting and re-entry
Chapter 4
Gravity in the solar system
Chapter 5
1
EARTH’S
GRAVITATIONAL
FIELD
Figure 1.1 The Earth rising as seen from the Moon
CHAPTER
Remember
Before beginning this chapter, you should be able to:
• recall and apply Newton’s Second Law of Motion:F = ma.
Key content
At the end of this chapter you should be able to:
• make a comparison between the acceleration due to gravity at various places over the Earth’s surface as well as at other locations throughout the solar system
• define weight as the force on an object due to a gravitational field
• explain that work done to raise or lower a mass in a gravitational field is directly related to a change in the gravitational potential energy of the mass
• calculate the weight of a body on Earth, above the Earth or on other planets
• define gravitational potential energy as the work done in moving an object from a very large distance away to a point in a gravitational field.
CHAPTER 1 EARTH’S GRAVITATIONAL FIELD
3
Gravity is a force of attraction that exists between any two masses. Usually this is a very small, if not negligible, force. However, when one or both of the masses is as large as a planet, then the force becomes very significant indeed. The force of attraction between the Earth and our own bodies is the force we call our weight. This force exists wherever we are on or near the Earth’s surface (although, as we shall see, with some variation). We can say that a gravitational field exists around the Earth and we live within that field.1.1
THE EARTH’S GRAVITY
The Earth is surrounded by a gravitational field. This type of field, discussed in more general terms in chapter 4, is a vector field within which a mass will experience a force.
(Other vector fields include electric and magnetic fields.) The gravitational field around the Earth can be drawn as shown in figure 1.2. Note that the direction of a field line at any point is the direction of the force experienced by a mass placed at that point.
The field vector: g
A field vector is a single vector that describes the strength and direction of a uniform vector field. For a gravitational field the field vector is g, which is defined in this way:
g = where
F = force exerted (N) on mass m
m = mass (kg) in the field
g = the field vector (N kg−1).
Vector symbols are indicated here in bold italics. The direction of the vector g is the same as the direction of the associated force.
Note that a net force applied to a mass will cause it to accelerate. Newton’s Second Law describes this relationship:
a = where
a = acceleration (m s−2).
Hence, we can say that the field vector g also represents the accel-eration due to gravity and we can calculate its value at the Earth’s surface as described below.
The Law of Universal Gravitation (discussed in more detail in chapter 4) says that the magnitude of the force of attraction between the Earth and an object on the Earth’s surface is given by:
F = G
Figure 1.2 The gravitational field around the Earth
F
m
----A field vector is a single vector that describes the strength and direction of a uniform vector field. For a gravitational field, the field vector is g.
1.1
Using a pendulum to determine g F m ----mEmO rE2---SPACE
4
where
mE = the mass of the Earth = 5.97 × 1024 kg
mO = mass of the object (kg)
rE = radius of the Earth = 6.38 × 106 m.
From the defining equation for g, on the previous page, we can see that the force experienced by the mass can also be described by:
F = mOg. Equating these two we get: mOg = G .
This simplifies to give: g = G
= .
Hence, g ≈ 9.80 m s−2.
The value of the Earth’s radius used here, 6378 km (at the Equator), is an average value so the value of g calculated, 9.80 m s−2, also represents an average value.
Variations in the value of g
Variation with geographical location
The actual value of the acceleration due to gravity, g, that will apply in a given situation will depend upon geographical location. Minor variations in the value of g around the Earth’s surface occur because:
• the Earth’s crust or lithosphere shows variations in thickness and structure due to factors such as tectonic plate boundaries and dense mineral deposits. These variations can alter local values of g.
• the Earth is not a perfect sphere, but is flattened at the poles. This means that the value of g will be greater at the poles, since they are closer to the centre of the Earth.
• the spin of the Earth creates a centrifuge effect that reduces the effec-tive value of g. The effect is greatest at the Equator and there is no effect at the poles.
As a result of these factors, the rate of acceleration due to gravity at the surface of the Earth varies from a minimum value at the Equator of 9.782 m s−2 to a maximum value of 9.832 m s−2 at the poles. The usual value used in equations requiring g is 9.8 m s−2.
Variation with altitude
The formula for g shows that the value of g will also vary with altitude above the Earth’s surface. By using a value of r equal to the radius of the Earth plus altitude, the following values can easily be calculated. It is clear from table 1.1 that the effect of the Earth’s gravitational field is felt quite some distance out into space.
The formula used is: g = G .
Note that as altitude increases the value of g decreases, dropping to zero only when the altitude has an infinite value.
mEmO rE2 ---mE rE2 ---6.672×10–11 ( ) 5.974( ×1024) 6.378×106 ( )2 ---mE rE+altitude ( )2
