Outline

Topics and syllabus points

1Motion, forces and energy74 total74 mapped
1.1Physical quantities and measurement techniques7 total7 mapped

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1.2Motion13 total13 mapped

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1.3Mass and weight5 total5 mapped

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1.4Density4 total4 mapped

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1.5Forces21 total21 mapped
1.5.1Effects of forces12 total12 mapped

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  • 1.5.1.9

    Define the spring constant as force per unit extension; recall and use the equation F k = x

    1 lesson
  • 1.5.1.10

    Define and use the term ‘limit of proportionality’ for a load–extension graph and identify this point on the graph (an understanding of the elastic limit is not required)

    1 lesson
  • 1.5.1.11

    Recall and use the equation F = ma and know that the force and the acceleration are in the same direction

    1 lesson
  • 1.5.1.12

    Describe, qualitatively, motion in a circular path due to a force perpendicular to the motion as: (a) speed increases if force increases, with mass and radius constant (b) radius decreases if force increases, with mass and speed constant (c) an increased mass requires an increased force to keep speed and radius constant mv 2 (F = is not required) r

    1 lesson
1.5.2Turning effect of forces6 total6 mapped

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1.5.3Centre of gravity3 total3 mapped

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1.6Momentum4 total4 mapped

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1.7Energy, work and power16 total16 mapped
1.7.1Energy6 total6 mapped

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1.7.2Work2 total2 mapped

Core

1.7.3Energy resources7 total7 mapped

Core

  • 1.7.3.1

    Describe how useful energy may be obtained, or electrical power generated, from: (a) chemical energy stored in fossil fuels (b) chemical energy stored in biofuels (c) water, including the energy stored in waves, in tides and in water behind hydroelectric dams (d) geothermal resources (e) nuclear fuel (f) light from the Sun to generate electrical power (solar cells) (g) infrared and other electromagnetic waves from the Sun to heat water (solar panels) and be the source of wind energy including references to a boiler, turbine and generator where they are used

    1 lesson
  • 1.7.3.2

    Describe advantages and disadvantages of each method in terms of renewability, availability, reliability, scale and environmental impact

    1 lesson
  • 1.7.3.3

    Understand, qualitatively, the concept of efficiency of energy transfer

    1 lesson

Supplement

1.7.4Power1 total1 mapped

Core

  • 1.7.4.1

    Define power as work done per unit time and also as energy transferred per unit time; recall and use the equations W (a) P = t ∆E (b) P = t

    1 lesson
1.8Pressure4 total4 mapped

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2Thermal physics45 total45 mapped
2.1Kinetic particle model of matter13 total13 mapped
2.1.1States of matter2 total2 mapped

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2.1.2Particle model8 total8 mapped

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2.1.3Gases and the absolute scale of temperature3 total3 mapped

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2.2Thermal properties and temperature15 total15 mapped
2.2.1Thermal expansion of solids, liquids and gases3 total3 mapped

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  • 2.2.1.3

    Explain, in terms of the motion and arrangement of particles, the relative order of magnitudes of the expansion of solids, liquids and gases as their temperatures rise

    1 lesson
2.2.2Specific heat capacity4 total4 mapped

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2.2.3Melting, boiling and evaporation8 total8 mapped

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2.3Transfer of thermal energy17 total17 mapped
2.3.1Conduction4 total4 mapped

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2.3.2Convection2 total2 mapped

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2.3.3Radiation9 total9 mapped

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2.3.4Consequences of thermal energy transfer2 total2 mapped

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3Waves56 total56 mapped
3.1General properties of waves10 total10 mapped

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3.2Light24 total24 mapped
3.2.1Reflection of light4 total4 mapped

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3.2.2Refraction of light9 total9 mapped

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3.2.3Thin lenses8 total8 mapped

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3.2.4Dispersion of light3 total3 mapped

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3.3Electromagnetic spectrum10 total10 mapped

Core

  • 3.3.1

    Know the main regions of the electromagnetic spectrum in order of frequency and in order of wavelength

    1 lesson
  • 3.3.2

    Know that all electromagnetic waves travel at the same high speed in a vacuum

    1 lesson
  • 3.3.3

    Describe typical uses of the different regions of the electromagnetic spectrum including: (a) radio waves; radio and television transmissions, astronomy, radio frequency identification (RFID) (b) microwaves; satellite television, mobile phones (cell phones), microwave ovens (c) infrared; electric grills, short range communications such as remote controllers for televisions, intruder alarms, thermal imaging, optical fibres (d) visible light; vision, photography, illumination (e) ultraviolet; security marking, detecting fake bank notes, sterilising water (f) X-rays; medical scanning, security scanners (g) gamma rays; sterilising food and medical equipment, detection of cancer and its treatment

    1 lesson
  • 3.3.4

    Describe the harmful effects on people of excessive exposure to electromagnetic radiation, including: (a) microwaves; internal heating of body cells (b) infrared; skin burns (c) ultraviolet; damage to surface cells and eyes, leading to skin cancer and eye conditions (d) X-rays and gamma rays; mutation or damage to cells in the body

    1 lesson
  • 3.3.5

    Know that communication with artificial satellites is mainly by microwaves: (a) some satellite phones use low orbit artificial satellites (b) some satellite phones and direct broadcast satellite television use geostationary satellites

    1 lesson

Supplement

  • 3.3.6

    Know that the speed of electromagnetic waves in a vacuum is 3.0 × 108 m / s and is approximately the same in air

    1 lesson
  • 3.3.7

    Know that many important systems of communications rely on electromagnetic radiation including: (a) mobile phones (cell phones) and wireless internet use microwaves because microwaves can penetrate some walls and only require a short aerial for transmission and reception (b) Bluetooth uses radio waves because radio waves pass through walls but the signal is weakened on doing so (c) optical fibres (visible light or infrared) are used for cable television and high-speed broadband because glass is transparent to visible light and some infrared; visible light and short wavelength infrared can carry high rates of data

    1 lesson
  • 3.3.8

    Know the difference between a digital and analogue signal

    1 lesson
  • 3.3.9

    Know that a sound can be transmitted as a digital or analogue signal

    1 lesson
  • 3.3.10

    Explain the benefits of digital signalling including increased rate of transmission of data and increased range due to accurate signal regeneration

    1 lesson
3.4Sound12 total12 mapped

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4Electricity and magnetism88 total88 mapped
4.1Simple phenomena of magnetism11 total11 mapped

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4.2Electrical quantities32 total32 mapped
4.2.1Electric charge10 total10 mapped

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4.2.2Electric current6 total6 mapped

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4.2.3Electromotive force and potential difference7 total7 mapped

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4.2.4Resistance5 total5 mapped

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4.2.5Electrical energy and electrical power4 total4 mapped

Core

4.3Electric circuits15 total15 mapped
4.3.1Circuit diagrams and circuit components2 total2 mapped

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4.3.2Series and parallel circuits10 total10 mapped

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  • 4.3.2.8

    Recall and use in calculations, the fact that: (a) the sum of the currents entering a junction in a parallel circuit is equal to the sum of the currents that leave the junction (b) the total p.d. across the components in a series circuit is equal to the sum of the individual p.d.s across each component (c) the p.d. across an arrangement of parallel resistances is the same as the p.d. across one branch in the arrangement of the parallel resistances

    1 lesson
  • 4.3.2.9

    Explain that the sum of the currents into a junction is the same as the sum of the currents out of the junction

    1 lesson
  • 4.3.2.10

    Calculate the combined resistance of two resistors in parallel

    1 lesson
4.3.3Action and use of circuit components3 total3 mapped

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4.4Electrical safety5 total5 mapped

Core

4.5Electromagnetic effects25 total25 mapped
4.5.1Electromagnetic induction5 total5 mapped

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4.5.2The a.c. generator2 total2 mapped

Supplement

  • 4.5.2.1

    Describe a simple form of a.c. generator (rotating coil or rotating magnet) and the use of slip rings and brushes where needed

    1 lesson
  • 4.5.2.2

    Sketch and interpret graphs of e.m.f. against time for simple a.c. generators and relate the position of the generator coil to the peaks, troughs and zeros of the e.m.f.

    1 lesson
4.5.3Magnetic effect of a current5 total5 mapped

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4.5.4Force on a current-carrying conductor3 total3 mapped

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4.5.5The d.c. motor2 total2 mapped

Core

  • 4.5.5.1

    Know that a current-carrying coil in a magnetic field may experience a turning effect and that the turning effect is increased by increasing: (a) the number of turns on the coil (b) the current (c) the strength of the magnetic field

    1 lesson

Supplement

4.5.6The transformer8 total8 mapped

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5Nuclear physics31 total31 mapped
5.1The nuclear model of the atom11 total11 mapped
5.1.1The atom3 total3 mapped

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  • 5.1.1.3

    Describe how the scattering of alpha (α) particles by a sheet of thin metal supports the nuclear model of the atom, by providing evidence for: (a) a very small nucleus surrounded by mostly empty space (b) a nucleus containing most of the mass of the atom (c) a nucleus that is positively charged

    1 lesson
5.1.2The nucleus8 total8 mapped

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5.2Radioactivity20 total20 mapped
5.2.1Detection of radioactivity5 total5 mapped

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5.2.2The three types of nuclear emission4 total4 mapped

Core

  • 5.2.2.1

    Describe the emission of radiation from a nucleus as spontaneous and random in direction

    1 lesson
  • 5.2.2.2

    Identify alpha (α), beta (β) and gamma (γ) emissions from the nucleus by recalling: (a) their nature (b) their relative ionising effects (c) their relative penetrating abilities (β+ are not included, β-particles will be taken to refer to β –)

    1 lesson

Supplement

5.2.3Radioactive decay5 total5 mapped

Core

  • 5.2.3.1

    Know that radioactive decay is a change in an unstable nucleus that can result in the emission of α-particles or β-particles and/or γ-radiation and know that these changes are spontaneous and random

    1 lesson
  • 5.2.3.2

    State that during α-decay or β-decay, the nucleus changes to that of a different element

    1 lesson

Supplement

  • 5.2.3.3

    Know that isotopes of an element may be radioactive due to an excess of neutrons in the nucleus and/or the nucleus being too heavy

    1 lesson
  • 5.2.3.4

    Describe the effect of α-decay, β-decay and γ-emissions on the nucleus, including an increase in stability and a reduction in the number of excess neutrons; the following change in the nucleus occurs during β-emission neutron → proton + electron

    1 lesson
  • 5.2.3.5

    Use decay equations, using nuclide notation, to show the emission of α-particles, β-particles and γ-radiation

    1 lesson
5.2.4Half-life3 total3 mapped

Core

  • 5.2.4.1

    Define the half-life of a particular isotope as the time taken for half the nuclei of that isotope in any sample to decay; recall and use this definition in simple calculations, which might involve information in tables or decay curves (calculations will not include background radiation)

    1 lesson

Supplement

  • 5.2.4.2

    Calculate half-life from data or decay curves from which background radiation has not been subtracted

    1 lesson
  • 5.2.4.3

    Explain how the type of radiation emitted and the half-life of an isotope determine which isotope is used for applications including: (a) household fire (smoke) alarms (b) irradiating food to kill bacteria (c) sterilisation of equipment using gamma rays (d) measuring and controlling thicknesses of materials with the choice of radiations used linked to penetration and absorption (e) diagnosis and treatment of cancer using gamma rays

    1 lesson
5.2.5Safety precautions3 total3 mapped

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6Space physics30 total30 mapped
6.1The Earth and the Solar System14 total14 mapped
6.1.1The Earth4 total4 mapped

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6.1.2The Solar System10 total10 mapped

Core

  • 6.1.2.1

    Describe the Solar System as containing: (a) one star, the Sun (b) the eight named planets and know their order from the Sun (c) minor planets that orbit the Sun, including dwarf planets such as Pluto and asteroids in the asteroid belt (d) moons, that orbit the planets (e) smaller Solar System bodies, including comets and natural satellites

    1 lesson
  • 6.1.2.2

    Know that, in comparison to each other, the four planets nearest the Sun are rocky and small and the four planets furthest from the Sun are gaseous and large, and explain this difference by referring to an accretion model for Solar System formation, to include: (a) the model’s dependence on gravity (b) the presence of many elements in interstellar clouds of gas and dust (c) the rotation of material in the cloud and the formation of an accretion disc

    1 lesson
  • 6.1.2.3

    Know that the strength of the gravitational field (a) at the surface of a planet depends on the mass of the planet (b) around a planet decreases as the distance from the planet increases

    1 lesson
  • 6.1.2.4

    Calculate the time it takes light to travel a significant distance such as between objects in the Solar System

    1 lesson
  • 6.1.2.5

    Know that the Sun contains most of the mass of the Solar System and this explains why the planets orbit the Sun

    1 lesson
  • 6.1.2.6

    Know that the force that keeps an object in orbit around the Sun is the gravitational attraction of the Sun

    1 lesson

Supplement

  • 6.1.2.7

    Know that planets, minor planets and comets have elliptical orbits, and recall that the Sun is not at the centre of the elliptical orbit, except when the orbit is approximately circular

    1 lesson
  • 6.1.2.8

    Analyse and interpret planetary data about orbital distance, orbital duration, density, surface temperature and uniform gravitational field strength at the planet’s surface

    1 lesson
  • 6.1.2.9

    Know that the strength of the Sun’s gravitational field decreases and that the orbital speeds of the planets decrease as the distance from the Sun increases

    1 lesson
  • 6.1.2.10

    Know that an object in an elliptical orbit travels faster when closer to the Sun and explain this using the conservation of energy

    1 lesson
6.2Stars and the Universe16 total16 mapped
6.2.1The Sun as a star2 total2 mapped

Core

  • 6.2.1.1

    Know that the Sun is a star of medium size, consisting mostly of hydrogen and helium, and that it radiates most of its energy in the infrared, visible light and ultraviolet regions of the electromagnetic spectrum

    1 lesson

Supplement

  • 6.2.1.2

    Know that stars are powered by nuclear reactions that release energy and that in stable stars the nuclear reactions involve the fusion of hydrogen into helium

    1 lesson
6.2.2Stars3 total3 mapped

Core

  • 6.2.2.1

    State that: (a) galaxies are each made up of many billions of stars (b) the Sun is a star in the galaxy known as the Milky Way (c) other stars that make up the Milky Way are much further away from the Earth than the Sun is from the Earth (d) astronomical distances can be measured in light-years, where one light-year is the distance travelled in (the vacuum of) space by light in one year

    1 lesson

Supplement

  • 6.2.2.2

    Know that one light-year is equal to 9.5 × 1015 m

    1 lesson
  • 6.2.2.3

    Describe the life cycle of a star: (a) a star is formed from interstellar clouds of gas and dust that contain hydrogen (b) a protostar is an interstellar cloud collapsing and increasing in temperature as a result of its internal gravitational attraction (c) a protostar becomes a stable star when the inward force of gravitational attraction is balanced by an outward force due to the high temperature in the centre of the star (d) all stars eventually run out of hydrogen as fuel for the nuclear reaction (e) most stars expand to form red giants and more massive stars expand to form red supergiants when most of the hydrogen in the centre of the star has been converted to helium (f) a red giant from a less massive star forms a planetary nebula with a white dwarf star at its centre (g) a red supergiant explodes as a supernova, forming a nebula containing hydrogen and new heavier elements, leaving behind a neutron star or a black hole at its centre (h) the nebula from a supernova may form new stars with orbiting planets

    1 lesson
6.2.3The Universe11 total11 mapped

Core

  • 6.2.3.1

    Know that the Milky Way is one of many billions of galaxies making up the Universe and that the diameter of the Milky Way is approximately 100 000 light-years

    1 lesson
  • 6.2.3.2

    Describe redshift as an increase in the observed wavelength of electromagnetic radiation emitted from receding stars and galaxies

    1 lesson
  • 6.2.3.3

    Know that the light emitted from distant galaxies appears redshifted in comparison with light emitted on the Earth

    1 lesson
  • 6.2.3.4

    Know that redshift in the light from distant galaxies is evidence that the Universe is expanding and supports the Big Bang Theory

    1 lesson

Supplement

  • 6.2.3.5

    Know that microwave radiation of a specific frequency is observed at all points in space around us and is known as cosmic microwave background radiation (CMBR)

    1 lesson
  • 6.2.3.6

    Explain that the CMBR was produced shortly after the Universe was formed and that this radiation has been expanded into the microwave region of the electromagnetic spectrum as the Universe expanded

    1 lesson
  • 6.2.3.7

    Know that the speed v at which a galaxy is moving away from the Earth can be found from the change in wavelength of the galaxy’s starlight due to redshift

    1 lesson
  • 6.2.3.8

    Know that the distance d of a far galaxy can be determined using the brightness of a supernova in that galaxy

    1 lesson
  • 6.2.3.9

    Define the Hubble constant H0 as the ratio of the speed at which the galaxy is moving away from the Earth to its distance from the Earth; recall and use the equation v H0 = d

    1 lesson
  • 6.2.3.10

    Know that the current estimate for H0 is 2.2 × 10 –18 per second

    1 lesson
  • 6.2.3.11

    Know that the equation d 1 = v H0 represents an estimate for the age of the Universe and that this is evidence for the idea that all the matter in the Universe was present at a single point

    1 lesson