Topic: Cosmology

1.04 know and use the relationship between average speed, distance moved and time taken

To calculate average speed use 

speed (m/s) = distance travelled (m)/ time taken (s)

1.18 know and use the relationship between weight, mass and gravitational field strength: W=mxg

Weight (N)= Mass (kg) x gravitational field strength (N/kg)

gravitational field strength on earth is approx. 10 N/kg and in GCSEs is taken to be 10 N/kg. 

8.02 know that: the universe is a large collection of billions of galaxies, a galaxy is a large collection of billions of stars, our solar system is in the Milky Way galaxy

The  Milky Way galaxy contains billions of stars

The Universe – billions of galaxies

8.03 understand why gravitational field strength, g, varies and know that it is different on other planets and the Moon from that on the Earth

An object’s gravitational field strength depends on its MASS. A massive object, like a star, will have a very large g-field. The Moon has less mass than the Earth, so its gravitational field is much weaker – approx 1/6th of the Earth’s. This means that we could jump higher on the Moon, and objects would fall more slowly, as they experience a weaker gravitational force.


A planet with a large radius will have a weaker gravitational field at its surface, because the surface is further away from the centre of the planet.

8.04 explain that gravitational force: causes moons to orbit planets, causes the planets to orbit the Sun, causes artificial satellites to orbit the Earth, causes comets to orbit the Sun

According to Newton, there is an attractive gravitational force between any two objects– pulling them together. E.g. the planets and comets experience an attractive force towards the Sun.

Moons and artificial satellites are attracted to their planets, and so are pulled towards them.

This gravitational force keeps them moving in curved paths called orbits. The Moon does not crash into the Earth, and the planets do not crash into the Sun because they are moving.

8.05 describe the differences in the orbits of comets, moons and planets

Comets have highly elliptical orbits, with the Sun at one focus. When they come in close to the Sun they speed up, due to the larger gravitational force on them. They also develop bright tails that point away from the centre of the Sun. These are caused by tiny ice crystals that melt and break off from the comet and reflect the bright light of the Sun.

Moons have circular orbits and planets orbit in slightly squashed circles, called ellipses. 

8.08 know that a star’s colour is related to its surface temperature

Stars are classified into 7 groups according to their colours (which is due to their surface temperature); O,B,A,F,G,K,M

O are hottest (> 33 000 K and blue), M are coolest (2000 – 3700K and red)

8.09 describe the evolution of stars of similar mass to the Sun through the following stages: nebula, star (main sequence) , red giant, white dwarf

• nebula

Stars form from large clouds of dust and gas particles (nebulae) that are drawn together by gravitational forces over millions of years. As the particles get closer the temperature and pressure becomes so large that nuclear fusion of hydrogen nuclei to helium nuclei occurs.  This releases enormous amounts of energy in the form of heat and light.


• star (main sequence)

Fusion produces forces that make the star expand outwards, but gravitational force is always pulling the particles within the star inwards. When these two opposing forces become balanced a star is stable and called a main sequence star. It should stay this way for millions of years, at a constant size and temperature.


• red giant

Eventually hydrogen fusion stops as the star runs out of fuel. Gravitational force is now bigger than the outward fusion force which causes the star to collapse inwards and compress. This causes it to heat up to even higher temperatures so that fusion of helium nuclei begins. The increased power output causes the star to expand greatly. The surface area is so large that it is cooler than before, so its colour changes to red and the star is called a red giant.


• white dwarf

Eventually fusion stops when the star runs out of helium nuclei and the gravitational force causes the star to collapse inwards and compress again. This heats it up so it changes colour to emit white light. The star is squashed so greatly by the gravitational force to become a small and very dense white dwarf. (They are so dense that a teaspoon full would weigh more than a cruise liner). A white dwarf eventually cools down and change colour as it does so, eventually becoming black.

8.10 describe the evolution of stars with a mass larger than the Sun

After the stable period, a giant star expands into red supergiant. (It produces all the elements up to iron during nuclear fusion). When it finally runs out of nuclei to fuse it collapses due to the gravitational force, and then explodes – an exploding star is called a supernova.


The explosion throws dust and gas back into space and so another nebula is formed. A dense core remains – called a neutron star, because it is made entirely from neutrons. If its mass is large enough it can compress further to become a black hole. (Their gravity is so strong that not even light can escape!)

8.11 understand how the brightness of a star at a standard distance can be represented using absolute magnitude

Apparent magnitude is simply how bright a star appears in the night sky.


But, the brightness of a star depends on its distance from Earth and its luminosity – how much power it produces. (A dim star could just be very far away, or very close but not very luminous).


Absolute magnitude enables us to compare the brightness of stars because it is a measure of how bright they would appear if they were all the same distance from the Earth. – 32.6 light years.

8.12 draw the main components of the Hertzsprung–Russell diagram (HR diagram)

This diagram shows the relationship between a star’s luminosity (its brightness or power output) and its surface temperature. A star moves to different positions in the diagram during its life, as its internal structure and temperature change.


Important Note: the temperature scale is reversed. It is hotter towards the origin of the x axis.

8.13 describe the past evolution of the universe and the main arguments in favour of the Big Bang

Scientists believe that about 14 billion years ago all matter in the Universe was in one extremely tiny and dense place. It then suddenly exploded, and has been expanding ever since. This expansion is shown by the red-shift of galaxies and the energy of the explosion can be seen everywhere in the Universe as the CMBR.

8.14 describe evidence that supports the Big Bang theory (red-shift and cosmic microwave background (CMB) radiation)

If we examine the light spectra for distant galaxies we can see that the wavelengths of the light have become longer. We call this stretching of the waves ‘red-shift’. It tells us that the galaxies producing the light are moving away from us .The further away a galaxy is, the greater its red-shift, so it is moving even faster. This is evidence that the Universe is expanding and so it supports the Big Bang Theory.


Microwave radiation can be detected EVERYWHERE in the Universe. These are the stretched remains of high energy gamma radiation that would have been produced in the explosion that created the Universe. They have stretched because the Universe is expanding.

8.15 describe that if a wave source is moving relative to an observer there will be a change in the observed frequency and wavelength

This is called the Doppler Effect. If something that emits a wave moves whilst it is doing so (imagine a noisy motorbike coming towards you then going further away, emitting sound waves the whole time) then the wavelength of the sound will become shorter as it is moving towards you, increasing the frequency, and  stretched as it is moving away, decreasing the frequency.


You will hear this as a change in pitch, getting higher as it approaches and lower as it moves away. The same thing happens for a moving object that is emitting light waves –e.g. a galaxy.

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Section 1: Principles of chemistry

      a) States of matter

      b) Atoms

      c) Atomic structure

     d) Relative formula masses and molar volumes of gases

     e) Chemical formulae and chemical equations

     f) Ionic compounds

     g) Covalent substances

     h) Metallic crystals

     i) Electrolysis

 Section 2: Chemistry of the elements

     a) The Periodic Table

     b) Group 1 elements: lithium, sodium and potassium

     c) Group 7 elements: chlorine, bromine and iodine

     d) Oxygen and oxides

     e) Hydrogen and water

     f) Reactivity series

     g) Tests for ions and gases

Section 3: Organic chemistry

     a) Introduction

     b) Alkanes

     c) Alkenes

     d) Ethanol

Section 4: Physical chemistry

     a) Acids, alkalis and salts

     b) Energetics

     c) Rates of reaction

     d) Equilibria

Section 5: Chemistry in industry

     a) Extraction and uses of metals

     b) Crude oil

     c) Synthetic polymers

     d) The industrial manufacture of chemicals

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