1. Energy! (gamma photons and neutrinos) 100sec100,000 years Too hot for matter to form 13 P3 4.1 Galaxies C* Describe how the Universe changed after the Big Bang A* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

2. Quarks and electrons form after 0.1sec Energy! (gamma photons and neutrinos) 100sec100,000 years Too hot for matter to form 13 P3 4.1 Galaxies C* Describe how the Universe changed after the Big Bang A* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

3. Quarks and electrons form after 0.1sec Energy! (gamma photons and neutrinos) 100sec100,000 years Plasma soup – universe is in a hot ionised state and is opaque Too hot for matter to form 13 P3 4.1 Galaxies C* Describe how the Universe changed after the Big Bang A* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

4. Quarks and electrons form after 0.1sec Energy! (gamma photons and neutrinos) 100sec100,000 years Plasma soup – universe is in a hot ionised state and is opaque Radiation de-couples from matter at 300,000 yrs. Background microwave energy is released. Universe becomes cold and dark except where gravity attracts uncharged atoms to form protostars fusing hydrogen to helium. Gravity pulls groups of stars together to form galaxies. Too hot for matter to form 13 P3 4.1 Galaxies C* Describe how the Universe changed after the Big Bang A* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

5. Quarks and electrons form after 0.1sec Energy! (gamma photons and neutrinos) 100sec100,000 years Plasma soup – universe is in a hot ionised state and is opaque Radiation de-couples from matter at 300,000 yrs. Background microwave energy is released. Universe becomes cold and dark except where gravity attracts uncharged atoms to form protostars fusing hydrogen to helium. Gravity pulls groups of stars together to form galaxies. Too hot for matter to form Large stars go supernova and fuse the heavier elements which condense to form new stars and rings of debris which condense into planets 13

6. Radiation de-couples from matter at 300,000 yrs. Background microwave energy is released.

7. Uncharged atoms don’t repel each other

8. During the dark age of the universe (first few billion years) gravity slowly pulled gas clouds of mainly hydrogen into clumps which formed stars and galaxies lighting up the universe. Uncharged atoms don’t repel each other

9. All the while the universe is expanding. Uncharged atoms don’t repel each other During the dark age of the universe (first few billion years) gravity slowly pulled gas clouds of mainly hydrogen into clumps which formed stars and galaxies lighting up the universe.

10. Uncharged atoms don’t repel each other During the dark age of the universe (first few billion years) gravity slowly pulled gas clouds of mainly hydrogen into clumps which formed stars and galaxies lighting up the universe. All the while the universe is expanding. Evidenced by ? ?

11. Light from the most distant galaxies has taken billions of years to reach us. Uncharged atoms don’t repel each other During the dark age of the universe (first few billion years) gravity slowly pulled gas clouds of mainly hydrogen into clumps which formed stars and galaxies lighting up the universe. All the while the universe is expanding. Evidenced by ? ?

12. The lumpiness of the Universe is a direct result of early fluctuations in the structure

13. The lumpiness of the Universe is a direct result of early fluctuations in the structure

14. The lumpiness of the Universe is a direct result of early fluctuations in the structure

15. The lumpiness of the Universe is a direct result of early fluctuations in the structure

17. 90% of the mass of the universe is missing! Astronomers can measure the mass of galaxies but the number of stars in them is not enough to account for their rapid rotations. There are a few theories about where this mass is, including brown dwarf stars neutrinos and super massive black holes!

18. 90% of the mass of the universe is missing! Astronomers can measure the mass of galaxies but the number of stars in them is not enough to account for their rapid rotations. There are a few theories about where this mass is, including brown dwarf stars neutrinos and super massive black holes!

19. 90% of the mass of the universe is missing! Astronomers can measure the mass of galaxies but the number of stars in them is not enough to account for their rapid rotations. There are a few theories about where this mass is, including brown dwarf stars neutrinos and super massive black holes!

21. If a gamma ray burst happened anywhere within a couple of hundred light years of us, the gamma radiation would be intense enough to kill everything on the Earth.