Energy!(gamma photons

and neutrinos)

100sec 100,000 years

Too hot for matter

to form

13

P3 4.1 GalaxiesC* Describe how the Universe changed after the Big BangA* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

Quarks and electrons form after 0.1sec

Energy!(gamma photons

and neutrinos)

100sec 100,000 years

Too hot for matter

to form

13

P3 4.1 GalaxiesC* Describe how the Universe changed after the Big BangA* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

Quarks and electrons form after 0.1sec

Energy!(gamma photons

and neutrinos)

100sec 100,000 years

Plasma soup – universe is in a hot

ionised state and is opaque

Too hot for matter

to form

13

P3 4.1 GalaxiesC* Describe how the Universe changed after the Big BangA* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

Quarks and electrons form after 0.1sec

Energy!(gamma photons

and neutrinos)

100sec 100,000 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 attractsuncharged 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 GalaxiesC* Describe how the Universe changed after the Big BangA* Explain how gravitational forces brought matter together to form structures like galaxies and stars.

Quarks and electrons form after 0.1sec

Energy!(gamma photons

and neutrinos)

100sec 100,000 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 attractsuncharged 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

Radiation de-couplesfrom matter at 300,000 yrs.

Background microwave energy is released.

Uncharged atomsdon’t repel each other

During the dark age of the universe (first few billion years) gravity slowlypulled gas clouds of mainly hydrogeninto clumps which formed stars and galaxies lighting up the universe.

Uncharged atomsdon’t repel each other

All the while the universeis expanding .

Uncharged atomsdon’t repel each other

During the dark age of the universe (first few billion years) gravity slowlypulled gas clouds of mainly hydrogeninto clumps which formed stars and galaxies lighting up the universe.

Uncharged atomsdon’t repel each other

During the dark age of the universe (first few billion years) gravity slowlypulled gas clouds of mainly hydrogeninto clumps which formed stars and galaxies lighting up the universe.

All the while the universeis expanding .Evidenced by ? ?

Light from the most distant galaxies has taken billions of years to reach us.

Uncharged atomsdon’t repel each other

During the dark age of the universe (first few billion years) gravity slowlypulled gas clouds of mainly hydrogeninto clumps which formed stars and galaxies lighting up the universe.

All the while the universeis expanding .Evidenced by ? ?

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

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

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

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

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!

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!

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!

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.