The BIg Bang (draft)

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BSL Version
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• The Big Bang is the idea that the universe began as just a single point, then expanded and stretched to grow as large as it is right now and it is still stretching.
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• One ten million trillion trillion trillionth of a second
  In order to explain what happened scientists use measurements of time that are very small.
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• At first…
  The Universe was unspeakably small and hot – getting larger and cooler ever since.
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Four fundamental forces

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• Four fundamental forces govern interactions between all objects in the universe.
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• This illustration shows above the four fundamental forces of the universe (clockwise from top left):
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  – gravity
  – electromagnetism
  – weak forces
  – strong forces
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• About one-billionth of one second after the Big Bang.
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• The Universe lay in a dense sea of quarks, where the first particles (neutrons and protons) were beginning to form.
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Dense sea of quarks

• A quark is a tiny particle which makes up protons (postive +) and neutrons (negative -).
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• About three minutes after the Big Bang there was a brief period of nucleosynthesis when quarks joined together to form protons (+), and neutrons (-).
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• First nuclei – Hydrogen and helium formed.
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• The early Universe after the Bang Big completely opaque (like a thick fog ~ no light to pass through during the dark ages).
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• Because the super-hot plasma where the light (photons) constantly scattered off free electrons and protons, preventing it from travelling far.
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• During this period, the temperature was so high that electrons and protons could not combine to form neutral atoms. 
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• This “cosmic fog” cleared as the universe expanded and cooled enough for electrons and protons to form neutral atoms (recombination), allowing light to travel freely.
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After 380,000 years…

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• The Universe cooled enough for electrons and nuclei to combine, forming neutral atoms (mostly hydrogen and helium), making the universe transparent and releasing the Cosmic Microwave Background (CMB) radiation.
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• Then it become cool enough for protons (+) and neutrons (-) to capture electrons.
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• The first atoms form.
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• After recombination, the universe was filled with neutral gas (mostly hydrogen and helium), but no stars or galaxies yet existed, so it was dark.
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• Gravity pulled gas and dark matter together, forming dense clouds that ignited into the first massive stars (Population III stars) and the first small galaxies, ending the Dark Ages.
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• The Universe remained completely opaque.
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• Then it become cool enough for protons (+) and neutrons (-) to capture electrons and form atoms.
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• The first stars began to shine.
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• Dark matter forms a scaffolding or filamentary strands across the universe, and galaxies appear along these strands.
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• Gas falls into the halo ~ ordinary matter (hydrogen, helium) is pulled into these halos as it cools and condenses, it forms: stars, star clusters and full galaxies.
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• Galaxies and Dark Matter ~ galaxies form in dark matter cradles on cosmic structure.
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• Dark matter collapes first ~ after the Big Bang, dark matter began clumping under gravity. Because it doesn’t interact with light or radiation, it could collapse earlier.
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• Without dark matter’s stabilising gravitational pull, galaxies would not have formed or held together in the shapes.
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• These clumps become “halos” ~ each halo is a gravitational bubble (a region where dark matter density is high.)
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• Today Universe is epanding faster than ever ~ driven by dark energy.
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• Cooling slowly, now around -274°C.
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• Growing more structured, with galaxies clustering into filaments and voids.
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• There is still much to be discovered about the Universe and the Big Bang.

Nucleus

• In a nutshell, atoms are the tiny bits that make up everything we see and touch, from the air to the stars. They’re made of protons, neutrons, and electrons.
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• Protons and neutrons are in the centre of each atom is a dense core called the nucleus.
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• Despite being incredibly tiny, the nucleus contains almost all of an atom’s mass. This is because the nucleus is home to two types of particles: protons and neutrons.
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• Protons – these are positively (+) charged particles found within the nucleus. The number of protons in an atom determines what element it is. (For example, an atom with one proton is hydrogen, an atom with two protons is helium, and so on.)
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• Neutrons – these are particles that have no charge (negative), hence the name ‘neutron’, which means ‘neutral’. They contribute to the mass of an atom and help to hold the nucleus together by counteracting the positive charge of the protons.
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• In a nutshell, atoms are the tiny bits that make up everything we see and touch, from the air to the stars; they’re made of protons, neutrons, and electrons.
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• Electrons are tiny particles that orbit the nucleus, similar to how planets orbit the sun.
  electrons are involved in chemical reactions and the formation of chemical bonds. They also determine the electrical and thermal conductivity of materials.
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• The arrangement of electrons in an atom can change, moving to higher energy levels or lower energy levels or even jumping from one atom to another.
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• These changes can result in the absorption or emission of light, leading to the colours we see in fireworks, neon lights, and even the rainbow!
  
  
  
  
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• Cosmology is a branch of astronomy that involves the origin and evolution of the universe, from the Big Bang to today and on into the future.
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Cosmology asks for the biggest questions:

• How did the universe begin?
• What is it made of?
• How is it changing over time?
• What will happen to it in the far furture?
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Expansion in the Universe

• future and large-scale (features are known as Cosmology.)
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• expanding and continuing getting bigger all the time.
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• most distant galaxies rush outwards in all directions – moving away from us at about 90% of the speed of light.
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• recent theories suggest that our Universe may just be one of countless bubbles of space-time – multiverses shows a cluster of interesting universes that happens to be neighbours. (See BizleyArt)
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Temperatures in the Universe

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• no maximum possible temperature in the Universe.
• accurate minimum possible temperature of -273ºc.
• working in specialised laboratories, they cannot achieve this ultimate low temperature than -273ºc.
• matter is not spread out evenly throughout the Universe.
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The Comic Web

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• Comic Web refers to the largest-scale structure of the Universe.
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• The Universe lies up of thin filaments (fibre), each one made of millions of galaxies and hot gas that surround huge empty space that contain nothing but clouds of hydrogen (gas) between galaxies.
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• A Comic Web-like pattern formed by gravity pulling matter into strands and nodes;
  ….– Filaments contain clusters of galaxies and hot gas.
  ….– Voids are huge, empty regions with very little matter.
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• The Big Bang is the idea that the universe began as just a single point, then expanded and stretched to grow as large as it is right now and it is still stretching.
  o

One ten million trillion trillion trillionth
of a second

• In order to explain what happened scientists use measurements of time that are very small.

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oooo

BSL Version

The Big Bang

o

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At first…

• the Universe was unspeakably small and hot – getting larger and cooler ever since.
  o

Four fundamental forces

• Four fundamental forces govern interactions between all objects in the universe.
  o

• This illustration shows above the four fundamental forces of the universe (clockwise from top left):
  – gravity
  – electromagnetism
  – weak forces
  – strong forces
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Science photo Library/Getty Images: Mark Garlick – Science photo, plus: adapted by L. Steenblik Hwang.

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BSL Version

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About one-billionth of one second…

• about one-billionth of one second after the Big Bang
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• the Universe lay in a dense sea of quarks and other particles – tiny pieces of anything; atoms, molecules, etc).
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Dense sea of quarks

• A quark is a tiny particle which makes up protons and neutrons.

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BSL Version

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About three minutes…

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• about three minutes after the Big Bang there was a brief period of nucleosynthesis when quarks joined together to form neutrons and protons.
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Atoms

• Atoms are the smallest units of an element that still retain the properties of that element.

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Nucleus

• In a nutshell, atoms are the tiny bits that make up everything we see and touch, from the air to the stars. They’re made of protons, neutrons, and electrons.

• protons and neutrons are in the centre of each atom is a dense core called the nucleus.
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• despite being incredibly tiny, the nucleus contains almost all of an atom’s mass. This is because the nucleus is home to two types of particles: protons and neutrons.
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• protons – these are positively (+) charged particles found within the nucleus. The number of protons in an atom determines what element it is. (For example, an atom with one proton is hydrogen, an atom with two protons is helium, and so on.)
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• neutrons – these are particles that have no charge (negative), hence the name ‘neutron’, which means ‘neutral’. They contribute to the mass of an atom and help to hold the nucleus together by counteracting the positive charge of the protons.
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• in a nutshell, atoms are the tiny bits that make up everything we see and touch, from the air to the stars; they’re made of protons, neutrons, and electrons.
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BSL Version

• explaining about three minutes…

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BSL Version

• explaining about nucleus

Electrons

Electrons are tiny particles that orbit the nucleus, similar to how planets orbit the sun.
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• they carry a negative charge, which balances the positive charge of the protons in the nucleus.
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• electrons are involved in chemical reactions and the formation of chemical bonds. They also determine the electrical and thermal conductivity of materials.
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• The arrangement of electrons in an atom can change, moving to higher energy levels or lower energy levels or even jumping from one atom to another.
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• These changes can result in the absorption or emission of light, leading to the colours we see in fireworks, neon lights, and even the rainbow!

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BSL Version

• explaining about electrons