Distances

Hertzsprung-Russell (H-R) diagram
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• Dark Matter (27%)
  Dark – does not emit or absorb light.
  Dark – does not collide.
  Dark – does not heat up like gas.
  Dark – providing the gravitational scaffolding for galaxies.
  Dark – hold galaxies together.
  Dark – control how fast galaxies rotate.
  Dark – anchor galaxy clusters.

The Universe’s behaviours

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• Dark Matter (27%)
  Dark – does not emit or absorb light.
  Dark – does not collide.
  Dark – does not heat up like gas.
  Dark – providing the gravitational scaffolding for galaxies.
  Dark – hold galaxies together.
  Dark – control how fast galaxies rotate.
  Dark – anchor galaxy clusters.

The Universe’s behaviours

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• Ordinary Matter (5%)
  Ordinary – the stuff made of protons, neutrons and electrons.
  Ordinary – responds strongly to gravity.
  Ordinary – can cool, radiate energy and collapses under gravity into;
  Ordinary ….stars, planets, nebulae, galaxies and galaxy clusters.

• This clumping is possible because Ordinary Matter (5%) can lose energy (through radiation), allowing it to cool and collapse – something dark matter cannot do.
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• The main different between solids, liquids, and gases is how their particles are arranged and move.
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Solids ( Rock / Ice)

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• Solids – Particles are close together and vibrate in fixed positions, giving solids a fixed shape. Solids can’t usually be compressed because there’s so little space between the particles.
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Liquids ( Water / Rain)

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• Liquids – Particles are close together but randomly arranged, allowing them to move around and over each other. Liquids have a fixed volume but no fixed shape, so they flow and take the shape of their container.
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Gas ( steam / air / gas )

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• Gases – Particles are widely spaced apart and move quickly in straight lines. Gases have no fixed shape or volume, so they expand to fill their container. Gases can be squeezed and compressed because there’s so much space between the particles.
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• Solids
  – ice/snow
  – brick
  – wood
  – iron/copper
  – car/train
  – book/paper
  – chair/table
  – apple

• Liquids
  – rain
  – water
  – petrol/oil
  – vinegar
  – paint
  – juice
  – tea
  – milk

• Gases
  – wind
  – helium
  – oxygen / air
  – carbon dioxide
  – hydrogen (gas)
  – steam
  – fog
  – smoke

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• Matters and Energy irregularly
  The universe consists of matters and matters irregularly distributed throughout the continuum of curving space-time, but most of the matter and energy is invisible to humans.
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BSL Version
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• Group and Clusters of Galaxies
  The largest astronomical objects are galaxies, followed in terms of diminishing size by nebulas, stars, planets, moons, asteroids, comets and meteorites.
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• Although galaxies are made up of many billions of stars, they are considered to be a single objects – this because their stars orbit around a common centre of gravity and have the same relative motion with respect to the rest of the Universe.
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• Astronomical objects tend towards a spherical shape because the gravitational forces across the surfaces of a sphere are in equilibrium.
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• Rotation tends to distort spherical objects into a discus-shape – the Earth, for example bulges slightly around the Equator.
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• Objects of less than about 50 miles / 80km in diameter have insufficient mass to achieve a spherical shape, which is why the smaller asteroids all have irregular shapes.
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BSL Version
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To measure the distance of a planet
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Astronomers use a baseline of
1 astronomical unit (AU),
which is the average distance
between Earth and the sun.
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BSL Version

BSL – Explaining of distance

• Sun >> Mercury
  (distance of 0.47AU = 36 million miles)
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• Sun >>>> Earth
  (distance of 1AU = 93 million miles)
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• Sun >>>>>>>>>>>> Jupiter
  (distance of 5.27AU = 483,600,000 million miles)

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• nearby stars distance is calculated by measuring the slight shift in angle of each star in comparison to stars far away, as the Earth orbits the Sun; this is called “Parallax Shift”.
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• parallax shift, it can only be used to measure nearby stars, so astronomers work out the distance to faraway stars and galaxies by comparing how bright they look with how bright they actually are.

BSL Version

• explaining about parallax shift

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• beyond classification and evolution, the Hertzsprung-Russell diagram offers invaluable insights into the fundamental properties and characteristics of stars.
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• each star’s position on the diagram reveals crucial information about its;
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  – luminosity
  – surface temperature
  – radius
  – mass
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• these classes have particular colours. Spectral type is most often written across the top of the H-R diagram going from hot, blue “O” stars (very hottest, brightest stars) on the left to cool, more red “M” stars (very coolest, dimmest stars) on the right.
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• the seven spectral classes in order of surface temperature from hottest to coolest are;
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O B A F G K M

BSL Version

• explaining about the hottest and coolest stars.