The Sun and the Origin of the Solar System. Mid-sized, G-type main sequence star Distance: 1 AU =...
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Transcript of The Sun and the Origin of the Solar System. Mid-sized, G-type main sequence star Distance: 1 AU =...
![Page 1: The Sun and the Origin of the Solar System. Mid-sized, G-type main sequence star Distance: 1 AU = 150 million km away Size: Actual radius 700,000 km =](https://reader036.fdocuments.us/reader036/viewer/2022062305/56649e3a5503460f94b2c6cf/html5/thumbnails/1.jpg)
The Sun and the Origin of the Solar System
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• Mid-sized, G-type main sequence star• Distance: 1 AU = 150 million km away• Size: Actual radius 700,000 km = 100 Earths• Temperature, Luminosity (surface) T = 6000 K
http://www.nasa.gov/multimedia/videogallery/index.html
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• 99.86% of the total mass of the Solar System• 75% hydrogen, 23% heliun• 2% O, C, Ne, Fe
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Sunspots• surface areas that are darker than
surroundings (lower temperatures)• regions of intense magnetic activity
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Solar Evolution
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Star (Sun) formation
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Stellar Evolution
• The Sun is a middle-aged, low-mass, main-sequence star • 5 billion years ago:
– Beginning of its life on main-sequence – Sun had 1/3 luminosity it has now.
• 5 billion years from now: – End of its life on main-sequence – Sun will have twice the luminosity it has now.
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• When H is exhausted, core shrinks. • Heats up• High temperatures ignites a shell of H around
the core. • Increased pressure drives the envelope of the
star outward. • Creates a Red giant
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– Contraction of core, raises the temperature – Ignites He shell around the core – Eventually the core stabilizes– Envelope is ejected as a "planetary nebula" – The core remains as a "white dwarf"
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Solar system formation
• Starting point: – A cloud of interstellar gas and dust, the
"solar nebula“– Most of it (98%) is hydrogen and helium, includes
dust grains of heavier material, formed in previous generations of stars.
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• Contraction• Accretion disk• Protostar• Condensation• Planetesimals
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Asteroid Belt
• Small bodies in the inner solar system • Asteroid Belt between Mars & Jupiter. • Orbits are strongly influenced by
Jupiter. • Made of rock, metal, or a mix of the
two.
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• >300,000 asteroidal objects • >150,000 with good enough orbits to give
official numbers • ~15,000 asteroids with official manes • When you know its orbit, you can name it.
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Examples of asteroid names
• Ceres (largest – 914 km)• Eros (landed on in2001 Feb 12)
• Bach • Beethoven • Lennon
• McCartney • Santana • Clapton
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Irregular shape• Too small for gravity to make them spherical
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Composition of Asteroids
• C-type: "Carbonaceous" – mostly carbon-bearing materials. ~75% of all asteroids.
• S-type: "Silicaceous" - mostly of silicates (stony or stony iron). 17% of all asteroids.
• M-type: "Metallic" - probably iron-rich
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Asteroid Origins
• fragments of larger, differentiated bodies shattered by collisions
• remnants of more primordial material that never got differentiated
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Impact with Earth
Would disrupt climates and trigger mass extinctions
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Meteoroids
• Chunks of rock & iron smaller than asteroids orbiting the Sun• Sizes range from grains to 100 meters across
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Meteor
• Streak of light when a meteoroid enters the Earth's atmosphere
• Most are tiny grains• Meteor showers are trails of
debris left behind by passing comets
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Meteorite
• Any remnant that reaches the ground intact.
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Russian Meteorite
• http://www.youtube.com/watch?v=90Omh7_I8vI
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Meteor Impacts• About 100 tons of meteoroids hit the Earth
each day• Most are no bigger than grains of sand or
smaller
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Earth Impact Effects Program
http://impact.ese.ic.ac.uk/ImpactEffects/
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Comets Small bodies consisting of aggregates of ices
mixed with rock & dust
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• As they approach the Sun, they heat up and the ices sublimate (go from solid to gas):
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Halley's Comet• In 1705, Edmund Halley computed the orbit of
the great comet of 1682 using Newton's laws • Found that orbit of 1682 comet was the same
as comets seen in 1531 & 1607. • Predicted return in 1758.• Seen again on Christmas day 1758, 12 years after Halley's death
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Origin of Comets
• Short-period comets are from the Kuiper Belt• Long-period comets are from the Oort Cloud
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Structure of Comets
• Nucleus: – Dirty snowball of ices & dust – >99% the mass of the comet
• Coma– Bright "head" of the comet– Low-density cloud of gas & dust sublimed off the
nucleus – Extends out to 100,000 km or more
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• Comets have two tails– Dust Tail, dusty particles swept back in a curved
path by solar radiation, white– Ion Tail, ionized atoms & molecules swept straight
back by the solar wind, blue
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Comet Orbits
• Typically have a high degree of eccentricity
http://www.windows2universe.org/comets/comet_model_interactive.html
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Kuiper Belt• Region of the Solar System beyond the planets
extending from the orbit of Neptune (at 30 AU) to approximately 55 AU from the Sun
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Oort Cloud
• Cloud of comets which may lie roughly 50,000 AU, or nearly a light-year, from the Sun.
• Nearly a quarter of the distance to Proxima Centauri, the nearest star to the Sun