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Evolution of the Sun
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Transcript
Evolution of the Sun
The Birth of the Sun
1
How are Stars Born?
The Big Bang Theory
- Most of the atoms and molecules that existed in the early Universe were Hydrogen and Helium.
- Large waves of energy pushed them closer to each other and gravitational forces lead them to collapse in on themselves.
Energy
- Energy is emitted and recieved by surrounding cosmos.
- Very large impact on Earth's atmospheres, climate, oceans, life, weather, radio communications, energy, magnetic fields, and so much more.
2
Faint Sun Paradox
#1
It is thought that the Sun was much weaker billions of years ago than it is today. If that is the case then questions arise about how the Earth stayed warm enough to keep life going instead of turning into a ball of ice.
#2
Journal of Geophysical Research
Solar Wind production was much stronger billions of years ago which may have caused the Earth to be warmer than expected
#3
NASA
Our young Sun was much more violent than it is today coronal mass ejections
3
Solar Flares
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What is it?
- Magnetic Energy built up in the solar atmosphere that is suddenly released.
- Emitted across the entire electromagnetic spectrum
- most dangerous emissions are energetic charged particles (high energy protons) and electromagnetic radiation (x-rays).
Impact
How does it affect us?
- We are phycially protected by the Earth's magnetic field and the atmosphere.
- Disturbs Earth's ionosphere radio communications.
- Solar flares can temporarily alter the upper atmosphere creating disruptions with signal transmission from satelittes (airplane navigation, financial clocks, GPS, cell-phone reception, power grids, & radio broadcasts)
What Can We Do?
NASA and NOAA's space weather prediction center helps us predict when solar flares are coming so that we can take necessary precautions.
Evolution of the Sun
4
What it is now and what it will become
Main Sequence
Main Sequence
- The most common star. Make up about 90% of all stars in the Universe.
- Main sequence stars maintain a spherical shape because as pressure from fusion is pushed out, gravity from inward pulls the gases in creating a hydrostatic balance.
- Their size, gravitational pull, and life expectancy are functions of the star’s mass.
- The Sun is expected survive for about 10 billion years on the main sequence before turning into a red giant and then eventually a white dwarf.
Runaway Greenhouse Effect
Runaway Greenhouse Effect
- As the Sun's energy increases & the amount of greenhouse gases in the atmosphere increases we will see an increase in the temperature of the Earth.
- If this temperature reaches the boiling point of water we can expect the oceans to vaporize and increase the effectiveness of heat-trapping.
- Accelerate the greenhouse effect = oceans evaporate faster and faster. Once the oceans are gone the atmosphere will stablize at a much higher temperature than what it is now.
Continued ...
Suppose the Earth's tempertaure increased so much that it caused chemical reactions to occur that drive the carbon dioxide out of the rocks and into the atmosphere ...
Red Giants & White Dwarfs
Red Giants & White Dwarfs
- The Sun will eventually burn out all of its hydrogen and begin buring helium. This is a Red Giant.
- Sun's atmosphere = to at least the size of the orbit of Mercury and at most the size of the orbit of Venus.
- Using up more nuclear fuel every six billion years than it ever did in its eleven billion years in the main sequence phase.
- Once the Sun has exhausted all of its fuel, it will become a White Dwarf.
Death of the Sun
5
The End of Our Solar System
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