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| “Science is the systematic enterprise of gathering knowledge about the world and organizing and condensing that knowledge into testable laws and predictions” –E.O. Wilson |
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1. Ask Question
2. Background research
3. Hypothesis
4. Experiment
5. Analyze Results
6. Report Results |
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| A well substantiated explanation of some aspect of the natural world that can incorporate facts, laws, logical inferences and tested hypotheses |
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| elements that compose living tissue |
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CNOHPS:Carbon, Nitrogen, Oxygen, Hydrogen, Phosphorus
Sulfur |
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| living components of a system |
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| non living components of a system |
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| number of protons in an element (H:1, C:6) |
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| average mass of atoms of an element, calc. using the relative abundance of isotopes in a naturally occurring element (C: 12.001, N:14.007) |
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| Atoms with the same number of protons but different number of neutrons (C12 = 6 p 6n, C14 = 6p 8n), Trace food webs, radioactively trace elements in nature |
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13.7 billion years ago
just seconds after… began to form H/He (est. 300 secs) |
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| high temperatures cause atoms to bind together 13.7 million years ago |
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12.7 billion years ago: stars formed and with them other heavier elements, bringing together different elements to make heavier elements (high temp, high pressure)
4He + 4He → 8Be
8Be + 4He → C12
C12 + He 4 → O16 |
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| How many stars are there? |
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Definition
Milky Way: 200-400 billion (low est.)
There might be 3000 galaxies (in a pin hole view of space)
All sand grains in every beaches = low est. of amt of stars
And then multiply by 1000 to 10000
Can produce a lot of carbon |
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| Emmanuel Swedenborg, Around a star is gas and dust → collide to make bigger objects, Solar Nebular Disk Model |
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Definition
a large, diffuse cloud of gas, star forms in center
As it moves it flattens out and then things begin to segregate into light and heavy elements (Heavier closer to center)
Spinning/movement of particles
Formation of protoplanets
Reason we have the solar system we have today
Closer to sun are rocky planets, further away is gaseous planets |
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Definition
Est. 4.570 billion years old
Meteorites give us access to debris left over from the formation of the solar system
Date meteorites using radioactive isotopes
Geologic time
0.12 Million years ago homo sapiens |
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| Factors of heating/melting in the early earth's interior |
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Definition
collisions: transfer of kinetic energy into heat
compression
radioactivity of elements (e.g. uranium, potassium, or thorium) decay causes the planet to heat up |
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100 million years after intial accretion, temperatures at depths of 400-800 km below the earth’s surface reach the melting point of iron
density stratification: the heavier elements, including the melted iron began to sink into the core of the earth
crust forms |
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Definition
Mass per unit volume g/cm3o Water: 1 g cm3
Glass: 2.5g cm3
Lead: 11.34g cm3
Mercury: 13.54g cm3
Gold: 19.30g cm3 |
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| Global chemical differentiation |
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| chemical separation was completed by about 4.3 billion years ago, and the earth had developed a inner and outer core, a mantle and crust |
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| chemical composition of earth |
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| each of the major layers has a distinctive chemical composition, with the crust being quite different from the earth as a whole |
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| formation of moon; 50 mil yrs after the intial creation of earth, giant planet the size of mars hit the earth made a huge crator and pushed elements away to create the moon, couldn’t go to far because of the gravitational pull |
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| evidence for giant impact hypothesis |
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Definition
Moon rock is younger than other celestial bodies
Moon rock is composed of rock similar to earth
Much less dense than earth/other planets
So no iron core
The earth is tilted 23.5 degress instead of its being on a perfect axis |
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Partial melting resulted in outgassing about 4 bil. Yr ago
Similar to gases emitted from volcanoes
Mainly water vapor
CO2, H |
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