2.  There are still many people who have not turned in their 100 point project or 100 point research packet. You wont pass this 9 weeks without those! I wont accept it after Friday!  If you skipped last Friday, you missed a quiz. If you need to make it up, it has to be before you leave for winter break, I will not let anybody make up work after we get back…especially if you missed it while skipping.

3.  Understand how our view of the solar system has changed over time and how discoveries made have led to our changing our view of the solar system.  Learn planetary characteristics such as number of moons, size, composition, type of atmosphere, gravity, temperature and surface features.  Understand the movement of planetary bodies.  Understand which planetary characteristics are more important than others when it relates to our understanding of other worlds.  Understand how proximity to the sun influences planets.  Understand the methods and tools scientists use to learn about other planets and moons in our solar system.  Understand the conditions needed for a habitable world and determine if there are habitable worlds in our solar system or outside the solar system.  Understand how we look for and study solar systems other than our own. 1.Complex Knowledge: demonstrations of learning that go aboveand above and beyond what was explicitly taught. 2.Knowledge: meeting the learning goals and expectations. 3.Foundational knowledge: simpler procedures, isolated details, vocabulary. 4.Limited knowledge: know very little details but working toward a higher level.

5.  Pluto  Mars  Venus  Titan  Earth  Jupiter

6. Today’s questions:  What is the difference between temperature, heat, and electromagnetic radiation?  What happens to the light from the Sun once it reaches a planet?  What is the greenhouse effect?  How can we determine how much light actually reaches a planet?

7.  Temperature: measure of the average energy of particles (atoms and/or molecules) in objects or systems  Heat: another word for a form of energy (thermal) related to the internal energy of an object or system and the changes within a system  Electromagnetic radiation: form of energy (other examples: chemical, kinetic, potential) that travels at the speed of light

8.  Some energy is absorbed by the planet and helps to determine a planet’s temperature.  But, the energy available to all planets is not the same. If all else were equal, the farther a planet is from the Sun, the lower the planet’s surface temperature would be.  But, not everything is equal.

10.  Reflect: change direction of radiation  Absorb: radiation is taken up or in by another molecule or atom  Transmit: radiation passes through  Balance temperature  Protect from dangerous radiation  Protect from debris  Change the surface with wind and weather patterns  Contain gases that affect temperature

11.  Gases that are made of molecules that can store large amounts of energy due to their structure

13. Composition of dry atmosphere, by volume - ppmv: parts per million by volumeparts per million GasVolume NitrogenNitrogen (N 2 )780,840 ppmv (78.084%) OxygenOxygen (O 2 )209,460 ppmv (20.946%) ArgonArgon (Ar)9,340 ppmv (0.9340%) Carbon dioxideCarbon dioxide (CO 2 )394.45 ppmv (0.039445%) NeonNeon (Ne)18.18 ppmv (0.001818%) HeliumHelium (He)5.24 ppmv (0.000524%) MethaneMethane (CH 4 )1.79 ppmv (0.000179%) KryptonKrypton (Kr)1.14 ppmv (0.000114%) HydrogenHydrogen (H 2 )0.55 ppmv (0.000055%) Nitrous oxideNitrous oxide (N 2 O)0.325 ppmv (0.0000325%) Carbon monoxideCarbon monoxide (CO)0.1 ppmv (0.00001%) XenonXenon (Xe)0.09 ppmv (9×10 −6 %) (0.000009%) OzoneOzone (O 3 )0.0 to 0.07 ppmv (0 to 7×10 −6 %) Nitrogen dioxideNitrogen dioxide (NO 2 )0.02 ppmv (2×10 −6 %) (0.000002%) IodineIodine (I 2 )0.01 ppmv (1×10 −6 %) (0.000001%) AmmoniaAmmonia (NH 3 )trace Not included in above dry atmosphere: Water vaporWater vapor (H 2 O) ~0.40% over full atmosphere, typically 1%-4% at surface

14.  Though astronauts and cosmonauts often encounter striking scenes of Earth's limb, this unique image, part of a series over Earth's colorful horizon, has the added feature of a silhouette of the space shuttle Endeavour. The image was photographed by an Expedition 22 crew member prior to STS-130 rendezvous and docking operations with the International Space Station.  The orange layer is the troposphere, where all of the weather and clouds which we typically watch and experience are generated and contained. This orange layer gives way to the whitish Stratosphere and then into the blue Mesosphere.

16.  If we didn’t have a greenhouse effect on Earth, it would be uninhabitable.  Earth’s average temperature now : 15 ∘ C, 60 ∘ F  Earth’s average temperature if our atmosphere was different: -17 ∘ C, 0 ∘ F

17. Inverse square law:  Amount of light an object receives from a source decreases by the square of the distance between the object and that source *works for gravity too!

19. Intensity of radiation at planet = 1370W/m 2 X 1AU (distance: Sun to planet in AU) 2 1370W/m 2 = solar constant (what we get on earth) Calculate intensity of radiation for: 1. Earth 2. Mars 3. Mercury 4. Neptune 5. Saturn 6. Pluto

20.  Albedo (reflectivity)  Ice :.80 or 80% reflected  Earth:.40 or 47% reflected  Asphalt :.04 or 4% reflected  Atmosphere  Reflection, Absorption, Transmission  Greenhouse gases in the atmosphere  Distance  Inverse square law

22. Answer Today’s Questions:  What is the difference between temperature, heat, and electromagnetic radiation?  What happens to the light from the Sun once it reaches a planet?  What is the greenhouse effect?  How can we determine how much light actually reaches a planet?

23.  Imagine you meet someone who did not know Earth had an atmosphere or what “atmosphere” even means.  How would you explain to him or her what an atmosphere is and why it is important?

24.  Use the 4 articles: a planet’s temperature the importance of an atmosphere the greenhouse effect – venus, Earth and mars the inverse square law To help add to your understanding of a planet’s temperature.

26. MercuryVenusEarthMarsJupiterSaturnUranus Neptune Rotation (hours) 140758322424.69.910.717.216.1 Revolution (years).24.6111.8811.929.4483.8163.8

27. We should be concerned about changes in the concentration of greenhouse gases in Earth’s atmosphere and the effects of such changes. We do not need to be concerned about changes in the concentration of greenhouse gases in Earth’s atmosphere and the effects of such changes.

28.  We SHOULD NOT be concerned about GHG on Earth.  Earth needs ghg to be habitable, they regulate/balance temperature  Important to other organisms (plants)  Most of our atmosphere is not ghg, and steps are being taken to reduce ghg emissions  The Earth normally goes through periods of hot and cold.  We SHOULD be concerned about GHG on Earth.  More ghg and higher temperatures than ever before  Our gh effect could spiral out of control and turn our planet into one like Venus  Temperature increases from ghg trapping energy are changing ecosystems (some catastrophically, some only a little)