A Guide to what you need to know EXAM 2 MUST KNOWS Exam 2 Content What and how much of what Exam 2 will cover Chapter 6 The Solar System Chapter SL General Planets Custom material Chapter 7 The Earth Part of Chapter 8 The Moon Part most of it Exam 2 structure will have 105 Points on Exam Top score 105 Multiple choice Fill in the Blank Short answer There will be bonus questions worth 5 pts total Max score possible 105 5 110 Exam 2 Content Equations to Know Hmm We haven t covered any new equations so this exam will be equation free Expect many questions that will test if you have learned the vocabulary related to these three chapters There will be a word bank for the fill in theblank Exam 1 Must Knows Chapter 5 What are the two main types of telescopes and how do they gather and focus light Reflectors using mirrors Refractors using lenses What is refraction Why are almost all professional telescopes reflectors I gave you FOUR reasons Be familiar with those Why is telescope size important Telescope area or collecting area determines how bright an object is Hence how bright something appears scales with the SQUARE of the telescope diameter Telescope diameter determines the angular resolution limit of a telescope Know what angular resolution is and that a smaller number smaller angular distance is better angular resolution Exam 1 Must Knows Chapter 5 How does telescope size relate to light gathering capacity Answer The light gathering capacity increases with the square of the telescope diameter How does telescope size relate to angular resolution proportional to What is a CCD and why is digital information a benefit to modern astronomy CCD is roughly 30x more efficient at counting the number of photons that hit it compared to photographic film Allows for digital processing and data analysis on the images data collected Exam 1 Must Knows Chapter 5 Know what atmospheric blurring i e seeing is What astronomers do to mitigate this problem High altitude observatories space based observatories technology to correct the blurring active and adaptive optics What are the two spectral windows of our atmosphere What is the basic design and advantages of radio telescopes Know that a major disadvantage of radio astronomy is its inherent angular resolution challenges due to radio waves having long wavelengths What is an interferometer how does it increase angular resolution What determines the effective diameter Exam 1 Must Knows Chapter 5 What wavelength regions are required for spacebased astronomy and what new information do the various wavelength regions provide Can see through dust in parts of IR Can see dust in IR microwave and radio Can study molecules in space with radio UV is good for looking at star formation regions of galaxies X ray and Gamma ray high energy wavelengths are good at looking at extremely hot objects such as active galactic nuclei supernovae black hole accretion disks etc Must Knows Chapter 6 The Solar System Be able to list all 8 planets in order Mercury Venus Earth Mars Jupiter Saturn Uranus Neptune Main contents of solar system SS more interested in knowing what is there rather than the specific numbers 1 Sun 8 planets four terrestrial planets four gas giant planets millions of asteroids in asteroid belt and Jupiter Trojan areas Kuiper Belt Oort Cloud The asteroid belt lies between the orbits of Mars and Jupiter The Kuiper belt lies beyond the orbit of Neptune at 30 AU and extends to about 50 AU The Oort cloud is very far away with most objects being near 50 000 AU Must Knows Chapter 6 Know that our discovery of extrasolar planetary systems has demanded a reworking of our thoughts about how planetary systems form Supermassive Jupiters orbiting closer to their host stars than our Mercury this flies in the face of a simple Nebular Hypothesis Condensation Theory and demands that planetary migration must be common and important in SS formation Planetary migration also explains the evidence of a spike in the amount of impacts on the early planets an event called The Late Heavy Bombardment Must Knows Chapter 6 Know the primary differences between terrestrial and gas giant planets Location composition size frequency and strength of magnetic fields etc All Jovian systems have ring systems no terrestrials do Difference between comets and asteroids How big are they compared to planets Density location and composition Asteroids Dense and rocky and mainly in Asteroid Belt Comets Low density rocky icy bodies that originate in Kuiper Belt or Oort Cloud Know what planet is the largest and smallest Jupiter and Mercury respectively Definition of Average Density Mass Volume for planet and what that tells us when compared to the surface density Must Knows Chapter 6 Know the NINE general characteristics of the Solar System that our formation theory has to account for I won t ask you to recite them but there will almost certainly be 1 or 2 question with respect to what these are and how our formation theory Nebular Theory Properties 1 4 Relates to structure of SS Condensation theory Properties 5 8 Mostly relates to chemical and density properties of the planets Know what Nebular Theory and Condensation Theory are how they operate what they explain and what they predict Exam will go into more depth than Quiz 3 did Know what is meant by Solar Nebula Must Knows Chapter 6 Know that the basis for condensation theory is that a temperature gradient exists in the disk such that the inner regions near the protosun are hot and the outer regions are cold Know what the ice line is the distance away form the protosun in the Solar Nebula at which water ice can condense out Know how the temperature gradient translates into the chemical and density gradient observed in the solar system What kinds of grains can you form at what distance interior to ice line Exterior to ice line How does this impact the expected size and compositions what planets are made out of of the formed protoplanets Must Knows Chapter 6 Know that the after grains form via condensation they stick together a process called accretion to form larger and larger objects planetesimals which can now influence each other gravitationally These collide to become larger protoplanets which can collide to become a planet Accretion of protoplanets builds terrestrial planets and possibly giant planet terrestrial cores Theories for how gas giant planets are made Core accretion and gravitational instability Understand that it was planetary migration of
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