1. Please press “1” to test your transmitter. :10 0 of 5 1.1 2.2 3.3 4.4 5.5 Review for Midterm II 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

2. The pre-birth phase of a star is called … :10 0 of 5 1.Baby star 2.Pre-star 3.Starillo 4.Protostar 5.supernova 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

3. Protostars Protostars = pre-birth state of stars: Hydrogen to Helium fusion not yet ignited Still enshrouded in opaque “cocoons” of dust => barely visible in the optical, but bright in the infrared.

4. Dense pockets gas in a giant molecular cloud which ultimately form stars, are called … :10 0 of 5 1.Starlets 2.Globules 3.Open star clusters 4.Star pockets 5.protostars 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

5. (Bok) Globules ~ 10 – 1000 solar masses; Contracting to form protostars Compact, dense pockets of gas which may contract to form stars.

6. From Mercury to Neptune, the average density of the planets … :10 0 of 5 1.Steadily decreases 2.Steadily increases 3.Remains almost constant. 4.Increases throughout the terrestrial planets, then decreases. 5.Decreases throughout the terrestrial planets, then increases. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

7. Condensation in the Early Solar System Only condensed materials could stick together to form planets Temperature in the protostellar cloud decreases outward. Further out → Protostellar cloud is cooler → lighter metals with lower melting point condensed → change of chemical composition throughout solar system Lighter substances condense at lower temperatures. → Average density of planets decreases outwards! The Condensation Sequence Temperature (K)CondensatePlanet (Estimated Temperature of Formation; K) 1500Metal OxidesMercury (1400) 1300Metallic iron and Nickel 1200Silicates 1000FeldspatsVenus (900) 680Troilite (FeS)Earth (600) Mars (450) 175H2O iceJovian pl. (175) 150Ammonia - water ice 120Methane – water ice 65Argon – neon icePluto

8. Planets orbiting stars other than our sun are scientifically called … :10 0 of 5 1.Alien Worlds 2.Extragalactic planets 3.Extra-universal planets 4.Extrasolar planets 5.Jovian planets 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

9. Extrasolar Planets All stars have gone through basically the same formation process as the sun. → Many stars should have planets! Extrasolar are very hard to image directly. → planets orbiting around other stars = “Extrasolar planets” Detection using the “wobbling” technique: Look for “wobbling” motion of the star due to the gravitational pull of the planet on the star.

10. How did the Jovian planets grow? :10 0 of 5 1.Only by random encounters with rocky clumps in the protoplanetary cloud. 2.First by random encounters with rocky clumps, then by gravitational attraction. 3.First by gravitational attraction of gas and dust, then by random encounters with rock and gas clumps. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

11. The Story of Planet Building Planets formed from the same protostellar material as the sun. Rocky planet material formed from clumping together of dust grains in the protostellar cloud. Mass of less than ~ 15 Earth masses: Planets can not grow by gravitational collapse Mass of more than ~ 15 Earth masses: Planets can grow by gravitationally attracting material from the protostellar cloud Earthlike planets Jovian planets (gas giants)

12. What is differentiation? :10 0 of 5 1.Centrifugal forces flinging heavy metals out to the outer layers of a planet, while lighter materials remain near the core. 2.The sun’s gravity pulling heavier metals towards it, while lighter ones remain at the opposite side. 3.Heavier metals sinking to the cores of planets, while the lighter ones remain in the crust. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

13. The Growth of Protoplanets As rocks melted, heavier elements sink to the center → differentiation → Terrestrial planets have heavy-metal (iron) cores and mantles of lighter substances

14. Near the Earth’s center, we find … :10 0 of 5 1.A core of solid iron. 2.A core of liquid iron. 3.A core of liquid silicon-based rocks. 4.A core of solid silicon-based rocks. 5.A core of pure gold. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

15. Earth’s Interior (II) Earth’s interior gets hotter towards the center. Earth’s core is as hot as the sun’s surface; metals are liquid near the core. Basic structure: Solid crust (light [Si-based] materials) Solid mantle (light elements, iron-poor) Liquid core (iron-rich) Solid inner core (iron-rich)

16. Seismic waves are bent or bounce off transitions between different materials or different densities or temperatures. Earth’s Interior Direct exploration of Earth’s interior (e.g. drilling) is impossible. Earth’s interior can be explored through seismology: Earth quakes produce seismic waves.

17. Earth quakes, tsunamis, and volcanic activity on Earth occur predominantly near … :10 0 of 5 1.large oceans. 2.the core of the Earth. 3.the centers of large continents. 4.the boundaries of tectonic plates. 5.the top of the atmosphere. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

18. Geological activity around the Pacific Volcanism: Mt. St. Helen Earthquakes: Kobe (Japan) Volcanism: Pinatubo (Philippines) Earthquakes: San Francisco

19. Volcanoes related to subduction zones are found … :10 0 of 5 1.Only on Earth. 2.Only on Mars. 3.Only on Venus. 4.Only on Mercury. 5.On all terrestrial planets. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

20. Shield Volcanoes Found above hot spots: Fluid magma chamber, from which lava erupts repeatedly through surface layers above. All volcanoes on Venus and Mars are shield volcanoes Volcanism on Earth (II)

21. The Alps have been formed by the collision between … :10 0 of 5 1.The North American and the South American Plate 2.The Pacific Plate and the Eurasian Plate 3.The Eurasian and the North American Plate 4.The Afrian and the Eurasian Plate 5.The Afrian and the Indian-Australian Plate. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

22. Earth’s Tectonic History

23. History of Geological Activity Surface formations visible today have emerged only very recently compared to the age of Earth.

24. X-rays from space interact with the atmosphere primerily through … :10 0 of 5 1.The dissociation of ozone molecules. 2.Inducing rotations of air molecules in the troposphere. 3.Inducing vibrations of air molecules in the troposphere. 4.Ionizing atoms and molecules in the Exosphere and Thermosphere. 5.Not at all: X-rays traverse the atmosphere nearly unabsorbed. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

25. The Electromagnetic Spectrum Need satellites to observe Wavelength Frequency High flying air planes or satellites

26. The Temperature Structure of Earth’s Atmosphere Exosphere: Heated by UV and X-rays from space Thermosphere: Heated by X-rays from space Stratosphere: Heated by UV radiation from space Troposphere: Heated by greenhouse effect Ozone Layer Atmosphere gets colder at larger distance from heat sources. Top of Ozone Layer Temperature Altitude

27. The most essential step in the greenhouse effect is … :10 0 of 5 1.The dissociation of ozone molecules by ultraviolet light. 2.The ionization of air molecules by X-rays. 3.The heating of air molecules by gamma-rays. 4.The absorption of infrared light by complex molecules in the stratosphere. 5.The absorption of optical light by complex molecules in the stratosphere. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

28. The Interactions between Light and Molecules Carbon dioxide (CO 2 ) / Water vapor (H 2 O) / any other asymmetric molecules (greenhouse gases) Infrared Causes asymmetric molecules to rotate This is the essential step of the Greenhouse Effect!

29. Which of the following is a greenhouse gas? :10 0 of 5 1.Hydrogen (H 2 ) 2.Oxygen (O 2 ) 3.Nitrogen (N 2 ) 4.Ammonia (NH 3 ) 5.All of the above. 1234567891011121314151617181920 2122232425262728293031323334353637383940 4142434445464748495051525354555657585960 6162636465666768697071727374757677787980 81828384858687888990919293949596979899100 101102103104105106107108109110111112113114115116117118119120 121122123124125126127128129130131132133134135136137138139140 141142143144145146147148149150151152153154155156157158159160 161162163164165166167168169170171172173174175176177178179180 181182183184185186187188189190191192193194195196197198199200 201202203204205206207208209210211212213214215216217218219220 221222223224225226227228229230231232233234235236237238239240 241242243244245246247248249250

30. Gases consisting of compounds of two or more different types of atoms: CO 2 (carbon dioxide) H 2 O (water vapor) CH 4 (methane) NH 3 (Ammonia) Greenhouse Gases Most common gases in Earth’s atmosphere (N 2, O 2 ) do not contribute to the greenhouse effect.