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How to study for this course Before coming to class: Read the corresponding chapter, or at least scan through the chapter and read the main headings. You must read the summary at the end of each chapter. Be aware of the topics to be discussed in class. During Class: Do not sleep or socialize during lecture, pay attention to lecture; and most of all, take notes: CORNELL NOTE METHOD. IMPORTANT: this is not a dictation class; you need to develop a note taking system. It is impossible to write every word from my power point presentations. Write the main issue or topic. If extra time you can expand. After Class: With you Conrell Notes in hand, go back to the textbook and expand your notes. Prepare index cards for reviewing with your study group before the exam Ch01-intro-nat-dis GLY3034: WEEK 1 1 1. Living organisms have been on Earth for about 80% of Earth's Ch01-intro-nat-dis history (p. 3) GLY3034: WEEK 1 2 The Scientific Method Collection of data By observation, by experimentation Formulation of Hypothesis (working model) Testing and modification of hypothesis Theory (or Principle or Law) 2. A theory is a hypothesis that has withstood many scientific tests (p. 4). Ch01-intro-nat-dis 3. Hypothesis, theory, and research are parts of the scientific method; an opinion is not! (p. 4) GLY3034: WEEK 1 3 Modern Theory and Practice of Geology 4. According to the principle of uniformitarianism, geologic processes we observe today have operated Ch01-intro-nat-dis GLY3034: WEEK 1 in the past 4 The Origin of Our System of Planets: The Nebular Hypothesis 5. the Big Bang took place approximately 10–15 billion years ago 7. Nuclear fusion is the process in which hydrogen atoms combine to form helium under intense pressure and high temperature. Ch01-intro-nat-dis GLY3034: WEEK 1 5 The Origin of Our System of Planets 10. Gravitational attraction and collisions caused dust and condensing material to accrete into planetesimals Ch01-intro-nat-dis GLY3034: WEEK 1 6 Formation of Nebula: Rotating clouds of gas and dust The two most abundant elements in nebulae (gas clouds) in the universe are Hydrogen and helium. Ch01-intro-nat-dis GLY3034: WEEK 1 7 The Origin of Our System of Planets 11. The four inner planets are small, rocky, and relatively lacking in volatile elements (p. 6) 12. The giant outer planets are composed mostly of hydrogen and helium (p. 7) 14. The Earth is approximately 4.6 billion years old (p. 8) Ch01-intro-nat-dis GLY3034: WEEK 1 8 8. According to the nebular hypothesis, the inner planets are dense and rocky because the inner planets were the first to condense from the solar nebula (p. 6) Ch01-intro-nat-dis 9. the following are examples of giant outer planets Saturn, Neptune, Pluto (p. 6) GLY3034: WEEK 1 9 Evolving Earth: A System of Interacting Components 15. The process by which an originally homogeneous Earth developed a dense core and a light crust is called differentiation Ch01-intro-nat-dis GLY3034: WEEK 1 18. The Earth's core is made up primarily of iron 19. The inner core is solid because pressures are high in the inner core 10 16. The heat that caused melting in Earth's early history was supplied from a large impact event and radioactivity Ch01-intro-nat-dis GLY3034: WEEK 1 11 17. List of events in chronological order, from oldest to youngest, in the evolution of the Earth: Nebula evolves to Sun and planetisimals, giant impact(s) occurs, molten Earth cools, Earth differentiates (p. 9). 24. Solar energy powers the Earth's external heat engine (p. 10). Ch01-intro-nat-dis 25. Radioactivity powers the Earth's internal heat engine (p. 10). GLY3034: WEEK 1 12 Main Layers of the Earth: Differentiation Core: 6370 – 2900km: Iron and Nickel Inner Core: Solid (6370 to 5150 km) Outer Core: Liquid (5150 – 2900 km) Mantle: Iron, Magnesium, Silicon, Oxygen Lower Mantle: 2900 to 250 km Asthenosphere: 100 – 250 km Upper Mantle: 250 to ~40 km Crust: 40 – 0 km: Silicon, Oxygen, Aluminum Continetal(35-40 Km), Oceanic(5 km) Ch01-intro-nat-dis GLY3034: WEEK 1 13 21. Ninety percent of the Earth is made up of four elements: iron, oxygen, silicon, and magnesium (p. 10) 22. Fifty percent of the Earth's crust is made up of oxygen (p. 10) Ch01-intro-nat-dis GLY3034: WEEK 1 14 Plate Tectonics: A Unifying Theory for Geologic Science 47. Alfred Wegener developed the theory of plate tectonics (p. 20) Ch01-intro-nat-dis A theory is a hypothesis that has withstood many scientific tests GLY3034: WEEK 1 15 Plate Tectonics: A Unifying Theory for Geologic Science 37. The theory of plate tectonics is widely accepted because it explains many of the Earth's major geological features (p. 14) Ch01-intro-nat-dis GLY3034: WEEK 1 16 Plate Tectonics: A Unifying Theory for Geologic Science 34. Earth's lithosphere is approximately 100–200 km thick (p. 14). Ch01-intro-nat-dis 35. The asthenosphere is hot and weak (p. 14) GLY3034: WEEK 1 17 38. Convection is the motion of a flowing material where hot matter rises from the bottom and cool matter sinks (p. 15). Ch01-intro-nat-dis GLY3034: WEEK 1 18 The Scientific Method: Collection of data By observation, by experimentation Formulation of Hypothesis (working model) Testing and modification of hypothesis Theory (or Principle or Law) A hypothesis that has withstood many scientific tests i.e, it has survived repeated challenges and is supported by a substantial body of data Ch01-intro-nat-dis GLY3034: WEEK 1 19 Methods and approach used in the study of geology and geological phenomena. Scientist use the scientific method, rely on theories that have withstood many trials, and follow the principle of uniformitarianism to study natural disasters Ch01-intro-nat-dis GLY3034: WEEK 1 20 Much of the present understanding of geology is based on the Principle of Uniformitarianism (or “Present is the key to the Past): Geological processes that we see in work today have worked much the same way over geological time. Ch01-intro-nat-dis GLY3034: WEEK 1 21 Inferences made from observations Ch01-intro-nat-dis GLY3034: WEEK 1 22 According to the principle of uniformitarianism geological processes we observe today have operated in the past Ch01-intro-nat-dis GLY3034: WEEK 1 23 Composition of the Earth 2/3 of the Earth is made of only Iron and Oxygen Only four elements made 90% of the Earth’s composition ¾ of the Earth is made Oxygen and Silicon Ch01-intro-nat-dis GLY3034: WEEK 1 24 Ch01-intro-nat-dis GLY3034: WEEK 1 25 Big Bang (12 – 13.5 billion years ago) •The Universe started with a cosmic explosion. •Before the Big Bang all matter were condensed in an single, infinitely dense point. •All matters in the Universe is expanding away from the center of explosion ever since Ch01-intro-nat-dis GLY3034: WEEK 1 26 Formation of Solar System: Proto Solar Nebula: Flattened disk of condensed matter Intense pressure and collisions heated the proto Sun to millions of degrees which started nuclear fusion Formation of the solar system (4.6 – 4.5 Ga) Planetesimals: kilometer sized chunks of aggregated matter Inner and Outer Planets Planets closer to the sun (Mercury, Venus, Earth and Mars) lost most of the volatiles becuause of intense heat from the Sun. These are the Inner Planets The volatiles condensed in planets farther out (Jupiter,Saturn, Neptune) Ch01-intro-nat-dis GLY3034: WEEK 1 27 Clear distinction between lithosphere and asthenosphere including physical and chemical properties. Lithosphere – Crust and upper mantle; strong solid. Asthenosphere – mantle; weak solid; more dense than the lithosphere. Ch01-intro-nat-dis GLY3034: WEEK 1 28 Ch01-intro-nat-dis GLY3034: WEEK 1 29 History of Life on Earth 1.8 by: oxygen breathing multicelled animal 600 Ma: Marine animals with hard parts 500 Ma: Fish with backbones 400 Ma: Early Land Plants 300 Ma: Insects 200 Ma: Dinosaurs, First Mammals Living organisms have been on Earth for about 80% of Earth’s history 0.5 Ma: Homo Sapiens Humans have been on Earth for less than 1% of Earth’s history GLY3034: WEEK 1 Ch01-intro-nat-dis 30 Explain the origin of the Earth The Earth formed from planetesimals that crashed into each other and stuck together. These planetesimals were pieces of debris from the Big Bang. As more planetesimals came together the gravitational pull became stronger, pulling in more meteors at faster speeds. Finally, the impacts were so strong that the kinetic energy from the falling meteors turned into heat and the Earth started to melt. The melting allowed the elements that made up the Earth to combine and a process differentiation took place to give origin to the layers of Earth that we see today. Ch01-intro-nat-dis GLY3034: WEEK 1 31