lecture_tan18 - Admin. 2/22/11 1. 2. 3. 4. 5. 6. 7. 8....

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Admin. 2/22/11 1. Class website http://www. astro . ufl .edu/~jt/teaching/ast1002/index.html 2. Discussion sections: Tuesday 1.55pm (period 7), Bryant 3 Wednesday 10.40am (period 4), Bryant 3 Thursday 3.00pm (period 8), Bryant 3 Office hr: Thursday (5pm), Bryant 302 3. Homework 5 due Sunday Feb. 27th by 11pm. 4. Reading this week : Chapters 0, 1, 2.1-2.4, 4-8, rest of 2, 9, 10 5. Email me Astro - news, jokes, tunes, images: ast1002_tan@astro. ufl . edu 6. Print out class notes and bring them to class - use these as a base outline to take extra notes in class. 7. Midterm 2: Thur. 17th March, in class. 8. Observing Project - Fridays 8.30pm - see class website. Key Concepts: Lecture 18: Solar System Formation, Light Formation of the Solar System: the Nebular Hypothesis Light: wave-like behavior Light: particle-like behavior Light: Interaction with matter - Kirchoff’s Laws Origin of Solar System • Observations of the different members of the solar system place constraints on theories of its formation – motions – chemical composition – age Origin of Solar System Planets orbit the Sun in same direction (counter-clockwise if viewed from above the Earth’s north pole) and in nearly the same plane. Most planets and the Sun also rotate in roughly this same direction, although planets can be tilted, occasionally by large angles. Most moons orbit around their parent planet in this same direction Solar system is differentiated – Terrestrial planets: high densities, small to moderate atmospheres, slow rotation, 0 to few moons – Jovians: low densities, thick atmospheres, fast rotation, many moons Asteroids are very old – primitive unevolved material - common age of oldest solar system material: 4.6 billion years. Comets are also very old: primitive icy fragments from Oort Cloud or Kuiper Belt
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Origin of the Solar System: Nebular Hypothesis Slowly rotating interstellar cloud Gravitational contraction – disk flattens conservation of angular momentum Sun forms at center of nebula Conservation of Momentum Momentum = mass x velocity Review Newton’s Laws of Motion (Lecture 9). Newton’s 1st Law implies momentum is conserved (i.e. is unchanging) if there are no forces acting on an object. overall momentum is also conserved (i.e. unchanged) since there is always an opposite force of equal strength. Conservation of Angular Momentum
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This note was uploaded on 09/07/2011 for the course AST 1002 taught by Professor Dr.haywoodsmith,jr during the Spring '07 term at University of Florida.

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lecture_tan18 - Admin. 2/22/11 1. 2. 3. 4. 5. 6. 7. 8....

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