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Week 1 and 2 notes

by: Ariel Kamen

Week 1 and 2 notes Astr 161

Marketplace > Towson University > Astr 161 > Week 1 and 2 notes
Ariel Kamen
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About this Document

These are the notes that we went over in class.
General Astronomy 1
Dr. Krause
Class Notes




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This 6 page Class Notes was uploaded by Ariel Kamen on Sunday September 11, 2016. The Class Notes belongs to Astr 161 at Towson University taught by Dr. Krause in Fall 2016. Since its upload, it has received 50 views.


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Date Created: 09/11/16
8/29/16      General Astronomy: Chapter 2 Patterns in the Sky Motions of the Earth: •   Earth rotates on its axis  —> general motions in the sky  —> corialis effect (effects weather) • Earth rotates about the sun —> seasons  —> precession  * when Earth rotates around the sun the tilts stays the same * Earth rotates towards East Tropics and Circles *  seasons are caused by the tilt of  the Earth LAB PHOTOS 8/31/16   1.   Precession (conclusion) 2.   Ancients and retrograde motion 3.   Copermicus 4.   Galileo Ptolemy (85 ­ 165 AD) Copernicus (1473 ­ 1543) Galileo (1571 ­ 1630) Galileo’s Observations with the Telescope ­mountains on the moon milky way ­ ­sunspots moons of Jupiter ­ ­phases of Venus  9/1/16    Chpt 3 Galileo (1564 ­ 1642) Kepler ­ phenomenological approach                           Newton ­ final principles approach Brahe (1546 ­ 1601) Kepler (1571 ­ 1630) Newton (1642 ­ 1727) Kepler’s 3 Laws of Motion Copernicus (1473 ­ 1543) 1.   Planetary orbits are ellipses with the sun at one focus b = semi ­ minor axis  cl = semi ­ major axis foci E = eccentricity O < E < 1  2. A line from the sun to planet sweeps out equal areas in equal times 3. P^2 = a^3  (years)   (au)        Newton’s 3 Laws of Motion 1.   Law of inertia (Galileo)   ­  when an object feels no net force its motion remains constant or at rest 2. When an object feels a net force, the object accelerates in the same direction as the net  force, and proportional to it  —> = —> F NBT  Ma ­Acceleration of gravity at Earth’s surface        g = (9.8 m/s)/s = 9.8 m/s^2 3. Action — reaction law   ­ 2 objects interacting 


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