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| d traveled by lt in one yr |
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| d at wh an obj of size 1AU would have an angular sz of 1" (one arcsecond) |
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| triangulation in astronomy |
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| greater th 100 parsecs (p is too small) |
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| det poles and =tor of cel sphere by... |
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| extending axis of rot and =torial plane of E |
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| suggested expln for a phen |
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| testable expln for th ebehavior of nat phen |
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| theoretical construct t reps algo. has vars, w a set of ships bw them |
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| rule for how nature will behave under certain conds |
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| pts at wh ecliptic cross cel equator |
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| (2)E’s axis of rot is tilted... |
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| at angle of 23.5˚ f perpendicular to plane of E’s orbit. this causes seasons |
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| Nernmost/Sernmost pts on suns path on cel sphere |
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| slow change in orientation of E's axis of rot. caused by gravitational pull of sun. causes pole and equinoz pos.s to shift rel to stars |
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| time f sunrise to sunset... |
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| ch.es thruout yr due to seasonal ch |
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| time it takes sun to move f highest pt on sky on one day to highest pt on second day |
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| time it takes E to complete one rot ab axis (m.ed w respect to stars) |
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| 1deg/day in its orbit runt the sun |
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| first sci to speak directly to ppl. invented astro telescope (saw moons, craters). studied moon exenively. |
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| studied movement of planets math.ly. Had idea of elliptical orbits. |
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| (2)Law of Planetary Motion #1 |
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| orbits of planets are ellipses w sun at one focus. Eccentricity e=c/a. (c=d f focus to center, a=semi-ajor axis) |
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| pt at wh E is closest to sun. E moves fastest at this time |
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| Law of Planetary Motion #2 |
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| line f planet to sun sweeps over equal areas in equal time intervals |
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| (2)Law of Planetary Motion #3 |
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| sq.s of orbital periods of planets ab sun are proportional to cubes of orbital semi-major axes. P^2=a^3 (P=orbital pd in yrs). |
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=k a^3 in any units.
=4Π² a³
GMo |
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| every body continues in a state of rest or uniform motion in a straight line unless compelled to ch that state by a force acting on it |
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| For every action hay an opp and equal reaction |
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| as much force on sun as sun is putting on E. But sun is much more massive, so its force is felt much greater. Hence the E revolves runt the sun |
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| Elliptical path of motion of E = |
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| suns gravitational pull + E's v in straight line |
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| (2)Laws of U.al Gravitation |
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| two bodies attract eo w force directly p.al to the mass of ea body and inversely p.al to the sq of the d bw them |
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| The moon falls runt E bc... |
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| the moons spd is fast enuf that its curvature of falling path is slightly flatter th t of E |
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| v an obj must have para to stay in circular orbit. Vc=sqrt(Gm/r) |
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| If planets v is less th circular v... |
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| (2)If planets v is more th circular v... |
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| planet will stay in elliptical orbit or escape f orbit |
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