ASTR 2310: Chapter 2 Emergence of Modern Astronomy Early Greek Astronomy Ptolemaic Astronomy Copernican Astronomy Galileo: The First Modern Scientist Kepler's.

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Presentation transcript:

ASTR 2310: Chapter 2 Emergence of Modern Astronomy Early Greek Astronomy Ptolemaic Astronomy Copernican Astronomy Galileo: The First Modern Scientist Kepler's Laws of Planetary Motion Proof of the Earth's Motion

ASTR 2310: Chapter 2 Early Greek Astronomy Smart, but limited experimentation Limited tools (e.g. no telescopes)‏ Our knowledge is fragmentary Still, lots of stuff right, from thousands of years ago E.g., lunar phases and eclipses understood, and more as well

ASTR 2310: Chapter 2 Aristotle's Explanations for Spherical Earth Gravity pulls everything together, strongly, and a sphere is the most compact form Partial lunar eclipses always show an arc of a circle and only spheres ALWAYS show such shadows from any angle Different stars visible as you move south, suggesting a curved Earth. African and Indian elephants similar and on “opposite sides of the world” so they must be close to each other...well, not quite!

ASTR 2310: Chapter 2 Aristarchus: Relative Distances to Sun and Moon Wikipedia:

ASTR 2310: Chapter 2 Aristarchus: Relative Distances to Sun and Moon A/C=cosine theta. Theta=87degrees means C=19A If theta = degrees (modern value) then C=390A

ASTR 2310: Chapter 2 Aristarchus: Relative Sizes of Moon, Earth, Sun Geometry involving eclipses Wiki: nces#Lunar_eclipsehttp://en.wikipedia.org/wiki/Aristarchus_On_the_Sizes_and_Dista nces#Lunar_eclipse Came up with 1:3:19 (modern values 1:4:390) for ratios of diameters.

ASTR 2310: Chapter 2 Eratosthenes: Size of the Earth Geometry involving the sun Wiki: Figured out what fraction (1/50) of the Earth's circumference corresponded to the distance between Alexandria and Syene Figure from Wired Magazine Theta is about 7 degrees Answer is the circumference is 46,000 km Modern value closer to 40,000 km

ASTR 2310: Chapter 2 Hipparchus: Extraordinary Observer Star Catalog (leading to detection of precession of the equinoxes)‏ Magnitude system (ASTR 2320 horror show!)‏ Accurate distance to the Moon (not too far off the modern value of 60.5 Earth radii)‏ Length of tropical year (good to 7 minutes)‏

ASTR 2310: Chapter 2 Emergence of Modern Astronomy Early Greek Astronomy Ptolemaic Astronomy Copernican Astronomy Galileo: The First Modern Scientist Kepler's Laws of Planetary Motion Proof of the Earth's Motion

ASTR 2310: Chapter 2 Ptolemaic Astronomy Ptolemy developed detailed mathematical model to predict positions of objects in the sky Used for 14 centuries Accurate but conceptually flawed

ASTR 2310: Chapter 2 Ptolemaic Astronomy Observed elements: Stars, with fixed relative positions, rotate around celestial pole Sun moves east along ecliptic, tilted at 23.5 degrees, about 1 degree per day Moon moves east also, not quite on ecliptic, about 13 degrees per day Planets usually move eastward (prograde), but sometimes west (retrograde). And only some planets.

ASTR 2310: Chapter 2 Ptolemaic Astronomy Earth doesn't move (no sense of motion, parallax)‏ Not quite at center Everything “circles” Lots of weird terms Predicts positions ok!

ASTR 2310: Chapter 2 Ptolemaic Astronomy Not all planets equal! Placements look odd Tested by Galileo

ASTR 2310: Chapter 2 Copernican Astronomy Sun at center -- heliocentric Still circles Simpler Not more predictive

ASTR 2310: Chapter 2 Copernican Astronomy Explanation for retrograde motion

ASTR 2310: Chapter 2 Copernican Astronomy Inferior Planets (no retrograde motion, always close to the sun), orbits smaller than Earth's Venus, Mercury Superior Planets (Mars, Jupiter, Saturn known by Greeks)‏ Retrograde motion, orbits larger than Earth's

ASTR 2310: Chapter 2 Copernican Astronomy More Terminology – draw Figure on board Opposition Conjunction Quadratures Elongation (angle between planet and sun)‏ Synodic period (e.g., time between conjunctions)‏ Sidereal period (period relative to background stars)‏

ASTR 2310: Chapter 2 Copernican Astronomy – Inferior Planets Orbital Periods and Relative Planetary Distances Angular Velocities (  )‏ Inferior Planets:  P =   +  syn (  P >   )‏ Inferior Planets: 1/P P = 1/P E + 1/P syn Period of Venus: (1/ days + 1/ days) - 1 So we get the orbital period of days

ASTR 2310: Chapter 2 Copernican Astronomy – Superior Planets Orbital Periods and Relative Planetary Distances Angular Velocities (  )‏ Superior Planets:  P =   -  syn (  P <   )‏ Superior Planets: 1/P P = 1/P E - 1/P syn Period of Mars: (1/ days - 1/ days) -1 So we get the orbital period of days

ASTR 2310: Chapter 2 Copernican Astronomy – Planetary Distances Relative to Earth-Sun Distance (Astronomical Unit)‏ See nice webpage at:

ASTR 2310: Chapter 2 Copernican Astronomy Inferior Planet Orbital Distances (assume circular)‏ D = 1 Astronomical Unit (1 AU): So d = cos  in AU

ASTR 2310: Chapter 2 Copernican Astronomy Superior Planet Orbital Distances Time t from position 1 to 2 Angle  = t (360/P E )‏ Angle  = t (360/P P )‏ So d = 1/(cos(  ))‏ Again in AU