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| the study of the Universe in which humans live |
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| smallest measurable unit of time |
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| How many constellations today? |
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| 88; 40 new, 48 are from classical age by Babylonians, Egyptians, Mesopotamians, and Greeks. |
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| what used to define a group of stars, now defines a section/area of sky with clear boundaries |
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| Groupings of stars, smaller than a constellation. For example: The Big Dipper is an asterism of the constellation Ursa Major. |
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| Daily motion of the sun, moon, planets and stars |
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| means "around the pole"; stars that circle the pole and never set |
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| radius: 23.5deg; due to the fact that the earth is not a perfect sphere. It's top-like motion. Moves reference marks such as celestial poles. |
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| first appeared in writings of Ptolemy; 1st mag. to 6th mag. 1 mag= 2.5 factor in brightness. |
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| inversely related to the square of its distance. If a star is twice as distance, 2^2 is 4...1/4 the luminosity of the first star. |
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| Astronomical Unit; average distance between the earth and sun. (1.5 x 10^11 km |
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| first to calculate circum. of earth |
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| Measured relative sizes of earth/moon/sun; was far off, but established that the sun was far away and larger than earth |
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| geocentric model; traced out the ecliptic |
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| anytime the sun crosses the celestial equator, even amount of sunlight per day. |
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| March 21st, our calendar's zero |
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| Point where the sun is furthest north or south |
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| furthest from the sun (July 6th) |
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| closest to the sun (Jan 3rd) |
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| An effect of the tilt of the earth's axis |
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| it causes sunlight to be more/less direct, which causes our seasons! |
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| orbital period of the moon relative to the stars. 27.3 days |
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| orbital period relative to the sun; time between successive new moons, 29.5 days (has to catch up to the sun, who has moved a degree a day across the sky. |
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| defined to be 24 hours. rotates 361 degrees to meet back to the sun after moving across its revolution. |
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| relative to the stars, 23 hr. 56min. |
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| only occurs when the line of nodes points toward the sun. |
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| Tilt between earth and lunar orbital plane: |
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| Amount of eclipses in a year |
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| min. 2 and max. 7 in one year |
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| observer sees partial covering of the sun; surrounds the umbra |
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| observer sees the sun completely covered, darkest portion of shadow |
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| beyond the apex of the umbra, observer sees partial covering of the sun because the object covering is not large enough; only solar eclipses |
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| occurs when the earth casts its shadow onto the moon; seen by everyone who can see the moon; separated by six months |
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| Length of Totality during Total Solar Eclipse |
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| no more than about 7 minutes |
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| Length of partial coverage from a Solar Eclipse |
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| gas being projected off and back down to the Sun and above the Chromosphere |
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| The ring of white light emission during total solar eclipse |
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| caused by mountains and valleys on Moon's surface; little rim of sun shining through on the edges |
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| a partial eclipse where it can only be seen through the antiumbra, where there is an annulus, or ring. |
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| an eclipse cycle that has a period of about 18 years, 11 days, and 8 hours. |
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| geocentric, used epicycles, was used for 1400 years, very accurate |
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| heliocentric, still used perfect circular motion, not as accurate as Ptolemy's model |
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| circle about which an epicycle travels |
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| point about which the epicycle seems to make uniform circular motion about the deferent |
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| circle about which planet travels, used to explain motions like retrograde motion |
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| Copernican's writing over heliocentricity |
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