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| In astronomy, the only way to inv objs (stars, galaxies, etc) is to... |
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| analyze the lt and other radn t come f them |
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| (6)By studying a star's radn we can learn ab its: |
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| energy output, surface temp, radius, chem composition, v, rot pd |
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| time it takes suns lt to reach E |
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| 3e8 m/s (too fast to be m.ed by human reactions) |
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| energy, waves, electromagnetic radn |
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| d bw repeating parts of a wave. ,\=c/v |
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| um (10^-6 m), nm (10^-9m), ao (10^-10m) |
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| infrared (IR) region has w |
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| ultraviolet (UV) region has w |
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| all colors of the rainbow |
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| anything t spreads out in waves |
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| as wave and carries energy |
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| star shifts toward longer w's (moves away f you) |
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| star shifts toward shorter w's (moves toward you) |
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Δλ= ch in w due to Doppler Effect
λ0= actual w emitted by source
vr= radial v |
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| doppler effect allows us to |
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| most common reason for emission of lt |
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| a m of how fast atoms are moving |
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| lowest temp there can poss be = 0K = -273C = -460F |
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| We see phases of the moon bc... |
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| its orbit runt E makes us see diff amts of it |
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| (3)Moon is tidally locked |
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| rot.ing w same pd ar axis as it is rot.ing ar E. T, we always see same sd of moon facing E. But moons dir towards sun changes |
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| time it takes moon to complete one full orbit runt E = 27.32 days |
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| time bw successive new moons = 29.53 days |
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| is tilted 5.2deg f the ecliptic plane |
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| moon is in Es shadow. E is directly bw moon and sun |
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| all of moon can see part of sun |
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| part of moon can see all of sun |
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| all of moon cant see sun. can last up to 1hr 40min. moon has reddish glow. total surface of moon enters E's umbra |
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| E is in moons shadow. moon is directly bw E and sun. sun appears as lg in sky as moon |
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| observer can see any of sun |
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| observer can see part of sun bc he/she is standing in moons penumbra |
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| moons umbra doesnt reach E. observer can see sliver or closed circle of sun |
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| forces f the moon arent strong enuf to deform E, but do deform water |
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| slowing due to friction f tides caused by E (i think) |
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| rot pd of moon = rev pd of moon = one month. E will also have one in 10bil yrs |
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| slows dn by 2 m/century. due to dissipation of Es energy caused by friction of oceans movement. T, length of day is increasing |
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| moon moves away to conserve angular momentum. Moons orbital pd increases. Moon gets smaller. Eventually there will be no more eclipses or tides |
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