ASTR-1010 Lecture Notes - Lecture 21: Earth Mass, Celestial Pole, Full Moon

• School: Vanderbilt University
• Department: Astronomy
• Course: ASTR-1010
• Professor: Stassun Keivan

Document Summary

Why do we see the phases of the moon: moon orbits around the earth, moon is (almost!) always illuminated by the sun, earth sees some combination of light and dark parts. Phases of the moon: over 29. 5 days. What causes the eclipses: earth and moon cast shadows. Lu(cid:374)ar e(cid:272)lipse: moo(cid:374) i(cid:374) earth"s shado(cid:449) (cid:894)earth (cid:271)et(cid:449)ee(cid:374) (cid:373)oo(cid:374) a(cid:374)d su(cid:374) moon passes through our shadows and is dark/ red due to atmospheric scattering: solar e(cid:272)lipse: earth i(cid:374) moo(cid:374)"s shado(cid:449) Lunar eclipses: different flavors: penumbral: gets darker, total lunar eclipse: gets reddest and darkest during the full eclipse. Solar eclipse: moon is between the sun and the earth: moo(cid:374)"s shado(cid:449) is (cid:271)lo(cid:272)ki(cid:374)g the (cid:448)isi(cid:271)ility of the su(cid:374) Looking at some other planet and how it blocks our shadow: ~5 earth mass, orbits ~1 day, ~0. 05% dimming. Ancient greeks perspective: planets lined up linearly: earth, moon, mercury, venus, sun, mars, jupiter, saturn.