NATS 1880 Chapter Notes - Chapter 9: Giant Planet, Galilean Moons, Christiaan Huygens

• School: York University
• Department: Natural Science
• Course: NATS 1880
• Professor: Paul Delaney

Document Summary

Jupite(cid:396)"s (cid:373)oo(cid:374) ga(cid:374)(cid:455)(cid:373)ede a(cid:374)d atu(cid:396)(cid:374)"s tita(cid:374) a(cid:396)e la(cid:396)ge(cid:396) tha(cid:374) me(cid:396)(cid:272)u(cid:396)(cid:455: the other three galilean moons and neptu(cid:374)e"s t(cid:396)ito(cid:374) a(cid:396)e (cid:271)igge(cid:396) tha(cid:374) pluto, the gravity of the jovian planets drew gas and dust from the surrounding solar nebula. This gas and dust forms a disc around each jovian planet. This (cid:272)ould"(cid:448)e happe(cid:374)ed (cid:449)he(cid:374) the jo(cid:448)ia(cid:374) pla(cid:374)ets (cid:449)e(cid:396)e (cid:455)ou(cid:374)g (cid:449)ith la(cid:396)ge(cid:396) e(cid:454)te(cid:374)ded atmospheres, easily allowing passing by objects to be captured: neptu(cid:374)e"s (cid:373)oon triton is believed to have been a planet. Ea(cid:396)th"s: like our moon, the jovian moons also keep their same face turned toward the planet, known as synchronous rotation. This happens by rotating once while completing one orbit: tidal friction: stretching the earth from the moon, increasing distance of moon from earth by. Jovian moons can have an internal heating different from that on the terrestrial worlds: the moons have an additional heating source known as tidal heating which arises from effects of tidal forces.