CHEM 110 Lecture Notes - Lecture 3: Red Supergiant Star, Substitute Good, Star Formation
Document Summary
At time 380,000 years, the temperature was 3000 k. this was the first time we saw neutral atoms in the universe. Atoms form from nuclei and electrons, releasing the cosmic microwave background radiation. At time 300 million years, the first stars and galaxies form. Star formation begins with the slow accumulation of gas. Gravitational attra(cid:272)tio(cid:374) of (cid:862)(cid:272)lu(cid:373)ps(cid:863) attra(cid:272)ts (cid:373)ore (cid:373)aterial together. Co(cid:374)tra(cid:272)tio(cid:374) causes the temperature and pressure to slowly increase. Energy comes fro(cid:373) (cid:374)u(cid:272)lear fusio(cid:374), sho(cid:449)(cid:374) i(cid:374) ei(cid:374)stei(cid:374)"s for(cid:373)ula, e-mc^2. An average star"s life (cid:272)(cid:455)(cid:272)le goes fro(cid:373) a stellar (cid:374)e(cid:271)ula to a(cid:374) a(cid:448)erage star, to a red gia(cid:374)t, to a pla(cid:374)etar(cid:455) (cid:374)e(cid:271)ula, to a (cid:449)hite d(cid:449)arf. The inside of average stars can form up to about iron (fe). The rest of the elements depend on massive stars. A (cid:373)assi(cid:448)e star"s life (cid:272)(cid:455)(cid:272)le goes fro(cid:373) stellar (cid:374)e(cid:271)ula to a (cid:373)assi(cid:448)e star, to a red supergiant, to a supernova, then either to a neutron star or to a black hole.
