AST101H1 Lecture Notes - Lecture 11: Pearson Education, Photon, Hydrogen Atom

• School: UTSG
• Department: Astronomy & Astrophysics
• Course: AST101H1
• Professor: Bryan Gaensler

Document Summary

Emission vs scattering: scattered light = red t-shirt; a solid object glowing as a blackbody, light scatters off shirt. Atomic energy levels: ele(cid:272)tro(cid:374)s li(cid:448)e i(cid:374) defi(cid:374)ed (cid:862)or(cid:271)itals(cid:863) arou(cid:374)d (cid:374)u(cid:272)leus, each orbital has different energy, closer-in orbitals = lower energy, each orbital has different energy, further out the more energy needed. Absorption lines: electron can change to a higher energy orbital by absorbing a photon of light corresponding exactly to the energy change. Figure 3 (gaensler: (cid:862)a(cid:271)sorptio(cid:374) li(cid:374)e(cid:863) (light missing at one specific color dip in continuum) Energy levels of hydrogen: simplest case: hydrogen atom, 1 protons, 0 neutrons, 1 electron, specific series of absorption lines. Clicker q&a: an absorption line is produced in a spe(cid:272)tru(cid:373) (cid:449)he(cid:374) : an electron absorbs a photon. Figure 4 (gaensler: every atom has a unique set of energy levels which means that each as a unique spectral fingerprint. Absorption: not just in the sun: earth"s at(cid:373)osphere (cid:271)lo(cid:272)ks out spe(cid:272)ifi(cid:272) (cid:272)olors fro(cid:373) su(cid:374)light (cid:894)espe(cid:272)ially i(cid:374) ultra(cid:448)iolet(cid:895)