1. How to Make Starlight (part 1) Chapter 7

2. Origin of light Light (electromagnetic radiation) is just a changing electric and magnetic field. Changing electric field (e.g., due to acceleration of an electron) generates electromagnetic radiation. We discuss two major mechanisms: Blackbody Radiation Spectral Line Emission

3. Heat and Temperature Temperature refers to the degree of agitation, or the speed with which the particles move (T~v 2 ). All atoms are vibrating unless at absolute zero temperature (T = 0 K = -459.7 F). Water freezes at 273 K and boils at 373 K. Heat refers to the amount of energy stored in a body as agitation among its particles and depends on density as well as temperature.

4. Blackbody Spectrum It is the spectrum that a "perfect emitter" or a "perfect absorber" (roughly a very thick or solid object) would radiate. A black object is the closest approximation to a perfect absorber.

6. The Difference Between Black and White “White” light – contains all the frequencies of the visible part of the spectrum. “White” light – contains all the frequencies of the visible part of the spectrum. White paint – diffusely scatters all frequencies of the visible part of the spectrum equally. White paint – diffusely scatters all frequencies of the visible part of the spectrum equally. Black paint – absorbs all frequencies of the visible part of the spectrum equally. Black paint – absorbs all frequencies of the visible part of the spectrum equally. “Blackbody” – emits and absorbs radiation over a specific set of frequencies. “Blackbody” – emits and absorbs radiation over a specific set of frequencies.

7. Discussion Question Why does NASA paint spacecraft white? Absorption Frequency Infrared Visible Absorption Spectrum of White Paint 40% 0% Absorption Spectrum of Black Paint 80%

8. Hotter objects emit photons with a higher average energy. Wien’s Law Wien’s Law The peak of the blackbody emission spectrum is given byThe peak of the blackbody emission spectrum is given by

10. Blackbody Radiation

11. The graph below shows the blackbody spectra of three different stars. Which of the stars is at the highest temperature? 1) Star A 2) Star B 3) Star C A B C Energy per Second Wavelength

12. Hotter objects emit more total radiation per unit surface area. Cold Hot Stefan-Boltzmann Law: Emitted power per square meter = σ T 4 σ = 5.7 x 10 -8 W/(m 2 K 4 )

13. You are gradually heating up a rock in an oven to an extremely high temperature. As it heats up, the rock emits nearly perfect theoretical blackbody radiation – meaning that it 1) is brightest when hottest. 2) is bluer when hotter. 3) is both 4) is neither

14. L=A  T 4

15. Campfires Campfires are blue on the bottom, orange in the middle, and red on top. Which parts of the fire are the hottest? the coolest? As atoms get hotter, they wiggle faster and collide to each other harder ---> more light they emit and more wiggle per second = frequency goes up = wavelength goes down. Thus bluer. Thus, as temperature goes up light gets stronger and gets blue.

16. Blackbody Radiation (a.k.a. Thermal Radiation) Every object with a temperature greater than absolute zero emits blackbody radiation.Every object with a temperature greater than absolute zero emits blackbody radiation. Hotter objects emit more total radiation per unit surface area.Hotter objects emit more total radiation per unit surface area. Hotter objects emit photons with a higher average energy.Hotter objects emit photons with a higher average energy.

17. How to Make Light (Part 2) Structure of atoms Structure of atoms Energy levels and transitions Energy levels and transitions Emission and absorption lines Emission and absorption lines Light scattering Light scattering

18. Atoms A Planetary Model of the Atom Atoms are made of electrons, protons, and neutrons. The bounding force: the attractive Coulomb (electrical) force between the positively charged nucleus and the negatively charged electrons.

19. Electrons can be in different orbits of certain energies, called energy levels. Different atoms have different energy levels, set by quantum physics. Quantum means discrete! Energy Levels

20.  To change its energy levels, an electron must either absorb or emit a photon that has the same amount of energy as the difference between the energy levels  E = h --- Larger energy difference means higher frequency.  Different jumps in energy levels means different frequencies of light absorbed. Excitation of Atoms

21. Spectral Line Emission If a photon of exactly the right energy is absorbed by an electron in an atom, the electron will gain the energy of the photon and jump to an outer, higher energy orbit. A photon of the same energy is emitted when the electron falls back down to its original orbit.

23. Spectral Line Emission Collisions (like in a hot gas) can also provide electrons with enough energy to change energy levels. A photon of the same energy is emitted when the electron falls back down to its original orbit.

24. Energy Levels of a Hydrogen Atom Different allowed “orbits” or energy levels in a hydrogen atom. Emission line spectrum Absorption line spectrum

26. Spectral Lines of Some Elements Argon Helium Mercury Sodium Neon Spectral lines are like a cosmic barcode system for elements.

27. Atoms of different elements have unique spectral lines because each element has atoms of a unique color has atoms of a unique color has a unique set of neutrons has a unique set of neutrons has a unique set of electron orbits has a unique set of electron orbits has unique photons has unique photons

29. The Solar Spectrum There are similar absorption lines in the other regions of the electromagnetic spectrum. Each line exactly corresponds to chemical elements in the stars.

31. Sources of spectral lines Reflection nebula Emission nebula

32. An Object’s Spectrum Encoded in an object’s spectrum is information about the emitter/absorber. This is how we learn what the Universe is made of!

33. Intensity (spatial distribution of the light) Spectra (composition of the object and the object’s velocity) There are three basic aspects of the light from an object that we can study from the Earth. Variability (change with time)