Light and Atoms

Transcription

1 Light and Atoms ASTR S1 Daniel Zucker E7A 317 ASTR170 Introductory Astronomy: II. Light and Atoms 1

2 Overview We ve looked at telescopes, spectrographs and spectra now let s find out how they can tell us what we want to know: What is an atom? How do atoms interact with light? What kinds of spectra do you see when you look at objects in the sky? What can you learn from a star s spectrum? ASTR170 Introductory Astronomy: II. Light and Atoms 2

3 The Power of Starlight Just by analyzing the light received from a star, astronomers can retrieve information about a star s 1. Total energy output 2. Surface temperature 3. Radius 4. Chemical composition 5. Velocity relative to Earth 6. Rotation period ASTR170 Introductory Astronomy: II. Light and Atoms 3

4 Radiation: Information from Space In astronomy, we cannot perform experiments with our objects (stars, galaxies, ). The only way to investigate them is by analyzing the light ( = radiation) which we observe from them. ASTR170 Introductory Astronomy: II. Light and Atoms 4

5 Light as a Wave (1) λ c = 300,000 km/s = 3*10 8 m/s Light waves are characterized by a wavelength λ and a frequency f. f and λ are related through f = c/λ ASTR170 Introductory Astronomy: II. Light and Atoms 5

6 Light as a Wave (2) Wavelengths of light are measured in units of nanometers (nm) or Ångströms (Å): 1 nm = 10-9 m 1 Å = m = 0.1 nm Visible light has wavelengths between 4000 Å and 7000 Å (= nm). ASTR170 Introductory Astronomy: II. Light and Atoms 6

7 Wavelengths and Colours Different colours of visible light correspond to different wavelengths. ASTR170 Introductory Astronomy: II. Light and Atoms 7

8 Light as Particles Light can also appear as particles, called photons (explains, e.g., photoelectric effect). A photon has a specific energy E, proportional to the frequency f: E = h*f h = 6.626x10-34 J*s is the Planck constant. The energy of a photon does not depend on the intensity of the light! ASTR170 Introductory Astronomy: II. Light and Atoms 8

9 The Electromagnetic Spectrum Wavelength Frequency Need satellites to observe High flying air planes or satellites ASTR170 Introductory Astronomy: II. Light and Atoms 9

10 Atomic Structure An atom consists of an atomic nucleus (protons and neutrons) and a cloud of electrons surrounding it. Almost all of the mass is contained in the nucleus, while almost all of the space is occupied by the electron cloud. ASTR170 Introductory Astronomy: II. Light and Atoms 10

11 Nuclear Density If you could fill just a teaspoon with material as dense as the matter in an atomic nucleus, it would weigh ~ 2 billion tonnes ASTR170 Introductory Astronomy: II. Light and Atoms 11

12 Different Kinds of Atoms The kind of atom depends on the number of protons in the nucleus. Most abundant: Hydrogen (H), with one proton (+ 1 electron) Next: Helium (He), with 2 protons (and 2 neutrons + 2 el.) Different numbers of neutrons different isotopes Helium 4 ASTR170 Introductory Astronomy: II. Light and Atoms 12

13 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. r 3, E 3 r 2, E 2 r 1, E 1 These characteristic electron energies are different for each individual element. ASTR170 Introductory Astronomy: II. Light and Atoms 13

14 Atomic Transitions An electron can be kicked into a higher orbit when it absorbs a photon with exactly the right energy. The photon is absorbed, and the electron is in an excited state. All other photons pass by the atom unabsorbed. E ph = E 3 E 1 E ph = E 4 E 1 Wrong energy (Remember that E ph = h*f) ASTR170 Introductory Astronomy: II. Light and Atoms 14

15 Colour and Temperature Stars appear in different colours, from blue (like Rigel) Orion Betelgeuse via green / yellow (like our sun) to red (like Betelgeuse). These colours tell us about the star s temperature. Rigel ASTR170 Introductory Astronomy: II. Light and Atoms 15

16 Black Body Radiation (1) The light from a star is usually concentrated in a rather narrow range of wavelengths. The spectrum of a star s light is approximately a thermal spectrum called a black body spectrum. A perfect black body emitter would not reflect any radiation. Thus the name black body. ASTR170 Introductory Astronomy: II. Light and Atoms 16

17 Two Laws of Black Body Radiation 1. The hotter an object is, the more energy it emits: Energy Flux F = σ*t 4 where F = Energy Flux = = Energy given off in the form of radiation, per unit time and per unit surface area [J/s/m 2 ]; σ = Stefan-Boltzmann constant ASTR170 Introductory Astronomy: II. Light and Atoms 17

18 Two Laws of Black Body Radiation 2. The peak of the black body spectrum shifts towards shorter wavelengths when the temperature increases. Wien s displacement law: λ max 3,000,000 nm / T K (where T K is the temperature in Kelvin) ASTR170 Introductory Astronomy: II. Light and Atoms 18

19 Stellar Spectra The spectra of stars are more complicated than pure blackbody spectra. They contain characteristic lines, called absorption lines. With what we have learned about atomic structure, we can now understand how those lines are formed. ASTR170 Introductory Astronomy: II. Light and Atoms 19

20 Kirchhoff s Laws of Radiation (1) 1. A solid, liquid, or dense gas excited to emit light will radiate at all wavelengths and thus produce a continuous spectrum. ASTR170 Introductory Astronomy: II. Light and Atoms 20

21 Kirchhoff s Laws of Radiation (2) 2. A low-density gas excited to emit light will do so at specific wavelengths and thus produce an emission spectrum. Light excites electrons in atoms to higher energy states Transition back to lower states emits light at specific frequencies ASTR170 Introductory Astronomy: II. Light and Atoms 21

22 Kirchhoff s Laws of Radiation (3) 3. If light comprising a continuous spectrum passes through a cool, low-density gas, the result will be an absorption spectrum. Light excites electrons in atoms to higher energy states Frequencies corresponding to the transition energies are absorbed from the continuous spectrum. ASTR170 Introductory Astronomy: II. Light and Atoms 22

23 The Spectra of Stars The inner, dense layers of a star produce a continuous (blackbody) spectrum. Cooler surface layers absorb light at specific frequencies. => Spectra of stars are absorption spectra. ASTR170 Introductory Astronomy: II. Light and Atoms 23

24 Analyzing Absorption Spectra Each element produces a specific set of absorption (and emission) lines. Comparing the relative strengths of these sets of lines, we can study the composition of gases. By far the most abundant elements in the Universe ASTR170 Introductory Astronomy: II. Light and Atoms 24

25 Lines of Hydrogen Most prominent lines in many astronomical objects: Balmer lines of hydrogen ASTR170 Introductory Astronomy: II. Light and Atoms 25

26 The Balmer Lines n = 1 n = 5 Transitions from 2 nd to higher levels of hydrogen H α H β H γ The only hydrogen lines in the visible wavelength range 2 nd to 3 rd level = H α (Balmer alpha line) 2 nd to 4 th level = H β (Balmer beta line) ASTR170 Introductory Astronomy: II. Light and Atoms 26

27 Observations of the H-Alpha Line Emission nebula, dominated by the red Hα line ASTR170 Introductory Astronomy: II. Light and Atoms 27

28 Absorption Spectrum Dominated by Balmer Lines Modern spectra are usually recorded digitally and represented as plots of intensity vs. wavelength ASTR170 Introductory Astronomy: II. Light and Atoms 28

29 The Balmer Thermometer Balmer line strength is sensitive to temperature: Most hydrogen atoms are ionized => weak Balmer lines Almost all hydrogen atoms in the ground state (electrons in the n = 1 orbit) => few transitions from n = 2 => weak Balmer lines ASTR170 Introductory Astronomy: II. Light and Atoms 29

30 Measuring the Temperatures of Stars Comparing line strengths, we can measure a star s surface temperature! ASTR170 Introductory Astronomy: II. Light and Atoms 30

31 Spectral Classification of Stars (1) Different types of stars show different characteristic sets of absorption lines. Temperature ASTR170 Introductory Astronomy: II. Light and Atoms 31

32 Spectral Classification of Stars (2) Mnemonics to remember the spectral sequence: Oh Oh Only Be Boy, Bad A An Astronomers Fine F Forget Girl/Guy Grade Generally Kiss Kills Known Me Me Mnemonics ASTR170 Introductory Astronomy: II. Light and Atoms 32

33 Stellar Spectra O B A F G K M Surface temperature ASTR170 Introductory Astronomy: II. Light and Atoms 33

34 The Composition of Stars From the relative strength of absorption lines (carefully accounting for their temperature dependence), one can infer the composition of stars. ASTR170 Introductory Astronomy: II. Light and Atoms 34

35 Class Announcements Assignment #1 given out today (Wednesday, 3 March), due Friday, 12 March Lecture PDFs and other materials available from: web.science.mq.edu.au/~zucker/astronomy_170.html First practicals today (immediately after lecture, E7B 213/217, 11:00 2:00) Sign up sheets for Observatory practicals will be available next week Physics/Astronomy & Astrophysics/Photonics BBQ next Thursday (11 March) 12:30 2:00 ASTR170 Introductory Astronomy: II. Light and Atoms 35

36 ASTR170 Introductory Astronomy: II. Light and Atoms 36