Chapter 6. Atoms and Starlight
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1 Chapter 6 Atoms and Starlight
2 What is light?
3
4 Light is an electromagnetic wave.
5 Wavelength and Frequency wavelength frequency = speed of light = constant
6 Particles of Light Particles of light are called photons. Each photon has a wavelength and a frequency. The energy of a photon depends on its frequency.
7 The Amazing 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
8 Spectra of stars are more complicated than pure blackbody spectra. Light and Matter characteristic lines, called absorption lines. To understand those lines, we need to understand atomic structure and the interactions between light and atoms.
9 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.
10 If you could fill a teaspoon just with material as dense as the matter in an atomic nucleus, it would weigh ~ 2 billion tons!!
11 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
12 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. These characteristic electron energies are different for each individual element. r 3, E 3 r 2, E 2 r 1, E 1
13 Atomic Transitions An electron can be kicked into a higher orbit when it absorbs a photon with exactly the right energy. E ph = E 3 E 1 E ph = E 4 E 1 The photon is absorbed, and the electron is in an excited state. Wrong energy (Remember that E ph = h*f) All other photons pass by the atom unabsorbed.
14 Chemical Fingerprints Downward transitions produce a unique pattern of emission lines.
15 Chemical Fingerprints Because those atoms can absorb photons with those same energies, upward transitions produce a pattern of absorption lines at the same wavelengths. Production of Absorption Lines
16 Chemical Fingerprints Each type of atom has a unique spectral fingerprint.
17 Chemical Fingerprints Observing the fingerprints in a spectrum tells us which kinds of atoms are present.
18 Example: Solar Spectrum
19 Color and Temperature Stars appear in different colors, from blue (like Rigel) via green / yellow (like our sun) to red (like Betelgeuze). Orion Betelgeuze These colors tell us about the star s temperature. Rigel
20 Blackbody Radiation 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 Blackbody Spectrum. A perfect blackbody emitter would not reflect any radiation. Thus the name Blackbody.
21 Two Laws of Blackbody Radiation 1. The hotter an object is, the more luminous it is. 2. The peak of the blackbody spectrum shifts towards shorter wavelengths when the temperature increases.
22 Kirchhoff s Laws of Radiation 1. A solid, liquid, or dense gas excited to emit light will radiate at all wavelengths and thus produce a continuous spectrum.
23 Kirchhoff s Laws of Radiation 2. 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..
24 Kirchhoff s Laws of Radiation 3. 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
25 The Spectra of Stars 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.
26 Most prominent lines in many astronomical objects: Balmer lines of hydrogen Lines of Hydrogen
27 The Balmer Lines n = 1 Transitions from 2 nd to higher levels of hydrogen H a H b H g The only hydrogen lines in the visible wavelength range. 2 nd to 3 rd level = H a (Balmer alpha line) 2 nd to 4 th level = H b (Balmer beta line)
28 Absorption spectrum dominated by Balmer lines Modern spectra are usually recorded digitally and represented as plots of intensity vs. wavelength.
29 Emission nebula, dominated by the red Ha line
30 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
31 Measuring the Temperatures of Stars Comparing line strengths, we can measure a star s surface temperature!
32 Temperature Spectral Classification of Stars Different types of stars show different characteristic sets of absorption lines.
33 Spectral Classification of Stars 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
34 Stellar spectra O B A F G K M Surface temperature
35 The Composition of Stars From the relative strength of absorption lines (carefully accounting for their temperature dependence), one can infer the composition of stars.
36 Infrared spectra of stars Major differences appear in the infrared spectra of cool stars (M stars T, L dwarfs).
37
38 The Doppler Effect The light of a moving source is blue/red shifted by Dl/l 0 = v r /c Blue Shift (to higher frequencies) v r Red Shift (to lower frequencies) l 0 = actual wavelength emitted by the source Dl = Wavelength change due to Doppler effect v r = radial velocity
39 Measuring the Shift Stationary Moving Away Away Faster Moving Toward Toward Faster We generally measure the Doppler effect from shifts in the wavelengths of spectral lines.
40 Example: Earth s orbital motion around the sun causes a radial velocity towards (or away from) any star.
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