Where do we start? ocreate the Universe oform the Earth and elements omove the elements into their correct positions obuild the atmosphere and oceans

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1 Where do we start? ocreate the Universe oform the Earth and elements omove the elements into their correct positions obuild the atmosphere and oceans 1

2 The BIG BANG The Universe was created 13.8 billion years ago in one BIG BANG... How do we know? Start with the atom 2

3 ENERGY Nucleus 3

4 ENERGY }E = hv Nucleus 4

5 5

6 400 nm Wavelength 700 nm Elemental Absorption Every element has a characteristic absorption/emission spectra - (ICP) 6

7 Spectrum of the Sun 7

8 700 nm Wavelength From the magnitude of the shift we can calculate the speed of the star. The most distant stars are moving the fastest. From distance and velocity information -> TIME 13.8 billion years! nm

9 10 10 Rretreat velocity of galaxy (cm/s) Distance of galaxy (cm) Figure How to Build a Habitable Planet Copyright Princeton University Press 2012

10 We really don t understand a lot about the composition of the Universe! Dark energy: 73% Dark matter: 23% Intergalactic gas: 3.6% Stars, etc.: 0.4% Figure How to Build a Habitable Planet Copyright Princeton University Press 2012

11 At the Start Big Blob of Neutrons (N) BANG 12 Minutes Protons and electrons 1 1H and 0-1 e 11

12 12 C, 13 C, 14 C, 12 C - 12

13 1. Cloud of protons and electrons 1 1H and 0-1 e 2. Fusion of Protons: H e 2 4 He + 6γ Now we are COOKING... Fusion produces heat E = mc 2 1 gram of hydrogen will produce 6.3x10 11 j of heat. Enough heat to boil 2 million liters of H 2 O Compare this to our terrestrial energy consumption. à 4x10 20 joules. 13

14 /Nuclear_fusion#/media/File: FusionintheSun.svg 14

15 1. Cloud of protons and electrons 1 1H and 0-1 e 2. Fusion of Protons: H e 2 4 He + 6γ 3. Fusion of Helium nuclei : 2 4 He He 8 4 Be 8 4Be He 12 6 C + γ 12 6 Be C + 4 He O + γ 15

16 i/nuclear_fusion#/media/fil e:cno_cycle.svg 16

17 1. Cloud of protons and electrons 1 1H and 0-1 e 2. Fusion of Protons: H e 2 4 He + 6γ 4. Fusion of carbon nuclei: Na H 12 6C C 20 10Ne He Mg + γ 3. Fusion of Helium nuclei : 2 4 He He 8 4 Be 8 4Be He 12 6 C + γ 12 6Be He 16 8 O + γ 17 This process stops at iron-56

18 Hydrogen burning Unburned hydrogen Hydrogen burning H-burning He-burning C-burning Ne-burning O-burning Siburning Unburned hydrogen Helium burning Unburned helium Name of process Fuel Products Temperature Hydrogen-burning Helium-burning Carbon-burning Neon-burning Oxygen-burning Silicon-burning H He C Ne O Mg to S He C, O O, Ne, Na, Mg O, Mg Mg to S Elements near Fe K K K K K K Figure How to Build a Habitable Planet Copyright Princeton University Press 2012

19 Elements H-1 through Fe-56 Supernovae Explosion Second Generation Star H through Fe and n 19

20 Elements H-1 through Fe-56 Supernovae Explosion Second Generation Star H through Fe and n H e 2 4 He + 4γ 1 1 H C 13 6C + 0 1β C He 16 8 O n Fe + 1 0n Co + 0-1β 20

21 21

22 Beta Decay 8 Proton Number N 14 C e Neutron Number 22

23 Electron Capture 20 Proton Number K e- 40 Ar Neutron Number 23

24 Alpha Decay 147 Proton Number Th 4 He 238 U Neutron Number 24

25 Solar System abundance Hydrogen Helium Oxygen Magnesium Boron Lithium Beryllium Silicon Iron Technetium (no stable isotopes; product of spontaneous fission) Promethium (no stable isotopes - i.e., product of spontaneous fission) Thorium Uranium Atomic number Figure How to Build a Habitable Planet Copyright Princeton University Press 2012

26 Review of Element Formation Big Bang Nuclear Cooking - Fusion Neutron Capture What is the end result? 26

27 H Relative Abundance, Universe He Li Be B C N O F Ne Na Mg Al Si P S C l A r K Ca Sc Ti V Cr Mn Fe Co Ni Cu Zn Ga Ge As Se Br K r Rb Sr Y Zr Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe Cs Ba La Hf Ta W Re Os Ir Pt Au Hg Tl Pb Bi Po At Rn Fr Ra Ac Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr 27

28 H Relative log(abundance, Universe) He Li B Na Mg Be Al Fe Ca K Ti Cr V Mn Co Ni Cu Zn Sc Ga C Si Ge N P As O S F C l Ne A r Se Br K r Rb Sr Y Cs Ba La Zr Hf Nb Ta Mo W Tc Re Ru Rh Pd Ag Cd In Os Ir Pt Au Hg Tl Sn Pb Sb Te I Xe Bi Po At Rn Fr Ra Ac Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr 28

29 H Relative log(abundance, Sun) He Na B Li Mg Be Al K Rb Cs Ca Sr Ba Sc Ti V Cr Y Zr Nb Mo La Fr Ra Ac Hf Ta W Mn Tc Fe Co Ni Cu Zn Ga C Si Ge Ru Rh Pd Ag Cd In Sn Re Os Ir Pt Au Hg Tl Pb N P O S F C l Ne A r As Se Br Kr Sb Te I Xe Bi Po At Rn Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr 29

30 What about the Earth? Relative log(abundance, Earth) O Na Li H Mg Al Be B K Rb Cs Ca Sr Ba Sc Y La Ti Zr V Nb Cr Mo Hf Ta W Mn Fe Co Ni Cu Zn Ga Tc Ru Rh Pd Ag Cd In Re Os Ir Pt Au Hg Tl Si Ge Sn Pb C N F P S C l As Sb Bi Se Te Br I He Ne Ar Kr Xe Po At Rn Fr Ra Ac Ce Pr Nd Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th U Pm Pa Np Pu Am Cm Bk Cf Es Fm Md No Lr 30

31 Another look at the earth on a linear scale. Relative Abundance, Earth O H Si Li Be B C N Na K Mg Ca Al F P S C l Sc Ti V Cr Mn Fe Co Ni Cu Zn Ga Ge As Se Br Kr Rb Sr Y Zr Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe Cs Ba La Hf Ta W Re Os Ir Pt Au Hg Tl Pb Bi Po At Rn Fr Ra Ac He Ne Ar Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr 31 Where did all the other elements go? H, He, C, N?? They got BLOWN AWAY stay tuned! This leaves just Si, Mg, Fe, and O

32 ...and just for fun Relative Abundance, Human O H Li Be B C N F He Ne Na Mg Al Si P S C l Ar K Ca Sc Ti V Cr Mn Fe Co Ni Cu Zn Ga Ge As Se Br Kr Rb Sr Y Zr Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe Cs Ba La Hf Ta W Re Os Ir Pt Au Hg Tl Pb Bi Po At Rn Fr Ra Ac Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr 32

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