CH217: King 1

Inflow = dVdt

=10 liters/minute

Outflow = − dVdt

= −k[water height (cm)]

Constant = Inflow =Outflow = − dVdt

= −k[water height (cm)]

CH217: King 2

Figure 01-09

Condensation

Condensation

Evapotranspiration

CondensationSublimation

Evaporation

Snow

Snow &glaciers

Mt.runoff

Rain

Vegetation

Stream Stream flow

Infiltration

Percolation

Advection

Advection

Overland flow

Rain

Ocean

GroundwaterGroundwater flow

Groundwater

Lake

Soil moisture

Copyright © Princeton University Press 2012

CH217: King 3

Figure 01-08

Igneousrocks

Metamorphicrocks

Sedimentaryrocks

Ocean crust

Melting

MeltingMelting

Plutonism

Burial & metamorphism

Met

amor

phism

Volcanism

Lava flowsWeathering & erosion

Deposition

Weathering& erosion

Deposition &lithification

Heatpressure& stress

Melting

Cooling &crystallization Volcanic

eruptions(lava)

SedimentsMagma

New materialadded from

depth

Fluid release& melting

Sediment

A

A

A

A

B

B

D

E

ED E

E

F

F

F

F

F

G

GG

H

H

C

CC

Copyright © Princeton University Press 2012

CH217: King 4

Where do we start?o Create the Universeo Form the Earth and elementso move the elements into their

correct positionso build the atmosphere and oceans

CH217: King 5

The BIG BANG

•  The Universe was created 13.7 billion years ago in one BIG BANG ...... How do we know?

•  Start with the atom

CH217: King 6

ENERGY

Nucleus

CH217: King 7

ENERGY

Nucleus

} E = hv

CH217: King 8

CH217: King 9

Elemental Absorption

Every element has a characteristic absorption/emission spectra - (ICP)

Wavelength400 nm 700 nm

CH217: King 10

http://images.encarta.msn.com/xrefmedia/aencmed/targets/illus/ilt/T014334A.gif

Spectrum of the Sun

CH217: King 11

•  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 13.7 billion years!

Wavelength

400 nm

700 nm

CH217: King 12

Figure 02-10

1010

109

108

1026 1027 1028

Distance of galaxy (cm)

Rret

reat

vel

ocity

of g

alax

y (c

m/s

)

How to Build a Habitable Planet Copyright © Princeton University Press 2012

CH217: King 13

Figure 02-15

Dark matter:23%

Intergalactic gas: 3.6%Stars, etc.: 0.4%

Dark energy: 73%

How to Build a Habitable Planet Copyright © Princeton University Press 2012

We really don’t understand a lot about the composition of the Universe!

CH217: King 14

At the Start

Big Blob of Neutrons (N)

Protons and

electrons

11H and -1

0e

BANG

12 Minutes

CH217: King 15

http://hyperphysics.phy-astr.gsu.edu/hbase/nuclear/nucnot.html

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

CH217: King 16

2. Fusion of Protons:

4 11H + 2-1

0e ⇒ 24He + 6γ

1. Cloud of protons and electrons

11H and -1

0e

Now we are COOKING ........... Fusion produces heat

E = mc2

1 gram of hydrogen will produce 6.3x1011 j of heat.Enough heat to boil 2 million liters of H2OCompare this to our terrestrial energy consumption.

CH217: King 17

https://en.wikipedia.org/wiki/World_energy_consumption#/media/File:World_energy_consumption.svg - 2016

CH217: King 18

2. Fusion of Protons:

4 11H + 2-1

0e ⇒ 24He + 6γ

1. Cloud of protons and electrons

11H and -1

0e

3. Fusion of Helium nuclei :

24He + 2

4He ⇔ 48Be

48Be + 2

4He ⇒ 612C + γ

612Be + 2

4 He ⇒ 816O + γC

CH217: King 19

2. Fusion of Protons:

4 11H + 2-1

0e ⇒ 24He + 6γ

1. Cloud of protons and electrons

11H and -1

0e

3. Fusion of Helium nuclei :

24He + 2

4He ⇔ 48Be

48Be + 2

4He ⇒ 612C + γ

612Be + 2

4 He ⇒ 816O + γ

4. Fusion of carbon nuclei:

1123Na + 1

1H

612C + 6

12C 1020Ne + 2

4He

1224Mg + γ

This process stops at iron-56

CH217: King 20

Figure 03-05

H-burningHydrogenburning

Heliumburning

Unburnedhydrogen

Unburnedhydrogen

Name of process Fuel Products Temperature

Hydrogen-burningHelium-burningCarbon-burningNeon-burningOxygen-burningSilicon-burning

HHeC

NeO

Mg to S

HeC, O

O, Ne, Na, MgO, Mg

Mg to SElements near Fe

60 × 106 °K200 × 106 °K800 × 106 °K

1500 × 106 °K2000 × 106 °K3000 × 106 °K

Unburnedhelium

He-burningC-burning

Ne-burningO-burning

Si-burning

Hydrogenburning

How to Build a Habitable Planet Copyright © Princeton University Press 2012

CH217: King 21

Elements H-1 through Fe-56

Supernovae

Explosion

Second Generation Star

H through Fe and n

CH217: King 22

Elements H-1 through Fe-56

Supernovae

Explosion

Second Generation Star

H through Fe and n

4 11H + 2 -1

0e ⇒ 24He + 4γ

11H + 6

12C ⇒ 613C + 1

0β +

613C + 2

4He ⇒ 816O + 0

1n

2656Fe + 0

1n ⇒ 2757 Co + -1

0β

CH217: King 23

CH217: King 24

5

6

7

8

6 7 8 9

Prot

on N

umbe

r

Neutron Number

14C

14Ne-

Beta Decay

CH217: King 25

17

18

19

20

20 21 22 23

Prot

on N

umbe

r

Neutron Number

40K

40Ar

e-

Electron Capture

CH217: King 26

143

144

145

146

147

89 90 91 92 93

Prot

on N

umbe

r

Neutron Number

234Th

238U

4He

Alpha Decay

CH217: King 27

Figure 03-01

HeliumHydrogen

Oxygen

Magnesium Silicon

Iron

Boron

Lithium

Beryllium Thor

ium

Ura

niumTe

chne

tium

(no

stab

le is

otop

es; p

rodu

ct o

fsp

onta

neou

s fiss

ion)

Prom

ethi

um (n

o st

able

isot

opes

- i.e

., pro

duct

of

spon

tane

ous fi

ssio

n)

0 10 20 30 40 50 60 80 9070Atomic number

Sola

r Sys

tem

abu

ndan

ce

10-2

10-1

100

101

102

103

104

105

106

107

108

109

1010

How to Build a Habitable Planet Copyright © Princeton University Press 2012

CH217: King 28

Review of Element Formation

•  Big Bang•  Nuclear “Cooking” - Fusion•  Neutron Capture•  What is the end result?

CH217: King 29

H H

H eH e

Li Be B C N N O O F F N eN e

Na Mg A l S i P S C lC l A rA r

K Ca Sc Ti V C r Mn Fe Co Ni Cu Zn Ga Ge As Se B r K rK r

Rb S r Y Z r Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I X eX e

Cs Ba La Hf Ta W Re Os I r Pt Au Hg Tl Pb B i Po At Rn

F r Ra Ac

Ce P r Nd Pm Sm Eu Gd Tb Dy Ho E r Tm Yb Lu

Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative Abundance, Universe

CH217: King 30

H H H eH e

LiBe B

C N N O O

F F N eN e

Na Mg A l S iP

S C lC l

A rA r

K CaSc

Ti V C r MnFe

Co NiCu Zn Ga Ge As Se B r K rK r

Rb S r Y Z r Nb MoTc

Ru Rh Pd Ag Cd In Sn Sb Te I X eX e

Cs Ba La Hf Ta W ReOs I r Pt Au Hg Tl Pb B i Po At Rn

F r Ra Ac

Ce P r NdPm

Sm Eu Gd Tb Dy Ho E r Tm Yb Lu

Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative log(Abundance, Universe)

CH217: King 31

H H H eH e

Li Be B

C N N O O

F F N eN e

Na Mg A l S iP

S C lC l A rA r

K CaSc

Ti V C r Mn

FeCo Ni

Cu Zn Ga Ge

As Se B r K rRb S r Y Z r Nb Mo

TcRu Rh Pd Ag Cd In Sn Sb

Te I Xe

CsBa La Hf Ta W Re Os I r Pt Au Hg Tl Pb

B i Po At Rn

F r Ra Ac

Ce P r NdPm Sm Eu Gd Tb

DyHo E r Tm Yb Lu

Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative log(Abundance, Sun)

CH217: King 32

What about the Earth?

H HeLi Be B

C

N N

O O

F F

Ne

Na Mg A l S iP S C lC l

A r

K Ca

ScTi

V C r MnFe

Co Ni Cu Zn GaGe As

SeB r

K rRb S r Y Z r Nb

Mo

Tc Ru RhPd

Ag Cd In Sn Sb

Te

I

XeCsBa La Hf Ta W

Re Os I r Pt Au HgTl

Pb

B iPo At Rn

F r Ra Ac Ce P r Nd

Pm

Sm Eu Gd Tb Dy Ho E r Tm Yb Lu

Th

Pa

U

Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative log(Abundance, Earth)

CH217: King 33

Another look at the earth on a linear scale.

H He

Li Be B C N N

O O

F F Ne

Na Mg A l

S i

P S C lC l A r

K Ca Sc Ti V C r MnFe

Co Ni Cu Zn Ga Ge As Se B r K r

Rb S r Y Z r Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe

Cs Ba La Hf Ta W Re Os I r Pt Au Hg Tl Pb B i Po At Rn

F r Ra Ac

Ce P r Nd Pm Sm Eu Gd Tb Dy Ho E r Tm Yb Lu

Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative Abundance, Earth

•  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

CH217: King 34

.....and just for fun

H H He

Li Be B C

N N

O O

F Ne

Na Mg A l S i P S C lC l A r

K Ca Sc Ti V C r Mn Fe Co Ni Cu Zn Ga Ge As Se B r K r

Rb S r Y Z r Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe

Cs Ba La Hf Ta W Re Os I r Pt Au Hg Tl Pb B i Po At Rn

F r Ra Ac

Ce P r Nd Pm Sm Eu Gd Tb Dy Ho E r Tm Yb Lu

Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr

Relative Abundance, Human