dV Inflow 10 liters/minute dt - Colby...
Transcript of dV Inflow 10 liters/minute dt - Colby...
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