life on our evolving planet optical physicist in aerospace for twenty years designed and analyzed...
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Life on Our Evolving Planetoptical physicist in aerospace for twenty years
designed and analyzed laser optical systems
Informal science educator in Morro Bay State ParkMuseum of Natural History for ten years
5 global evolution walks in parks12 animated slide shows in museum3 poster exhibits in museum and at Cal Poly
Cal Poly adjunct physics professor for seven yearsand research scholar in residence
4 senior projects Phys 461-4648 summer student projects13 special problems projects (Phys, Geol, Bio, Chem 200 or 400)Phys470 Advanced Topics: Solar and Global Evolution
visit my website at www.calpoly.edu/~rfield
Bob Field
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What is a system?
Is the system open or closed?
a system has parts that interact
and may have emergent properties
Dr Art Sussman’s Guide to Planet Earthenergy flows, matter cycles, web of life
energy
matter
energy
matter
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How did a giant cloud of cold dilute gas and
dust evolve into astronauts in a spacecraft
orbiting a planet orbiting a star?
The ultimate question for
Earth System History is:
Life on Our Evolving Planet
The National Academy of Sciences says that
it is the role of science to provide
plausible natural explanations of natural phenomena
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Simple building blocksevolve into complex systems
when energy flows
Everything Evolvesoceans and atmosphere
solid Earth and Sunmolecules and cells
organisms and ecosystems
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C6 12
N7 14
O8 16
H1 1
He2 4Periodic Table of
Chemical Elements
92% ~8%
0.07%0.04%0.02%0.01%
Abundance in Universe in %0.1% }
Ne10 20
Na11 23
Mg12 24
Al13 27
Si14 28
P15 31
S16 32
Cl17 35
Ar18 40
K19 39
Ca20 40
Cr24 62
Mn25 55
Fe26 56
Ni28 59
0.02% everything else
Big stars build big atomsSunlight is the waste product
Sun fuses 4 H1 → He4
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composition in our LANL solar evolution code
sunsolar composition
"metals", 1
Helium, 28
Hydrogen, 71
solar "metals" composition
Nitrogen, 7.0
Magnesium, 5.0other, 1.3
Carbon, 22.9Oxygen, 63.9
composition by mass
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about 93% CHO by mass
ancient atmosphere ??? 2CO2+CH4+NH3+4H2O
Carbon, 18.7
Nitrogen, 7.3
Oxygen, 66.3
Hydrogen, 7.8
Simple building blocks
comet volatiles composition
Nitrogen, 5.2
Sulfur, 1.3Phosphorus, 0.3
Carbon, 16.6
Hydrogen, 7.8
Oxygen, 68.7
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about 97% CHO by mass
Complex Systems
bacteria composition
Oxygen, 73.8
Hydrogen, 10.0
Carbon, 12.2
Nitrogen, 3.1
Sulfur, 0.3Phosphorus, 0.6
mammal composition
Hydrogen, 9.3
Oxygen, 63.6
Carbon, 19.3
Calcium, 1.4
Nitrogen, 5.1
Phosphorus, 0.6
Sulfur, 0.6
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wikipedia
elemental composition of the ocean and the atmosphere
seawater
Hydrogen, 10.8
Oxygen, 85.7
Sodium, 1.05
Chlorine, 1.9Carbon, 0.0026
other, 0.308
atmosphere
Carbon, 0.01
Nitrogen, 78
Argon, 1.1
Oxygen, 20.9
Hydrogen, 0.01
composition by mass
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McDonough
Elemental Composition of the Earth
whole EarthSulfur, 0.6
Chromium, 0.5
Calcium, 1.7other, 0.5
Aluminum, 1.6
Silicon, 16.1
Magnesium, 15.4
Nickel, 1.8
Oxygen, 29.7
Iron, 32
Continental Crust
Calcium, 5.29
other, 4Aluminum, 8.41
Silicon, 26.77
Magnesium, 3.2
Oxygen, 45.3
Iron, 7.07
composition by mass
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OH C H
H
H
OH C H
H
H
C
H
H
C C C C C C C C C C CH N
CC CH N
C
H
H OH
H
H
H
C OC
CH N
CC NNC
H
N
H
N
CHONSP molecules are abundant in space:100 tons per year of IDPs land on Earth
(interplanetary dust particles) Cradle of Life pages 133-5 by William Schopf
C
H
H S
Organic molecules have many variations on a few themes
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backbone of
phospholipid (H and O not shown)
CO, H2, PO4 are building blocks of phospholipids found in cell membranes
RC C C C C C C C
PiC C C C C
CC
C
fatty membrane spheresform naturally in meteors
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all cells are descended from a common ancestor
What do cells do?
Modern cells are chemical factories that store, exchange, and transform
matter, energy, and information
prokaryote
eukaryote
5 kingdoms:bacteria
algaefungusplant
animal
energy
matter
energy
matter
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What are the building blocks of molecules?
A, B, and C are all about 97% CHO
OC SH N P
Life’s Origin page 15by Walter Schopf A B C
Hydrogen 61 63 56
Oxygen 26 29 31
Carbon 10.5 6.4 10
Mammal
Nitrogen 2.4 1.4 2.7
Sulfur 0.13 0.06 0.3
Phosphorus 0.13 0.12 0.08
Calcium 0.23 - -
Bacteria Comet
composition by number of atoms
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atoms can share or transfer electronsH – 1He – 0O – 2C – 4N – 3S – 2
P – 3 or 5
H
H
O
O
O
O
P
N
NC H
H
H
H
C
O
O
SH
H
N
H
HH O ON
OO
H
H
O
O
OC SH N P
many common molecules are made from CHONSP
C
O
S
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Methane can form new molecules O
H C H
H
H
O
methanolmethane
formaldehyde
formic acid biochemists give big names to
small molecules
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C
H
O
HC
H
C
H O
C
H
H
OC
H
H
O
H
H
O
C
H
H
O
C
H
H O C
H
H O
C
H
H O
C
H
H O
C
H
H O C
H
H O
6 CH2O+ energy+ catalyst
C
O
C
H
O
C H
H
O
glucose is a building block of carbohydrates
glucose
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C
H
O
HC
H
C
H O
C
H
H
OC
H
H
O
H
H
O
C
H
H
O
Sunlight
photosynthesis makes glucose from sunlight, carbon dioxide, and water
C
O H
H
O
O
6 H2O
H
H
O
H
H
O H
H
O
H
H
O H
H
O
C
O
O
C
O
O
C
O
O
C
O
O
C
O
O
6 CO26 O2glucose
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C
O
C
H
O
C H
H
O
C
O
C
H
O
C H
H
O
glucose supplies energy to make ATP
C3H3O3
C
H
O
HC
H
C
H O
C
H
H
OC
H
H
O
H
H
O
C
H
H
O
C3H3O3
glucose
ATP
ATP
aerobic fermentation makes 2 more ATP
ATP
ATP
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C
H
O
HC
H
C
H O
C
H
H
OC
H
H
O
H
H
O
C
H
H
O
respiration liberates energy by oxidizing glucose into carbon dioxide and water
C
O H
H
O
O
6 H2O
H
H
O
H
H
O H
H
O
H
H
O H
H
O
C
O
O
C
O
O
C
O
O
C
O
O
C
O
O
6 CO2
ATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATP
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low tide in Corallina Cove - Montana de Oro
Bob Field 2000
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Moon
core
lower mantle
upper mantle
oceanic lithosphere
oceaniccrust
oceans
biosphere
atmosphere
subcontinentallithosphere
sedimentslower crust
upper crust
impactsInteractions
between Earth systems
Condie33Fig 1.33
sunw
hen
en
ergy
flo
ws,
co
mp
lexi
ty g
row
s
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Solar and Global Evolutionare parts of Cosmic Evolution
generic systemaverage power density (W/kg)
galaxies 0.00005
stars 0.0002
planets 0.01
plants 0.1
animals 2
brains 15
society 50
table from Chaisson139 when energy flows, complexity grows
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The Facts of Life: From the Oceans to the Stars
I. Oceans and Atmosphere Evolve
1. Voracious Predators
2. Luke Skylighter and Dark Weighter
3. Fire and Ice
II. The Solid Earth and Sun Evolve
4. Toxic Flying Insects
5. Global Cooling
6. Solar Heating
III. The Biosphere Evolves
7. Bacteria and Viruses
8. Gaia and Hypersea
9. Asteroids and Astronauts
IV. Intelligent Life Evolves
10. Cosmo Sapiens
11. Sustainability
12. The Quest for HOPE
Appendices
A. Five Billion Year Global Evolution Timelines
B. Earth Systems Database
1. Oceans and Atmosphere
2. Sun and Solid Earth
3. Biosphere
©Bob Field 2007
The National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? Global evolution studies explore five kingdoms of life and the five billion years of physical, chemical, and biological evolution that have shaped the solid Earth, hydrosphere, atmosphere, and biosphere (including its molecules, cells, organisms, and ecosystems).
This is the dust cover of a book that I want to write.
I have been researching the subject for years.
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I am seeking students and faculty to help me develop a
global evolution website featuring:
1. a five-billion-year timeline of globally important events
in 100 million year intervals
2. a database of properties and processes of the Sun and
the Earth and its subsystems
3. time dependent math models of solar and global system
structures and flows of energy and material
4. constructivist thematic educational resources for
students, educators, and the public
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Global Evolution: The First Five Billion YearsThe National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? The short answer is when energy flows, complexity grows.
The fact is that the solid Earth, hydrosphere, atmosphere, and biosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems, a process that I call global evolution. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of a complex natural system.
Solar SystemSun
Solid Earth
HydrosphereAtmosphere
Geobiosphere
Molecules and CellsOrganisms and Ecosystems
Astronauts
Global Evolution Timelines Earth Systems Data Base
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The Structure and Evolution of the Solar System including the Sun and the Solid Earth
The first section investigates the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of the solar system including the Sun and the Solid Earth.
Solar System Sun Solid Earth
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The Structure and Evolution of the Hydrosphere, Atmosphere, and Geobiosphere
The fact is that the hydrosphere, atmosphere, and geobiosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems, a process that I call global evolution. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of these global systems.
Hydrosphere Atmosphere Geobiosphere
percolation
precipitation
27
vapor transport10
groundwater flow
return flow10
percolation
precipitation
27
vapor transport10
groundwater flow
return flow10
precipitation
94
precipitation
94
After Stowe
oceans hold340 M cubic miles
units - 1000 cubic miles/year
evaporation & transpiration
17 evaporation
104
evaporation & transpiration
17 evaporation
104
Average Global Energy Budget
50
100
20
30
incidentsunlight
absorb
scatteredsunlight
absorb
sea + land
atmosphere
Sun
30
30
evap
condense
90
65
155
absorb
radiate
radiate
5
110
105
radiate
absorb
radiated heatLWIR
30
30
evap
condense
90
65
155
absorb
radiate
radiate
5
110
105
radiate
absorb
radiated heatLWIR
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The Structure and Evolution of molecules, cells, organisms, ecosystems, and even astronauts
How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? The short answer is when energy flows, complexity grows.
The fact is that the solid Earth, hydrosphere, atmosphere, and biosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of a complex natural system.
Molecules and Cells Organisms and Ecosystems Astronauts
A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G AA C UA C UC C UC C UG A UG A UG C UG C UC A GC A GU G UU G UC A AC A AA U AA U AC G CC G CG U AG U A
after Trefil and HazenThe Sciences:
An Integrated Approach
AlaHis Tyr Val Thr Val Arg Leu GlyH2OH2O H2OH2O
H2OH2O H2OH2O H2OH2O H2OH2O H2OH2O H2OH2O
ribosomes synthesize proteins by translating mRNA to tRNAs that are attached to amino acids
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Global Evolution Timelines:Can you identify and sequence the globally important events in the natural history of the oceans, atmosphere, solid Earth, Sun, molecules, cells, organisms, and ecosystems?
from MY
to MY
MYA Eraoceans
and atmosphere
solid Earth and Sun
molecules and cells
organisms and
ecosystems-300 -200 -4900-200 -100 -4800-100 0 -4700
ZAMS 100 -4600100 200 -4500200 300 -4400300 400 -4300400 500 -4200500 600 -4100600 700 -4000700 800 -3900800 900 -3800900 1000 -37001000 1100 -36001100 1200 -35001200 1300 -34001300 1400 -33001400 1500 -32001500 1600 -31001600 1700 -30001700 1800 -29001800 1900 -28001900 2000 -27002000 2100 -26002100 2200 -25002200 2300 -24002300 2400 -23002400 2500 -22002500 2600 -21002600 2700 -20002700 2800 -19002800 2900 -18002900 3000 -17003000 3100 -16003100 3200 -15003200 3300 -14003300 3400 -13003400 3500 -12003500 3600 -11003600 3700 -10003700 3800 -9003800 3900 -8003900 4000 -7004000 4100 -6004100 4200 -5004200 4300 -4004300 4400 -3004400 4500 -2004500 4600 -1004600 4700 now
Phaner- ozoic
Pro
tero
zoic
The Natural History of Planet Earth Timeline: Five Billion Years of Solar and Global Evolution
Had
ean
Pre-Hadean
Arc
hae
an
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Earth Systems Database: The SunThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
Solar Evolution
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
0E+00 1E+09 2E+09 3E+09 4E+09Time (years)
Rel
ativ
e V
alu
e
T/Tsun
R/Rsun
L/Lsun
cycle 17
relative volume
fusion core 16
radiative zone 343
convective zone 641
relative mass
fusion core 481radiative
zone 492
convective zone 27
relative heat flow
1000988
1000
0
200
400
600
800
1000
fusion core radiative zone convective zone
relative total energy
radiative zone 356
fusion core 637
convective zone 7
relative fusion power
convective zone 0
fusion core 988
radiative zone 12
Sun layers volume (cm3) mass (g)average density
(g/ cm3)
relative volume
relative mass
relative average density
fusion core 2.22E+31 9.57E+32 43.19 16 481 30784
radiative zone 4.86E+32 9.79E+32 2.01 343 492 1434
convective zone 9.10E+32 5.37E+31 0.06 641 27 42
whole Sun 1.42E+33 1.99E+33 1.40 1000 1000 1000
layerstotal
energy (ergs)
fusion power
(erg/ s)
luminosity (erg/ s)
relative total
energy
relative fusion power
relative heat flow
fusion core 1.95E+48 3.80E+33 3.80E+33 637 988 988
radiative zone 1.09E+48 4.62E+31 3.85E+33 356 12 1000
convective zone 2.00E+46 0.00E+00 3.85E+33 7 0 1000
whole Sun 3.06E+48 3.85E+33 3.85E+33 1000 1000 1000
layers volume (cm3) mass (g)average density
(g/ cm3)
relative volume
relative mass
relative average density
fusion core 2.22E+31 9.57E+32 43.19 16 481 30784
radiative zone 4.86E+32 9.79E+32 2.01 343 492 1434
convective zone 9.10E+32 5.37E+31 0.06 641 27 42
whole Sun 1.42E+33 1.99E+33 1.40 1000 1000 1000
layerstotal
energy (ergs)
fusion power
(erg/ s)
luminosity (erg/ s)
relative total
energy
relative fusion power
relative heat flow
fusion core 1.95E+48 3.80E+33 3.80E+33 637 988 988
radiative zone 1.09E+48 4.62E+31 3.85E+33 356 12 1000
convective zone 2.00E+46 0.00E+00 3.85E+33 7 0 1000
whole Sun 3.06E+48 3.85E+33 3.85E+33 1000 1000 1000
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Earth Systems Database: The Solid EarthThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
layersinternal
energy (J )
heat sources
(W)total heat flow (W)
relative internal energy
relative heat
sourcesrelative
heat flowinner core 3.15E+29 9.85E+11 9.85E+11 19 23 23outer core 5.35E+30 1.11E+12 2.10E+12 315 26 49lower mantle 9.12E+30 2.43E+13 2.64E+13 537 568 617upper mantle 2.09E+30 8.22E+12 3.46E+13 123 192 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000continental crustocean crust
layersinternal
energy (J )
heat sources
(W)total heat flow (W)
relative internal energy
relative heat
sourcesrelative
heat flowcore 5.67E+30 2.10E+12 2.10E+12 333 49 49mantle 1.12E+31 3.25E+13 3.46E+13 659 760 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000
layersvolume (m^3) mass (kg)
average density
(kg/ m^3)relative volume
relative mass
relative average density
inner core 7.63E+18 9.83E+22 1.29E+04 7 17 2348outer core 1.69E+20 1.83E+24 1.08E+04 156 308 1977lower mantle 6.00E+20 2.92E+24 4.87E+03 554 492 889upper mantle 2.67E+20 9.63E+23 3.61E+03 246 162 658lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000continental crustocean crust
layersvolume (m^3) mass (kg)
average density
(kg/ m^3)relative volume
relative mass
relative average density
core 1.77E+20 1.93E+24 1.19E+04 163 325 2162mantle 8.66E+20 3.88E+24 4.24E+03 800 654 773lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000
layersinternal
energy (J )
heat sources
(W)total heat flow (W)
relative internal energy
relative heat
sourcesrelative
heat flowinner core 3.15E+29 9.85E+11 9.85E+11 19 23 23outer core 5.35E+30 1.11E+12 2.10E+12 315 26 49lower mantle 9.12E+30 2.43E+13 2.64E+13 537 568 617upper mantle 2.09E+30 8.22E+12 3.46E+13 123 192 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000continental crustocean crust
layersinternal
energy (J )
heat sources
(W)total heat flow (W)
relative internal energy
relative heat
sourcesrelative
heat flowcore 5.67E+30 2.10E+12 2.10E+12 333 49 49mantle 1.12E+31 3.25E+13 3.46E+13 659 760 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000
layersvolume (m^3) mass (kg)
average density
(kg/ m^3)relative volume
relative mass
relative average density
inner core 7.63E+18 9.83E+22 1.29E+04 7 17 2348outer core 1.69E+20 1.83E+24 1.08E+04 156 308 1977lower mantle 6.00E+20 2.92E+24 4.87E+03 554 492 889upper mantle 2.67E+20 9.63E+23 3.61E+03 246 162 658lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000continental crustocean crust
layersvolume (m^3) mass (kg)
average density
(kg/ m^3)relative volume
relative mass
relative average density
core 1.77E+20 1.93E+24 1.19E+04 163 325 2162mantle 8.66E+20 3.88E+24 4.24E+03 800 654 773lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000
relative internal energy
lithosphere7
lower mantle537
upper mantle123
outer core315
inner core19
relative mass
lithosphere21
lower mantle492
upper mantle162
outer core308
inner core17
relative volume
lower mantle554
upper mantle246
outer core156
lithosphere37
inner core7
relative total heat sources
lithosphere191
lower mantle568
upper mantle192
outer core26
inner core23
relative heat flow
23 49
1000
809
617
0
200
400
600
800
1000
inner core outer core lowermantle
uppermantle
lithosphere
models of growth of continental volume (%)
4 3 2 1 0BYA
100
75
50
25
0
1992
geo
chem
ical
Van Andel
linear re
ference
1992 geochemicalBYA: %
0: 1000.6: 902.6: 103.6: 04.5: 0
4 3 2 1 0BYA
100
75
50
25
0
1992
geo
chem
ical
Van Andel
linear re
ference
1992 geochemicalBYA: %
0: 1000.6: 902.6: 103.6: 04.5: 0
4 3 2 1 0BYA
100
75
50
25
0
1992
geo
chem
ical
Van Andel
linear re
ference
1992 geochemicalBYA: %
0: 1000.6: 902.6: 103.6: 04.5: 0
from VanAndel Fig. 13.6
Radiogenic Heat Flow (W)
0000E+00
20E+12
40E+12
60E+12
80E+12
100E+12
120E+12
-5 -4 -3 -2 -1 0Time (BY)
Rad
iog
enic
Hea
t F
low
(W
)
Total
U-235
K-40
U-238
Th-232
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Earth Systems Database: The HydrosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
Percent of total
97.25
2.050.68
0.010.005
0.001
0.0001 0.000040.00001
0.0001
0.001
0.01
0.1
1
10
100
Oce
ans
Ice
cap
s &
gla
cier
s
Gro
un
dw
ater
Lak
es
So
ilm
ois
ture
Atm
osp
her
e
Str
eam
s &
rive
rs
Bio
sph
ere
reservoir
stored water
wikipedia
average rate (10³ km³/year)
10771
36
398434
0
100
200
300
400
500
Precipitationover land
Evaporationfrom land
Runoff &groundwater
from land
Precipitationover oceans
Evaporationfrom oceans
water fluxwikipedia
transmission vs. depth
0
50
100
150
200
250
300
350
0 1 3 10 30 100depth (m)
pure
particulate
DOM
chlorophyll
Field - solar sea flux code
300 350 400 450 500 550 600 650 700 750 8000
0.2
0.4
0.6
0.8
max
0
Tz z k 0 Hy ( )
21 Hx ( )
Field - solar sea flux code
transmitted sunlight in pure water vs. depth(0, 1, 3, 10, 30, 100 meters)
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Earth Systems Database: The AtmosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
Average Flux for Clean, Dry Air at 35 N
0
100
200
300
400
500
Total UV Visible Infrared
0.3-3.0 0.3-0.4 0.4-0.7 0.7-3.0Spectral Band (microns)
Flu
x (W
/m^
2)
Scattering Losses
Absorption Losses
Flux at Surface
Field - solar flux code
cloudfree sky
12108642240
0.02
0.04
0.06
0.08
0.1
0.12
NoonMidnight 6 am14 16 18 20 22 24
Noon Midnight6 pm
Summer SolsticeSolar Flux vs. Time of Day
EquatorEquator
Tropicof
Cancer
Tropicof
Cancer
Arctic CircleArctic Circle
North PoleNorth Pole
Average Global Energy Budget
50
100
20
30
incidentsunlight
absorb
scatteredsunlight
absorb
sea + land
atmosphere
Sun
30
30
evap
condense
90
65
155
absorb
radiate
radiate
5
110
105
radiate
absorb
radiated heatLWIR
30
30
evap
condense
90
65
155
absorb
radiate
radiate
5
110
105
radiate
absorb
radiated heatLWIR
Thermal Structure of Troposphere
0
1
2
3
4
5
6
7
8
9
10
210 220 230 240 250 260 270 280 290 300 310 320
Temperature (K)
alt
itu
de
(k
m)
downwelling temperature (K)
upwelling temperature (K)
Salby237
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Earth Systems Database: The BiosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
carbon (Gt) on a logarithmic scale
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
1E+6
1E+7
1E+8
1E+9
Atmos
phere
CO2 (at
pre-i
ndus
trial
280 p
pmv)
Ocean
Dissolv
ed in
orga
nic (D
IC)
Dissolv
ed or
ganic
(DOC)
Particu
late o
rgan
ic (P
OC)
Ocean
biota
Land b
iota
Phytom
ass
Bacter
ia an
d fun
gi
Land A
nimals
Land
Soil hu
mus
Reacti
ve fr
actio
n of h
umus
Dead o
rgan
ic matt
er, li
tter,
peat
Inor
ganic
soil
(CaC
O3)
Sedim
ents
Carbon
ate se
dimen
ts
Organ
ic matt
er se
dimen
ts
Contin
ental
crus
t
Ocean
ic cru
st
Upper
mantle
FluxCarbon Gt/year
gross primary production 203from atmosphere to land biota 110
from ocean to ocean biota 93respiration 89.5
from land biota to atmosphere 46.9from ocean biota to ocean 42.6
Net primary production (NPP) 113.5from atmosphere to land biota 63.1
from ocean to ocean biota 50.4Volatilization from soil organic matter to atmosphere 62.5Net exchange from atmosphere to land 0.6Weathering consumption of CO2 from atmosphere to sediments 0.26Net exchange to atmosphere from ocean 0.51
dissolution from atmosphere to ocean 96evasion to atmosphere from ocean 96.51
River input of dissolved C (DIC + DOC) to ocean 0.6DIC 0.38DOC 0.22POC 0.19PIC 0.18
Oceanic sediment long-term storage 0.28Carbonates 0.22
Organic matter 0.06Volcanism, metamorphism, hydrothermal from land to atmosphere 0.22Uplift 0.4
bacteria composition
Oxygen, 73.8
Hydrogen, 10.0
Carbon, 12.2
Nitrogen, 3.1
Sulfur, 0.3Phosphorus, 0.6
mammal composition
Hydrogen, 9.3
Oxygen, 63.6
Carbon, 19.3
Calcium, 1.4
Nitrogen, 5.1
Phosphorus, 0.6
Sulfur, 0.6
Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et alin Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003
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4 MY
4 BYhttp
://g
eolo
gy.w
r.us
gs.g
ov/p
arks
/gti
me/
Gti
mes
cale
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Time MYA Event
4 Development of hominid bipedalism
4-1 Australopithecus exist
3.5 The Australopithecus Lucy walks the Earth
2 Widespread use of stone tools
2-0.01 Most recent ice age
1.6-0.2 Homo erectus exist
1-0.5 Homo erectus tames fire
0.3Geminga supernova explosion at a distance of roughly 60 pc--roughly as bright as the Moon
0.2-0.03 Homo sapiens neanderthalensis exist
0.050-0 Homo sapiens sapiens exist
0.04-0.012Homo sapiens sapiens enter Australia from southeastern Asia and North America from northeastern Asia
0.025-0.010 Most recent glaciation--an ice sheet covers much of the northern United States
0.020 Homo sapiens sapiens paint the Altamira Cave
0.012 Homo sapiens sapiens have domesticated dogs in Kirkuk, Iraq
0.01 First permanent Homo sapiens sapiens settlements
0.01 Homo sapiens sapiens learn to use fire to cast copper and harden pottery
0.006 Writing is developed in Sumeria
www.talkorigins.org/origins/geo_timeline.html
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Time MYA Event
4600 Formation of the approximately homogeneous solid Earth by planetesimal accretion
4300Melting of the Earth due to radioactive and gravitational heating which leads to its differentiated interior structure as well as outgassing of molecules such as water, methane, ammonia, hydrogen, nitrogen, and carbon dioxide
4300Atmospheric water is photodissociated by ultraviolet light to give oxygen atoms which are incorporated into an ozone layer and hydrogen molecules which escape into space
4000 Bombardment of the Earth by planetesimals stops
3800 ? The Earth's crust solidifies--formation of the oldest rocks found on Earth
3800 ? Condensation of atmospheric water into oceans
3500-2800 Prokaryotic cell organisms (eubacteria and archaebacteria) develop
3500-2800Beginning of photosynthesis by cyanobacteria which releases oxygen molecules into the atmosphere and steadily works to strengthen the ozone layer and change the Earth's chemically reducing atmosphere into a chemically oxidizing one
2400Rise in the concentration of oxygen molecules stops the deposition of uraninites (since they are soluble when combined with oxygen) and starts the deposition of banded iron formations
1600The last reserves of reduced iron are used up by the increasing atmospheric oxygen--last banded iron formations
1500 Eukaryotic cell organisms develop (common ancestors of algae, fungi, plants, animals)
1500-600 Rise of multicellular organisms (algae, fungi, plants, animals)
580-545 Fossils of Ediacaran organisms are made (biomineralized bodies)
www.talkorigins.org/origins/geo_timeline.html
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from MY
to MY
MYA Eraoceans
and atmosphere
solid Earth and Sun
molecules and cells
organisms and
ecosystems-300 -200 -4900-200 -100 -4800-100 0 -4700
ZAMS 100 -4600100 200 -4500200 300 -4400300 400 -4300400 500 -4200500 600 -4100600 700 -4000700 800 -3900800 900 -3800900 1000 -37001000 1100 -36001100 1200 -35001200 1300 -34001300 1400 -33001400 1500 -32001500 1600 -31001600 1700 -30001700 1800 -29001800 1900 -28001900 2000 -27002000 2100 -26002100 2200 -25002200 2300 -24002300 2400 -23002400 2500 -22002500 2600 -21002600 2700 -20002700 2800 -19002800 2900 -18002900 3000 -17003000 3100 -16003100 3200 -15003200 3300 -14003300 3400 -13003400 3500 -12003500 3600 -11003600 3700 -10003700 3800 -9003800 3900 -8003900 4000 -7004000 4100 -6004100 4200 -5004200 4300 -4004300 4400 -3004400 4500 -2004500 4600 -1004600 4700 now
Phaner- ozoic
Pro
tero
zoic
The Natural History of Planet Earth Timeline: Five Billion Years of Solar and Global Evolution
Had
ean
Pre-Hadean
Arc
hae
anName ten or more
globally important eventsin any column.
Think about the W5H:whowhatwhenwherewhyhow
Emphasis onconnections not collections
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Senior Projects, Summer Projects, non-thesis Masters Projects, or Special Problems BIO, CHEM, or GEOL 200 or 400
Students may do library research (books, journals, websites), original thinking, and/or data analysis.
Five Billion Years of Global EvolutionIdentify and sequence globally important physical, chemical, and/or biological events and processes in the five billion year history of the solid Earth, hydrosphere, atmosphere, and/or biosphere (molecules, cells, organisms, and ecosystems) with emphasis on Pre-Cambrian eras.
Prokaryote and Eukaryote EvolutionStudy the structure and evolution of prokaryotes, eukaryotes, biologically
important molecules, and/or metabolic processes. Emphasis is on Pre-Cambrian cladograms based on molecular clocks and fossil records.
Biochemical and Geochemical EvolutionStudy biochemical, geochemical, and/or biogeochemical properties and
processes from cellular to global scales in Hadean, Archaean, Proterozoic, and/or Phanerozoic Eras.
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http://en.wikipedia.org/wiki/Bacterium
Prokaryote and
Eukaryote Evolution
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Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et alin Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003
4112
Arc
haea
3977
Aqu
ifex
3644
The
rmot
oga
3096
Chl
orob
ium
Cya
noba
cter
ia26
88 F
irm
icut
es29
23 F
usob
acte
rium
2800
Pro
teob
acte
ria
1351
Ani
mal
s14
58 F
ungi
1558
Alg
ae
1609
Alg
fung
imal
1513
Fun
gim
al
2309
Euk
aryo
tes
2100
? R
espi
rato
rs
Evaluate accuracy of molecular timescales
Identify and describe node organisms and characters
Provide common names for each label
Enter data into my 5 BY timeline
Investigate environmental and ecological causes
Examine environmental and ecological impacts
Describe ecosystems prevalent in each era
Create separate charts for each geologic era
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global average of 40 inches of precipitation per year
recycles 120,000 cubic miles of water and transfers heat
percolation
precipitation
27
vapor transport10
groundwater flow
return flow10
precipitation
94
After Stowe
oceans hold340 M cubic miles
units - 1000 cubic miles/year
evaporation & transpiration
17 evaporation
104
Biochemical and
Geochemical Evolution
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photic zone(light)
aphotic zone(dark)
Sun
V B G Y O R IRUV
10% 50' 0' 300' 40' 15' 2'
solid Earth Ocean
atmosphere
where is the biosphere?
oceans and atmosphere scatter, absorb, and transfer
energy
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Thermohaline (temperature- and salinity-controlled density) circulation of the oceans can be simplistically defined by a great conveyor belt. In this model, warm, salty surface water is chilled and sinks in the North Atlantic to flow south towards Antarctica. There, it is cooled further to flow outward at the bottom of the oceans into the Atlantic, Indian, and Pacific basins. After upwelling primarily in the Pacific and Indian Oceans, the water returns as surface flow to the North Atlantic. While traveling deep in the ocean the originally nutrient-depleted water becomes increasingly enriched by organic matter decomposition in important nutrients (e.g., phosphate, nitrate, silicate) and dissolved CO2. Figure courtesy of Jim Kennett and Jeff Johnson, University of California Santa Barbara.
http://seis.natsci.csulb.edu/rbehl/ConvBelt.htm
ocean conveyor belt
deep
deep
shallow
Ocean currents distribute nutrients and moderate temperatures by transferring tropical heat to arctic
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blackbody radiation reduced by inverse square
distance
atmospheric absorption and scattering losses
reflection losses and refraction at air-sea surface
seawater absorption and scattering losses
horizontal receiving surface
stellar temperature
stellar radius
radius of planetary
orbit
wavelengths
polarizations
atmospheric composition: absorbers &
scatterers
flux above atmosphere
flux above sea surface
flux spectrum incident on horizontal surface
flux spectrum absorbed in last meter
flux spectrum scattered in last meter
flux reflected by air-sea interface
SolarSeaFlux Flow Chart
transmission angle
seawater composition: absorbers &
scatterers
incidence angle
seawater depth
©Bob Field 2003
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Temperatureof the atmosphere
ocean
10 km
sea level
Stratosphere
Troposphere has 75% of airdensity and temperature
decrease with altitudetemperaturevs. altitude
Sun
cool-70F
warm60F
ozone layer
After Tarbuck
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Average Global Energy Budget
50
100
20
30
incidentsunlight
absorb
scatteredsunlight
absorb
sea + land
atmosphere
Sun
30
30
evap
condense
90
65
155
absorb
radiate
radiate
5
110
105
radiate
absorb
radiated heatLWIR
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annual carbon cycle in the atmosphere
ocean
90
R
Ph
93
Ph
110109
R
+1
+3billions of tons of carbon
Sun
7
ff
-7
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where is the carbon?(billions of metric tons)
Sun
from Biology of plants 5th Ed. by Raven et al. page 115
sediments20,000,000
deep ocean38,000,000
carbon dioxide gasin atmosphere 700
Dissolved organic matter ~2000
humus2000 fossil fuels
5000?
dissolved gas 40,000
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Hea
ling
Gai
a by
Jam
es L
ovel
ock
p139
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BIO 200 Special Problems in Biological Sciences for lower division undergraduates
Joshua Yang - Carbon in the Geobiosphere
Tim Tappscott - Prokaryote Evolution
Raechel Harnoto – Astrobiology and Global Evolution
BIO 100 Orientation to Biological SciencesIntroduction to Biological Sciences faculty, department and campus resources, research opportunities, possible careers, studying science, and current topics in biology.
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convective zone
fusioncore
The Sun creates, stores, and radiates energy
radiative zone
zonevolume
~r3 masstotal
energy
fusion core r < ¼ 1/64 1/2 2/3
radiative r < 0.7 1/3 1/2 1/3
convective r > 0.7 2/3 1/80 1/100
The Sun evolves because fusion changes the composition of the core which changes density, temperature, and luminosity
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H Mass Fraction (X) vs. RadiusX=.70, Y=.28, Z=.02
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0E+00 2E+10 4E+10 6E+10 8E+10
Radius (cm)
X
ZAMS X
1.5 BY X
3 BY X
4.5 BY X
6 BY X
7.5 BY X
9 BY X
Guzik Field Lopez x70y28z02 112005
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Density (g/cm^3)
0
20
40
60
80
100
120
140
160
0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10
radius (cm)
Guzik - LANL solar evolution code
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Temperature (K)
00E+0
2E+6
4E+6
6E+6
8E+6
10E+6
12E+6
14E+6
16E+6
0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10
radius (cm)
Guzik - LANL solar evolution code
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Solar Evolution
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
0E+00 1E+09 2E+09 3E+09 4E+09Time (years)
Re
lati
ve
Va
lue
T/Tsun
R/Rsun
L/Lsun
cycle 17
L = 4πR2·σT4
Guzik + Field
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dhillon phy213 website
Equations of Stellar Structure
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relative volume
fusion core 16
radiative zone 343
convective zone 641
relative mass
fusion core 481radiative
zone 492
convective zone 27
relative heat flow
1000988
1000
0
200
400
600
800
1000
fusion core radiative zone convective zone
relative total energy
radiative zone 356
fusion core 637
convective zone 7
relative fusion power
convective zone 0
fusion core 988
radiative zone 12
Sun
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layers volume (cm3) mass (g)average density
(g/ cm3)
relative volume
relative mass
relative average density
fusion core 2.22E+31 9.57E+32 43.19 16 481 30784
radiative zone 4.86E+32 9.79E+32 2.01 343 492 1434
convective zone 9.10E+32 5.37E+31 0.06 641 27 42
whole Sun 1.42E+33 1.99E+33 1.40 1000 1000 1000
layerstotal
energy (ergs)
fusion power
(erg/ s)
luminosity (erg/ s)
relative total
energy
relative fusion power
relative heat flow
fusion core 1.95E+48 3.80E+33 3.80E+33 637 988 988
radiative zone 1.09E+48 4.62E+31 3.85E+33 356 12 1000
convective zone 2.00E+46 0.00E+00 3.85E+33 7 0 1000
whole Sun 3.06E+48 3.85E+33 3.85E+33 1000 1000 1000
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greatly simplified
H1 + H1 → H2 + e+ + υ
H2 + H1 → He3 + γ
nucleosynthesis: billion years or seconds?
e+ + e- → γ + γ
photons lose energy quickly
neutrino escapes from Sun
proton turns into neutron
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million years
He3 + He3 → He4 + H1 + H1
http://theory.uwinnipeg.ca/mod_tech/node209.html
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Electrical forces keep protons apartbecause like charges repel
CoulombBarrier
attr
acti
vere
pu
lsiv
e
YukawaAttractiveNuclearPotential
The rich get richer.If you can climb the rim,
you can drop in the craterand gain kinetic energy.
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1
2
Never gonna happen, my friend!
Proton needs 1000 times more thermal energy
than average
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1
2
Tunneling happens all the time!
Thermonuclear fusion generates energy to replace energy radiated into space,
but it takes energy to get started
How did the Sun get hot originally?
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As cold gases condense to form the Sun,
they get hot and lose energy
This stage lasts 100,000 years.The Sun was 1000 times brighter.
gravitational attraction
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Solar FormationHow did a cold dilute gas contract under gravitational attraction and produce a core hot enough and dense enough to sustain thermonuclear fusion?My simplified but detailed explanation of solar formation is more complete than most non-mathematical discussions.
1. Enormous molecular clouds resist gravitational contraction for billions of years with the help of kinetic energy, rotational energy, and magnetic fields until an external perturbation alters the properties of a portion of the cloud enough to trigger free fall contraction as gravitational attraction dominate other influences.
2. My simple explanation of solar formation will ignore rotation and magnetic effects and will assume the cloud is a cold dilute self-gravitating gas with uniform composition, density, and temperature and the mass of the Sun.
3. Gas particles in the cloud accelerate as they fall toward the center of mass because there is no hydrostatic support.
4. Gas density remains uniform as it increases because all particles have the same free fall time since velocity and acceleration increase linearly with radius since a = GM/r2 = G(4πρr/3).
5. Collisions in the center raise the temperature, internal energy, and pressure producing temperature and pressure gradients as the opacity increases.
6. The developing pressure gradient provides some hydrostatic support for the increasingly dense core gases.
7. Falling particles continue to compress the core, increasing its density, pressure, and temperature.
8. The differential pressure reduces the contraction near the center producing a density gradient.
9. Gas opacity initially increases with density and temperature, trapping radiant energy in the interior.
10. Surface cooling by radiative transport also increases the interior temperature gradient.
11. The high opacity of the interior maintains the increased temperature gradient.
12. A convection instability forms and convection transports trapped interior heat from the core to the surface.
13. At very high temperature, opacity decreases as bound electrons are freed.
14. The core density increases enough to fuse hydrogen nuclei.
15. Radiative energy transport replaces convective energy transport except for the outer gases.
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Solar EvolutionHow can the Sun grow brighter over time while the
core hydrogen abundance decreases?1. Energy generated by fusion replaces energy diffusing from the core to the surface.
2. Nucleosynthesis reduces the core hydrogen abundance and particle density.
3. Some core electrons are annihilated by positrons produced during nucleosynthesis.
4. Core opacity decreases as temperature rises and density of core electrons decrease.
5. The decrease in core particles does not decrease the local energy density or pressure.
6. The core temperature rises as the average energy per particle rises.
7. Decreases in core hydrogen abundance reduce protons available for fusion, but fusion rate increases
slightly due to the increased core temperature.
8. Luminosity increases as the temperature and temperature gradient increase and opacity decreases.
9. Increased luminosity increases energy density and pressure at larger radii.
10. Pressure increase expands envelope and forces more particles into core.
11. Core contraction maintains the pressure gradient required for hydrostatic support.
12. Gravitational contraction increases core density, pressure, temperature, and energy density.
13. Fusion rate increases with core density and temperature – enough to sustain higher luminosity.
14. Solar envelope expands as its temperature rises, increasing the surface radius and temperature.
15. The Sun’s luminosity increases as its surface radius and temperature grow over billions of years.
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Earth creates, stores, and radiates energy
ICB
CMB
inner core - conduction
outer core – convection?
lower mantle - convection
D” - conduction
upper mantle - convection
lithosphere - conduction
atmosphere - radiation
convection is powered by radiogenic heat sources and produces chemical evolution
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Radiogenic Heat Flow (W)
0000E+00
20E+12
40E+12
60E+12
80E+12
100E+12
120E+12
-5 -4 -3 -2 -1 0Time (BY)
Rad
iog
enic
Hea
t F
low
(W
)
Total
U-235
K-40
U-238
Th-232
Earth’s composition evolves as rare but critical elements decay
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Whole Earth, Crust, Mantle, Core Element Mass Percent
Fe85.5
O44
Si21
Mg22.8
Fe32.0
O29.7
Si16.1
Mg15.4
Ni5.2
Ca2.53
Al2.35
Fe6.26
Al8.41
Ca5.29
Fe7.07
O45.3Si
26.77
Mg3.2
Ni1.8
Ca1.7
Al1.6
Fe
O
Si
Mg
Ni
Ca
Al
S
Cr
Si6
Whole Earth CrustMantleCore
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models of growth of continental volume (%)
4 3 2 1 0BYA
100
75
50
25
0
1992
geo
chem
ical
Van Andel
linear re
ference
1992 geochemicalBYA: % 0: 100 0.6: 90 2.6: 10 3.6: 0 4.5: 0
from VanAndel Fig. 13.6
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Density (kg/m^3)
0
2000
4000
6000
8000
10000
12000
14000
0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6
radius (m)
Den
sity
(kg
/m^
3)
inner core R < 1221.5 km
outer core R < 3480 km
lower mantle R < 5701 km
D” R < 3630 km
upper mantle R < 6291 km
lithosphere R < 6371 km
ICB
CMB
Mantle
Core
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Temperature Evolution (K)
0
1000
2000
3000
4000
5000
6000
0E+00 1E+06 2E+06 3E+06 4E+06 5E+06 6E+06 7E+06Radius (m)
Te
mp
era
ture
(K
)
boundaries
4 BYA
2 BYA
0 BYA
assume temperature changes linearly with time
Mantle
Core
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total heat flow (W)
00E+0
5E+12
10E+12
15E+12
20E+12
25E+12
30E+12
35E+12
40E+12
45E+12
0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6
radius (m)
tota
l hea
t fl
ow
(W
)
boundaries
current total heat flow (W)
radiogenic heat flow (W)
current lost heat flow (W)
current ΔGBE heat flow (W)
latent heat flow (W)
CMB
Mantle
Core
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relative internal energy
lithosphere7
lower mantle537
upper mantle123
outer core315
inner core19
relative mass
lithosphere21
lower mantle492
upper mantle162
outer core308
inner core17
relative volume
lower mantle554
upper mantle246
outer core156
lithosphere37
inner core7
relative total heat sources
lithosphere191
lower mantle568
upper mantle192
outer core26
inner core23
relative heat flow
23 49
1000
809
617
0
200
400
600
800
1000
inner core outer core lowermantle
uppermantle
lithosphere
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Volume, Mass, Density, Energy, Heat, and Heat Flow
layersinternal
energy (J )
heat sources
(W)total heat flow (W)
relative internal energy
relative heat
sourcesrelative
heat flowinner core 3.15E+29 9.85E+11 9.85E+11 19 23 23outer core 5.35E+30 1.11E+12 2.10E+12 315 26 49lower mantle 9.12E+30 2.43E+13 2.64E+13 537 568 617upper mantle 2.09E+30 8.22E+12 3.46E+13 123 192 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000continental crustocean crust
layersvolume (m^3) mass (kg)
average density
(kg/ m^3)relative volume
relative mass
relative average density
inner core 7.63E+18 9.83E+22 1.29E+04 7 17 2348outer core 1.69E+20 1.83E+24 1.08E+04 156 308 1977lower mantle 6.00E+20 2.92E+24 4.87E+03 554 492 889upper mantle 2.67E+20 9.63E+23 3.61E+03 246 162 658lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000continental crustocean crust
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visibleradiation
optical absorption impedes energy flow
From where we sit, brighter than a
thousand suns briefly
transparentplanet
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thermalconduction
thermal scattering impedes energy flow 5000°F
2.5°F/mile or 0.001°F/foot
solidplanet
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thermalconvection
viscosity and density affect energy flow
moltenplanet
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C
H
O
H C
H
C
H O
C
H
H
OC
H
H O
H
H
O
C
H
H
O
C
H
H O C
H
H O
C
H
H O
C
H
H O
C
H
H O C
H
H O
6 CH2O+ energy+ catalyst
fructose is an isomer of glucose: table sugar forms by joining them
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G G G G G G G
G F
simple sugar building blocks combine to form carbohydrates
when water is squeezed out
table sugar
cellulose
H2O
H2O H2O H2O H2O H2O H2O
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C
H
H
O
C
H
H
O
C
H
H O
C
H
H
O
C
H
H
O
ribose is a building block of ATP, RNA..
C
H
H O C
H
H O
C
H
H O
C
H
H O
C
H
H O
5 CH2O+ energy+ catalyst
deoxyriboseribose
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H
N
N NCN
C HC
H
C
H
CHN
CH N
CH N
nucleic acids are building blocks for energy and information in ATP, RNA...
CH N
CH N CH N
5 HCN+ energy+ catalyst
adenine
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RPiPi Pi
Nucleotides are combinations of nucleic acids,
ribose sugar, and inorganic phosphate
A
PiPi Pi
RH2O
H2O
UGCT
D
triphosphates transport energy for transfer RNAs, membrane synthesis, and sugar synthesis.
monophosphates relay signals within a cell
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nucleotide building blocks combine to form RNA and DNA
when water is squeezed out
R
A
Pi R
U
Pi R
C
Pi R
A
Pi R
G
Pi
H2O H2O H2O H2O
C
H
H
O
C
H
H
O
C
H
H O
C
H
H
O
C
H
H
O
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OC
H
N
O
CH
H
H
H
CH N
amino acids are readily made fromsimple molecules by adding energy
C
H
H O
O
H
Hwater
formaldehyde
hydrogen cyanide
glycine
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OC
H
N
O
CH
H
H
H
CH N
amino acids are readily made fromsimple molecules by adding energy
C
R
H O
O
H
Hwater
“R”-aldehydehydrogen cyanide
genericamino acid
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OC SH N
amino acids are building blocks of proteins that function as enzymes and structures
OC
H
N
O
CH
H
H
H
C
OC
H
N
O
CH
H
H
H
H H
C
N
C
OC
H
N
O
CH H
H
H H
C
C
CC
CC
C
H
H
HH
HH
all 20 amino acids have the same backboneand all have H and OH on the ends
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A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G AA C UC C UG A UG C UC A GU G UC A AA U AC G CG U A
after Trefil and HazenThe Sciences:
An Integrated Approach
AlaHis Tyr Val Thr Val Arg Leu GlyH2O H2O
H2O H2O H2O H2O H2O H2O
some of the 20 amino acids are represented by more than one of
the 64 triplet codons
ribosomes synthesize proteins by translating mRNA to tRNAs that are attached to amino acids
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Catalysts are vital to many processes:Proteins help produce complex molecules
after Trefil and HazenThe Sciences:
An Integrated Approach
Modern cellular processes are highly regulated
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DNA+RNA+Protein WorldRNA+Protein World
RNA World
Peptide (PNA) World?Thioester World?
Clay World?
Which self-replicating molecules came first?
no record of early biochemistry
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Molecular and metabolic evolution may be relatively simple and rapid
Chance affects diversity and abundanceNecessity provides natural selection
All inheritable biological changes are based on molecular evolution
D
A
Pi D
T
Pi D
C
Pi D
A
Pi D
G
Pi
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mRNA provides the message to link amino acids into proteins
A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A
How does a computer “design” its own software?
AlaHis Tyr Val Thr Val Arg Leu Gly
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1
52 321
A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A
How does information evolve?
21 3 4
2 3
21 3
21 3
4 5
duplication
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4 5
1
52 321
A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A
How does information evolve?
21 3 4
2 321 3 21 3
deletion and insertion