Transcript Life on Our Evolving Planet slides

Life on Our Evolving Planet
optical physicist in aerospace for twenty years
designed and analyzed laser optical systems
Informal science educator in Morro Bay State Park
Museum of Natural History for ten years
5 global evolution walks in parks
12 animated slide shows in museum
3 poster exhibits in museum and at Cal Poly
Bob Field
Cal Poly adjunct physics professor for seven years
and research scholar in residence
4 senior projects Phys 461-464
8 summer student projects
13 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
What is a system?
a system has parts that interact
and may have emergent properties
Is the system open or closed?
energy
energy
matter
matter
Dr Art Sussman’s Guide to Planet Earth
energy flows, matter cycles, web of life
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
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?
Simple building blocks
evolve into complex systems
when energy flows
Everything Evolves
oceans and atmosphere
solid Earth and Sun
molecules and cells
organisms and ecosystems
Abundance in Universe in %0.07%
0.04%
1 1
Na Mg
11 23 12 24
0.02%
0.1%
0.01%
Periodic Table of
Chemical Elements
0.02% everything else
K Ca
Cr Mn Fe
Ni
19 39 20 40
24 62 25 55 26 56
28 59
Sun fuses 4
1
H
}
92%
H
~8%
He
2 4
C N O
Ne
6 12 7 14 8 16
10 20
Al Si P S Cl Ar
13 27 14 28 15 31 16 32 17 35 18 40
→
4
He
Sunlight is the waste product
Big stars build big atoms
composition in our LANL solar evolution code
sun
solar composition
"metals", 1
solar "metals" composition
Magnesium, 5.0
other, 1.3
Helium, 28
Nitrogen, 7.0
Hydrogen, 71
Carbon, 22.9
composition by mass
Oxygen, 63.9
Simple building blocks
ancient atmosphere ???
2CO2+CH4+NH3+4H2O
Sulfur, 1.3
Phosphorus, 0.3
Hydrogen, 7.8
Nitrogen, 5.2
Hydrogen, 7.8
Nitrogen, 7.3
Carbon, 16.6
Carbon, 18.7
Oxygen, 68.7
Oxygen, 66.3
comet volatiles composition
about 93% CHO by mass
Complex Systems
Phosphorus, 0.6
Calcium, 1.4
Sulfur, 0.6
Phosphorus, 0.6
Sulfur, 0.3
Hydrogen, 10.0
Nitrogen, 3.1
Nitrogen, 5.1
Hydrogen, 9.3
Carbon, 12.2
Carbon, 19.3
Oxygen, 63.6
mammal composition
Oxygen, 73.8
bacteria composition
about 97% CHO by mass
elemental composition of the ocean and the atmosphere
seawater
atmosphere
Sodium, 1.05
Chlorine, 1.9
Carbon, 0.0026
Argon, 1.1
other, 0.308
Hydrogen, 10.8
Hydrogen, 0.01
Oxygen, 20.9
Carbon, 0.01
Oxygen, 85.7
Nitrogen, 78
composition by mass
wikipedia
Elemental Composition of the Earth
whole Earth
Sulfur, 0.6
Aluminum, 1.6
Calcium, 1.7
Nickel, 1.8
Continental Crust
Chromium, 0.5
other, 0.5
other, 4
Aluminum, 8.41
Iron, 7.07
Calcium, 5.29
Magnesium, 15.4
Iron, 32
Silicon, 16.1
Magnesium, 3.2
Silicon, 26.77
Oxygen, 45.3
Oxygen, 29.7
composition by mass
McDonough
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
H
H
C
O
H
H
H
C
H
O H
H
H
C N
H
C
C
C
C
C
H
H
C
C
O
C
H
C
C
H
H
C
C
H
H
C
C
O H
C N
H
H
C
C
C N
N C N
H
N C
C N
H
C
H
Organic molecules have many variations on a few themes
S
fatty membrane spheres
form naturally in meteors
CO, H2, PO4 are building blocks of
phospholipids found in cell membranes
R
Pi
C
C
C
C
C
C
C
C
C
C
C
C
backbone of
phospholipid
(H and O not shown)
all cells are cells
descended
a common
ancestor
Modern
are from
chemical
factories
that store, exchange, and transform
What
do
cells
do?
matter, energy, and information
prokaryote
5 kingdoms:
bacteria
algae
fungus
plant
animal
energy
energy
matter
matter
eukaryote
C
H
O
Life’s Origin page 15
by Walter Schopf
A
Mammal
Hydrogen
Oxygen
Carbon
Nitrogen
A,Sulfur
B, and
Phosphorus
Calcium
2.4
C 0.13
are
0.13
0.23
S
N
B
Bacteria
P
C
Comet
What are
building
61 the 63
56
26
29
31
blocks10.5of molecules?
6.4
10
all
1.4
0.06
about
0.12
-
97%
composition by number of atoms
2.7
0.3
CHO
0.08
-
many common molecules
are made from CHONSP
C
O
C
O
H
H
O
N
S
P
atoms can share or transfer electrons
H–1
O O
H
O
He – 0
H O
P
O
N
N
H
O
OH– 2 O O
H
C–4
N–3
H
H S
H
O
N
C H
SO – 2 N
H
H
H
P – 3 or 5
O
C
S
Methane can form new molecules
O
methanol
methane
H
H
O
C
H
H
formaldehyde
formic acid
biochemists give
big names to
small molecules
glucose is a building block of carbohydrates
H
C
H
O
H O
H
H
C
O
H
glucose
O
O
C
H
H
C
O H
H
C
H
H
H
H
C
C
O
O
H
H
O
C
O
H
C
H
C
H
H
H
O
O
C
C
C
H
O
H
H
H
C
O
6 CH2O
+ energy
+ catalyst
H
C
H
O
photosynthesis makes glucose from
sunlight, carbon dioxide, and water
O
O
C
C
O
O
O
C
O
O
C
O
H
H O
H
O
C
C
O
O
6 O2
H
C
O H
Sunlight
O
H O
H
H
H
H O
H O
C
H
H
H
C
H
O
C
H O
H
H
C
C
O
O
H O
H O
H
H
H
H
6 CO2 glucose
O
6 H2O
glucose supplies energy to make ATP
H
H O
C3H3O3
H
C
O
H
O
C
O
C
O
C
H
H
H
glucose
C
H
C
O H
O
H
H
ATP
H
ATP
C
O ATP
H ATP
C
H
C
O
H
C
O
C
O
C
H
H
O
H
C3H3O3
aerobic fermentation makes 2 more ATP
respiration liberates energy by oxidizing
glucose into carbon dioxide and water
O
O
C
C
O
O
O
O
C
C
O
O
O
O
C
C
O
O
6 CO2
ATP ATPH ATP
O C ATP
H
ATP HATP
C ATP
O H
ATP ATP
H
H ATP
ATP ATP
C
H
ATP ATP
ATP
O
C
H
ATP ATP ATP
O
ATP ATPH ATP
ATP ATP ATP
ATP ATP ATP
ATP
ATP
ATPH
ATPC
H
ATP
O
C
ATP
O
ATP
H
ATP
ATP
H O
H O
H
H
H O
H O
H
H
H O
H O
H
H
6 H2O
 Bob Field 2000
low tide in Corallina Cove - Montana de Oro
Moon
Interactions
between
Earth systems
sun
impacts
when energy flows,
complexity grows
atmosphere
Condie33
Fig 1.33
biosphere
oceans
upper crust
lower crust
sediments
subcontinental
lithosphere
oceanic
crust
oceanic lithosphere
upper mantle
lower mantle
core
Solar and Global Evolution
are parts of Cosmic Evolution
generic system
galaxies
stars
planets
plants
animals
brains
society
table from Chaisson139
average power
density (W/kg)
0.00005
0.0002
0.01
0.1
2
15
50
when energy flows, complexity grows
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
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).
©Bob Field 2007
This is the dust cover of a book that I want to write.
I have been researching the subject for years.
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
Global Evolution: The First Five Billion Years
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? 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 System
Sun
Solid Earth
Hydrosphere
Atmosphere
Geobiosphere
Global Evolution Timelines
Molecules and Cells
Organisms and Ecosystems
Astronauts
Earth Systems Data Base
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
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.
Sun
vapor transport
10
precipitation
precipitation
27
evaporation & transpiration
17
Average Global Energy Budget
incident
sunlight
scattered
sunlight
100
30
65
5
94
evaporation
percolation
radiate
104
20
Hydrosphere
absorb
condense
105
30
radiate
oceans hold
340 M cubic miles
groundwater flow
155
absorb
return flow
10
units - 1000 cubic miles/year
radiated heat
LWIR
After Stowe
atmosphere
sea + land
50
90
110
30
absorb
absorb
radiate
evap
Atmosphere
Geobiosphere
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.
ribosomes synthesize proteins by translating
mRNA to tRNAs that are attached to amino acids
H 2O
H2O
H2O
H2O
H2O
H 2O
H2O
H2O
His Ala Tyr Val Thr Val Arg Leu Gly
GUA CGC AUA CAAUGUCAGGCUGAU CCU ACU
AUGCAUGCGUAUGUUACAGUCCGACUAGGAUGA
after Trefil and Hazen
The Sciences:
An Integrated Approach
Molecules and Cells
Organisms and Ecosystems
Astronauts
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?
The Natural History of Planet Earth Timeline:
Five Billion Years of Solar and Global Evolution
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now
PreHadean
Hadean
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0
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Archaean
-300
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ZAMS
100
200
300
400
500
600
700
800
900
1000
1100
1200
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4000
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4400
4500
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Era
Proterozoic
from to
MYA
MY MY
Phanerozoic
oceans
and
atmosphere
solid Earth
and
Sun
molecules
and
cells
organisms
and
ecosystems
Earth Systems Database: The Sun
These databases document the structures, functions, composition, interactions and flows of
energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
Solar Evolution
1.0
0.9
Relative Value
0.8
0.7
0.6
T/Tsun
0.5
R/Rsun
L/Lsun
0.4
cycle 17
0.3
0.2
0.1
0.0
0E+00
relative volume
2E+09
3E+09
Time (years)
relative mass
Sun
fusion core
16
relative heat flow
1000
988
1000
layers
convective
zone 27
radiative
zone 343
convective
zone 641
1E+09
fusion core
481
radiative
zone 492
1000
800
volume (cm3) mass (g)
4E+09
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
600
relative total energy
400
relative fusion power
200
convective
zone 7
radiative
zone 12
0
fusion core
radiative zone
convective
zone 0
convective zone
radiative
zone 356
fusion core
637
fusion core
988
layers
total
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
Earth Systems Database: The Solid Earth
These databases document the structures, functions, composition, interactions and flows of energy
and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
models of growth of continental volume (%)
Radiogenic Heat Flow (W)
100
Radiogenic Heat Flow (W)
120E+12
100E+12
75
Total
U-235
80E+12
K-40
U-238
60E+12
50
Th-232
40E+12
25
20E+12
0000E+00
-5
-4
-3
-2
Time (BY)
-1
relative volume
upper mantle
162
relative heat flow
outer core
308
lower mantle
492
1000
1000
800
809
relative internal energy
inner core
19
lithosphere
7
upper mantle
123
600
400
200
23
49
outer core
0
outer core
315
lower
mantle
Va
ce
ren
e
f
al
e
ic
rr
a
m
e
e
lin
ch
o
ge
2
9
19
from VanAndel Fig. 13.6
4
3
layers
inner core
outer core
lower mantle
upper mantle
lithosphere
whole Earth
continental crust
ocean crust
volume
(m^3)
7.63E+18
1.69E+20
6.00E+20
2.67E+20
4.03E+19
1.08E+21
internal
volume
energy
(m^3) (J)
3.15E+29
1.77E+20
5.35E+30
8.66E+20
9.12E+30
4.03E+19
2.09E+30
1.08E+21
1.20E+29
1.70E+31
2
BYA
1
mass (kg)
9.83E+22
1.83E+24
2.92E+24
9.63E+23
1.25E+23
5.94E+24
average
density
(kg/m^3)
1.29E+04
1.08E+04
4.87E+03
3.61E+03
3.11E+03
5.48E+03
relative
volume
7
156
554
246
37
1000
heat
sources
(W)
mass
(kg)
9.85E+11
1.93E+24
1.11E+12
3.88E+24
2.43E+13
1.25E+23
8.22E+12
5.94E+24
8.17E+12
4.28E+13
average
total
heat
density
flow (W)
(kg/m^3)
9.85E+11
1.19E+04
2.10E+12
4.24E+03
2.64E+13
3.11E+03
3.46E+13
5.48E+03
4.28E+13
4.28E+13
relative
internal
relative
energy
volume
19
163
315
800
537
37
123
1000
7
1000
0
relative
mass
17
308
492
162
21
1000
relative
average
density
2348
1977
889
658
567
1000
relative total heat sources
617
inner core
l
n de
A
n
0
relative mass
upper mantle
246
lower mantle
554
0
inner core
lithosphere 17
21
inner core
lithosphere7
37
outer core
156
upper
mantle
lithosphere
inner core
23
outer core
26
lithosphere
191
upper mantle
192
lower mantle
537
1992 geochemical
BYA: %
0: 100
0.6: 90
2.6: 10
3.6: 0
4.5: 0
lower mantle
568
layers
layers
inner core
core
outer core
mantle
lower mantle
lithosphere
upper Earth
mantle
whole
lithosphere
whole Earth
continental crust
ocean crust
relative
relative
heat
relative
relative
average
sources
flow
mass heat
density
23
23
325
2162
26
49
654
773
568
617
21
567
192
809
1000
1000
191
1000
1000
1000
Earth Systems Database: The Hydrosphere
These 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
500
97.25
1
stored water
2.05
0.68
0.1
0.01
0.01
0.001
434
400
398
water flux
300
0.005
wikipedia
0.001
0.0001
0.0001
0.00004
Biosphere
10
Streams &
rivers
100
average rate (10³ km³/year)
Atmosphere
Soil
moisture
Lakes
Groundwater
Ice caps &
glaciers
Oceans
0.00001
200
100
71
36
0
wikipedia
reservoir
107
Precipitation
over land
Evaporation
from land
Runoff &
groundwater
from land
Precipitation
over oceans
Evaporation
from oceans
transmission vs. depth
transmitted sunlight in pure water vs. depth
Field - solar sea flux code
(0, 1, 3, 10, 30, 100 meters)
350
max
300
Field - solar sea flux code
pure
250
0.8
particulate
200
DOM
chlorophyll
150
0.6
Tz      z k  0 
Hy (  )
100
0.4
50
0.2
0
0
1
3
10
depth (m)
30
100
0
0
30 0
1
35 0
40 0
45 0
50 0
55 0
  Hx(  )
60 0
65 0
70 0
75 0
80 0
2
Earth Systems Database: The Atmosphere
These databases document the structures, functions, composition, interactions and flows of energy
and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
cloudfree sky
Sun
Average Global Energy Budget
Average Flux for Clean, Dry Air at 35 N
Field - solar flux code
500
incident
sunlight
scattered
sunlight
100
30
Scattering Losses
Flux (W/m^2)
400
radiated heat
LWIR
65
5
Absorption Losses
Flux at Surface
300
radiate
200
condense
105
30
absorb
100
radiate
0
atmosphere
Total
UV
0.3-3.0
0.12
155
20
absorb
Visible
Infrared
0.3-0.4
0.4-0.7
Spectral Band (microns)
sea + land
0.7-3.0
50
90
110
30
absorb
absorb
radiate
evap
Summer Solstice
Thermal Structure of Troposphere
Solar Flux vs. Time of Day
0.1
Equator
downwelling temperature (K)
Tropic
of
Cancer
upwelling temperature (K)
10
9
8
altitude (km)
0.08
Arctic Circle
0.06
North Pole
0.04
7
6
5
Salby237
4
3
2
0.02
1
0
0
24
2
Midnight
4
6
6 am
8
10
12
Noon
14
16
18
6 pm
20
22
24
Midnight
210
220
230
240
250
260
270
280
Temperature (K)
290
300
310
320
Earth Systems Database: The Biosphere
These databases document the structures, functions, composition, interactions and flows of energy
and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.
Phosphorus, 0.6
Calcium, 1.4
Sulfur, 0.6
carbon (Gt) on a logarithmic scale
Phosphorus, 0.6
Sulfur, 0.3
Hydrogen, 10.0
Nitrogen, 3.1
1E+9
Nitrogen, 5.1
1E+8
Hydrogen, 9.3
1E+7
Carbon, 12.2
1E+6
1E+5
Carbon, 19.3
1E+4
1E+3
Oxygen, 63.6
Oxygen, 73.8
1E+2
1E+1
bacteria composition
CO
2
iss
D
(a
tp
re
-in
du
mammal composition
A
str tm
ia osp
l2 h
80 er
o
pp e
D lved
iss
m
i
n
v
Pa olve org Oc )
rti d an ea
cu or ic n
la ga (D
te ni
or c ( IC)
ga D
ni OC
c
O (PO )
ce
an C)
La bio
nd ta
Ba P bi
ct hy ota
er to
ia m
a a
La nd ss
nd fun
A gi
R
ni
D ea
m
ea ct
al
d
s
or ive
ga fra So Lan
ni ct il
c m io hu d
n
m
In
or atte of us
ga r , hu
ni lit m
c s te us
oi r, p
l( e
Ca at
C
O arb
rg
S CO
o
an na ed 3)
ic te im
m se en
at di ts
te
m
Co r s en
nt edi ts
in m
en en
O tal ts
ce cr
a
u
U nic st
pp cr
er us
m t
an
tle
1E+0
Flux
Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et al
in Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003
gross primary production
from atmosphere to land biota
from ocean to ocean biota
respiration
from land biota to atmosphere
from ocean biota to ocean
Net primary production (NPP)
from atmosphere to land biota
from ocean to ocean biota
Volatilization from soil organic matter to atmosphere
Net exchange from atmosphere to land
Weathering consumption of CO2 from atmosphere to sediments
Net exchange to atmosphere from ocean
dissolution from atmosphere to ocean
evasion to atmosphere from ocean
River input of dissolved C (DIC + DOC) to ocean
DIC
DOC
POC
PIC
Oceanic sediment long-term storage
Carbonates
Organic matter
Volcanism, metamorphism, hydrothermal from land to atmosphere
Uplift
Carbon
Gt/year
203
110
93
89.5
46.9
42.6
113.5
63.1
50.4
62.5
0.6
0.26
0.51
96
96.51
0.6
0.38
0.22
0.19
0.18
0.28
0.22
0.06
0.22
0.4
http://geology.wr.usgs.gov/parks/gtime/Gtimescale.pdf
4 MY
4 BY
Time MYA
4
Event
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
0.3
Homo erectus tames fire
Geminga 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
0.04-0.012
Homo 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
Time MYA
Event
4600
Formation of the approximately homogeneous solid Earth by planetesimal accretion
4300
Melting 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
4300
Atmospheric 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
3500-2800
Beginning 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
2400
Rise 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
1600
The 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
The Natural History of Planet Earth Timeline:
Five Billion Years of Solar and Global Evolution
-4900
-4800
-4700
-4600
-4500
-4400
-4300
-4200
-4100
-4000
-3900
-3800
-3700
-3600
-3500
-3400
-3300
-3200
-3100
-3000
-2900
-2800
-2700
-2600
-2500
-2400
-2300
-2200
-2100
-2000
-1900
-1800
-1700
-1600
-1500
-1400
-1300
-1200
-1100
-1000
-900
-800
-700
-600
-500
-400
-300
-200
-100
now
oceans
and
atmosphere
solid Earth
and
Sun
molecules
and
cells
PreHadean
Hadean
-200
-100
0
100
200
300
400
500
600
700
800
900
1000
1100
1200
1300
1400
1500
1600
1700
1800
1900
2000
2100
2200
2300
2400
2500
2600
2700
2800
2900
3000
3100
3200
3300
3400
3500
3600
3700
3800
3900
4000
4100
4200
4300
4400
4500
4600
4700
Archaean
-300
-200
-100
ZAMS
100
200
300
400
500
600
700
800
900
1000
1100
1200
1300
1400
1500
1600
1700
1800
1900
2000
2100
2200
2300
2400
2500
2600
2700
2800
2900
3000
3100
3200
3300
3400
3500
3600
3700
3800
3900
4000
4100
4200
4300
4400
4500
4600
Era
Proterozoic
from to
MYA
MY MY
Phanerozoic
Name ten or more
globally important events
in any column.
Think about the W5H:
who
what
when
where
why
how
Emphasis on
connections not collections
organisms
and
ecosystems
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 Evolution
Identify 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 Evolution
Study 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 Evolution
Study biochemical, geochemical, and/or biogeochemical properties and processes
from cellular to global scales in Hadean, Archaean, Proterozoic, and/or
Phanerozoic Eras.
Prokaryote
and
Eukaryote
Evolution
http://en.wikipedia.org/wiki/Bacterium
Identify and describe node organisms and characters
1458 Fungi 1351 Animals
Provide common names for each label
1513 Fungimal
Enter data into my 5 BY timeline
1609 Algfungimal
Investigate environmental and ecological causes
1558 Algae
Examine environmental and ecological impacts
2100? Respirators
Describe ecosystems prevalent in each era
2309 Eukaryotes
3096 Chlorobium
2923 Fusobacterium
2800 Proteobacteria
2688 Firmicutes
Cyanobacteria
3644 Thermotoga
3977 Aquifex
Evaluate accuracy of molecular timescales
4112 Archaea
Create separate charts for each geologic era
Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et al
in Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003
precipitation
Biochemical
and
Geochemical
Evolution
vapor transport
10
precipitation
27
evaporation & transpiration
17
94
evaporation
percolation
104
return flow
10
oceans hold
340 M cubic miles
units - 1000 cubic miles/year
groundwater flow
After Stowe
global average of 40 inches of precipitation per year
recycles 120,000 cubic miles of water and transfers heat
Sun
10%
50'
0' 300'
40'
15'
2'
atmosphere
UV V B G Y O R IR
photic zone
(light)
solid Earth
oceans and atmosphere scatter,
absorb, and transfer energy
where is the biosphere?
Ocean
aphotic zone
(dark)
ocean conveyor belt
http://seis.natsci.csulb.edu/rbehl/ConvBelt.htm
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 nutrientdepleted 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.
Ocean currents distribute nutrients and moderate
temperatures by transferring tropical heat to arctic
stellar
temperature
SolarSeaFlux Flow Chart
©Bob Field 2003
stellar radius
blackbody radiation reduced
by inverse square distance
flux above
atmosphere
radius of
planetary
orbit
atmospheric absorption and
scattering losses
flux above sea
surface
wavelengths
atmospheric
composition:
absorbers &
scatterers
reflection losses and
refraction at air-sea surface
incidence
angle
seawater absorption and
scattering losses
polarizations
seawater
composition:
absorbers &
scatterers
seawater
depth
horizontal receiving surface
flux reflected by
air-sea interface
transmission
angle
flux spectrum incident
on horizontal surface
flux spectrum
absorbed in last meter
flux spectrum
scattered in last meter
f
Sun
Stratosphere
ozone layerTemperature
of the atmosphere
cool
-70F
temperature
vs. altitude
10 km
Troposphere has 75% of air
density and temperature
decrease with altitude
warm
60F
sea level
ocean
After Tarbuck
Sun
Average Global Energy Budget
incident
sunlight
scattered
sunlight
100
30
radiated heat
LWIR
65
5
radiate
20
155
absorb
condense
105
30
absorb
radiate
atmosphere
sea + land
50
90
110
30
absorb
absorb
radiate
evap
Sun
annual carbon cycle in the atmosphere
Ph
109
7
R
ff
110
Ph
90
93
+1
-7
R
ocean
billions of tons of carbon
+3
where is the carbon?
(billions of metric tons)
Sun
carbon dioxide gas
in atmosphere 700
humus
2000
dissolved gas 40,000
fossil fuels
5000?
sediments
20,000,000
from Biology of plants 5th Ed. by Raven et al. page 115
Dissolved organic
matter ~2000
deep ocean
38,000,000
Healing Gaia by James Lovelock p139
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 Sciences
Introduction to Biological Sciences faculty, department and campus resources, research
opportunities, possible careers, studying science, and current topics in biology.
The Sun creates, stores, and radiates energy
zone
fusion core r < ¼
radiative
volume
~r3
1/64
total
mass
energy
1/2
2/3
r < 0.7
1/3
1/2
1/3
convective r > 0.7
2/3
1/80
1/100
fusion
core
The Sun evolves
becausezone
fusion changes the
radiative
composition of the core which changes
density, temperature, and luminosity
convective zone
H Mass Fraction (X) vs. Radius
X=.70, Y=.28, Z=.02
0.7
0.6
ZAMS X
0.5
X
1.5 BY X
0.4
3 BY X
0.3
6 BY X
4.5 BY X
7.5 BY X
0.2
9 BY X
0.1
0.0
0E+00
2E+10
4E+10
6E+10
8E+10
Radius (cm)
Guzik Field Lopez x70y28z02 112005
Density (g/cm^3)
160
140
120
100
80
60
40
20
0
0E+00
1E+10
2E+10
3E+10
4E+10
5E+10
6E+10
7E+10
radius (cm)
Guzik - LANL solar evolution code
Temperature (K)
16E+6
14E+6
12E+6
10E+6
8E+6
6E+6
4E+6
2E+6
00E+0
0E+00
1E+10
2E+10
3E+10
4E+10
5E+10
6E+10
7E+10
radius (cm)
Guzik - LANL solar evolution code
Solar Evolution
1.0
0.9
Relative Value
0.8
0.7
0.6
0.5
L=
4πR2·σT4
T/Tsun
R/Rsun
L/Lsun
0.4
cycle 17
0.3
0.2
0.1
0.0
0E+00
1E+09
2E+09
3E+09
Time (years)
4E+09
Guzik + Field
Equations of Stellar Structure
dhillon phy213 website
relative volume
relative mass
Sun
fusion core
16
convective
zone 27
radiative
zone 343
relative heat flow
convective
zone 641
1000
988
1000
fusion core
481
radiative
zone 492
1000
800
600
relative total energy
400
relative fusion power
200
convective
zone 7
radiative
zone 12
0
fusion core
radiative zone
convective
zone 0
convective zone
radiative
zone 356
fusion core
637
fusion core
988
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
layers
total
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
nucleosynthesis: billion years or seconds?
H1 + H1 → H2 + e+ + υ
H2 + H1 → He3 + γ
proton turns
into neutron
e+ + e- → γ + γ
photons lose
energy quickly
neutrino escapes
from Sun
greatly simplified
He3 + He3 → He4 + H1 + H1
million years
http://theory.uwinnipeg.ca/mod_tech/node209.html
attractive
repulsive
Electrical forces keep protons apart
because like charges repel
Coulomb
Barrier
Yukawa
Attractive
Nuclear
Potential
The rich get richer.
If you can climb the rim,
you can drop in the crater
and gain kinetic energy.
Never gonna happen, my friend!
1
2
Proton needs 1000 times
more thermal energy
than average
Tunneling happens all the time!
How did the Sun get hot originally?
1
2
Thermonuclear fusion generates energy
to replace energy radiated into space,
but it takes energy to get started
As cold gases condense to form the Sun,
they get hot and lose energy
gravitational attraction
This stage lasts 100,000 years.
The Sun was 1000 times brighter.
Solar Formation
How 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.
Solar Evolution
How 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.
Earth creates, stores, and radiates energy
atmosphere - radiation
lithosphere - conduction
upper mantle - convection
lower mantle - convection
D” - conduction
outer core – convection?
inner core - conduction
ICB
convection is powered by
radiogenic heat sources and
produces chemical evolution
CMB
Radiogenic Heat Flow (W)
Earth’s composition evolves as
rare but critical elements decay
Radiogenic Heat Flow (W)
120E+12
100E+12
Total
U-235
80E+12
K-40
U-238
60E+12
Th-232
40E+12
20E+12
0000E+00
-5
-4
-2
-3
Time (BY)
-1
0
Whole Earth, Crust, Mantle, Core Element Mass Percent
Mg
15.4
Mg
3.2
Whole Earth
Crust
Mantle
Core
CaAl
Ni
1.6
1.7
1.8
Al
8.41
Ca
5.29
Ca
2.53
Mg
22.8
Si
16.1
Si
26.77
Si
21
Fe
Fe
7.07
O
Fe
32.0
Al Fe
2.35 6.26
Si
Mg
Ni
5.2
Ni
Si
6
Ca
Fe
85.5
O
44
Al
O
45.3
O
29.7
S
Cr
models of growth of continental volume (%)
100
75
50
1992 geochemical
BYA: %
0: 100
0.6: 90
2.6: 10
3.6: 0
4.5: 0
25
0
4
3
2
BYA
1
0
from VanAndel Fig. 13.6
Density (kg/m^3)
14000
Core
Density (kg/m^3)
12000
10000
ICB
8000
CMB
lithosphere
R < 6371 km
upper mantle
R < 6291 km
lower mantle
R < 5701 km
D”
R < 3630 km
outer core
R < 3480 km
inner core
R < 1221.5 km
6000
4000
Mantle
2000
0
0E+0
1E+6
2E+6
3E+6
4E+6
radius (m)
5E+6
6E+6
7E+6
Temperature Evolution (K)
assume temperature changes linearly with time
6000
Core
Temperature (K)
5000
Mantle
4000
3000
boundaries
4 BYA
2 BYA
0 BYA
2000
1000
0
0E+00
1E+06
2E+06
4E+06
3E+06
Radius (m)
5E+06
6E+06
7E+06
total heat flow (W)
45E+12
total heat flow (W)
40E+12
Mantle
boundaries
35E+12
current total heat flow (W)
30E+12
radiogenic heat flow (W)
25E+12
current lost heat flow (W)
20E+12
current ΔGBE heat flow (W)
latent heat flow (W)
15E+12
10E+12
Core
5E+12
00E+0
0E+0
1E+6
2E+6
CMB
3E+6
4E+6
radius (m)
5E+6
6E+6
7E+6
relative volume
relative mass
inner core
lithosphere 17
21
inner core
lithosphere7
37
outer core
156
upper mantle
162
upper mantle
246
relative heat flow
lower mantle
554
outer core
308
lower mantle
492
1000
1000
800
809
relative internal energy
inner core
19
lithosphere
7
upper mantle
123
600
relative total heat sources
617
400
200
23
49
inner core
outer core
0
outer core
315
lower
mantle
upper
mantle
lithosphere
inner core
23
outer core
26
lithosphere
191
upper mantle
192
lower mantle
537
lower mantle
568
Volume, Mass, Density, Energy, Heat, and Heat Flow
layers
inner core
outer core
lower mantle
upper mantle
lithosphere
whole Earth
continental crust
ocean crust
layers
layers
inner core
core
outer core
mantle
lower mantle
lithosphere
upper Earth
mantle
whole
lithosphere
whole Earth
continental crust
ocean crust
volume
(m^3)
7.63E+18
1.69E+20
6.00E+20
2.67E+20
4.03E+19
1.08E+21
mass (kg)
9.83E+22
1.83E+24
2.92E+24
9.63E+23
1.25E+23
5.94E+24
average
density
(kg/m^3)
1.29E+04
1.08E+04
4.87E+03
3.61E+03
3.11E+03
5.48E+03
internal
volume
energy
(m^3) (J)
3.15E+29
1.77E+20
5.35E+30
8.66E+20
9.12E+30
4.03E+19
2.09E+30
1.08E+21
1.20E+29
1.70E+31
heat
sources
(W)
mass
(kg)
9.85E+11
1.93E+24
1.11E+12
3.88E+24
2.43E+13
1.25E+23
8.22E+12
5.94E+24
8.17E+12
4.28E+13
average
total
heat
density
flow (W)
(kg/m^3)
9.85E+11
1.19E+04
2.10E+12
4.24E+03
2.64E+13
3.11E+03
3.46E+13
5.48E+03
4.28E+13
4.28E+13
relative
volume
7
156
554
246
37
1000
relative
internal
relative
energy
volume
19
163
315
800
537
37
123
1000
7
1000
relative
mass
17
308
492
162
21
1000
relative
average
density
2348
1977
889
658
567
1000
relative
relative
heat
relative
relative
average
sources
heat
flow
mass
density
23
23
325
2162
26
49
654
773
568
617
21
567
192
809
1000
1000
191
1000
1000
1000
transparent
planet
visible
radiation
From where we sit,
brighter than a
thousand suns briefly
optical absorption
impedes energy flow
solid
planet
thermal
conduction
thermal scattering
impedes energy flow
5000°F
2.5°F/mile or
0.001°F/foot
molten
planet
thermal
convection
viscosity and density
affect energy flow
fructose is an isomer of glucose:
table sugar forms by joining them
H
C
H
O
C
O
H
H
H
H
H
H
C
O
O
C
H O
C
H
H
O
H
C
H
H
C
C
O
O
H
H
H
H
C
C
H
O
O
H
H
H
C
O
H
6 CH2O
+ energy
+ catalyst
C
H
O
table sugar
H2O
G
F
cellulose
G
H2O
G
H2O
G
H2O
G
H2O
G
H2O
G
H 2O
G
simple sugar building blocks
combine to form carbohydrates
when water is squeezed out
ribose is a building block of ATP, RNA..
H
C
ribose
deoxyribose
O
H
H
H
C
H
C
H
O
H
H
H
C
H
5 CH2O
+ energy
+ catalyst
C
C
O
O
H
H
H O
C
H
H
O
C
C
H
O
O
H
H
O
H
C
H
O
nucleic acids are building blocks for
energy and information in ATP, RNA...
H
C N
H
C N
5 HCN
+ energy
+ catalyst
H
H
C N
H
C
N
C
C
N C
H
N H
N
N
C
H
adenine
H
C N
H
C N
Nucleotides are combinations of nucleic acids,
ribose sugar, and inorganic phosphate
H2O
R
D
Pi
Pi
R
Pi
monophosphates
relay signals
within a cell
H2O
U
G
C
T
A
Pi
Pi
Pi
triphosphates transport energy for transfer RNAs,
membrane synthesis, and sugar synthesis.
R
A
Pi
H2O
H2O
Pi
R
Pi
R
U
H2O
R
C
A
Pi
H2O
R
Pi
G
nucleotide building blocks
combine to form RNA and DNA
when water is squeezed out
H
H O
C
H
O
H
C
C
H
H
H
O
C
C
H
O
O
H
H
amino acids are readily made from
simple molecules by adding energy
H O
water
glycine
H
H
H
O
H N
C
C
O
H
H
H
C
O
H
H
C N
formaldehyde
hydrogen cyanide
amino acids are readily made from
simple molecules by adding energy
H O
water
generic H
amino acid
H
H
H
O
N
C
C
H
O
H
H
C
O
R
H
C N
hydrogen cyanide
“R”-aldehyde
amino acids are building blocks of proteins
that function as enzymes and structures
H
H
O
H N
C
C
O
H
H
O
H N
C
C
H
C
H
H
H
H
H
H
H
C
C
C C
O
H N
C
C
H
C
H
O
H
H
C
C
C
N
O
H
H
C
H
H
H
all 20 amino acids have the same backbone
C H O N S
and all have H and OH on the ends
ribosomes synthesize proteins by translating
mRNA to tRNAs that are attached to amino acids
H2O
H2O
H2O
H2O
H2O
H2O
H2O
H2O
His Ala Tyr Val Thr Val Arg Leu Gly
some of the 20 amino acids are
represented by more than one of
the 64 triplet codons
G U A C G C A U A C AA U G U C A G G C U G A U C C U A C
U G CAU GC GUAU GU UACAGU C C GAC UAG GAU GA
after Trefil and Hazen
The Sciences:
An Integrated Approach
Catalysts are vital to many processes:
Proteins help produce complex molecules
Modern cellular processes
are highly regulated
after Trefil and Hazen
The Sciences:
An Integrated Approach
Which self-replicating
molecules came first?
DNA+RNA+Protein World
RNA+Protein World
RNA World
no record of early biochemistry
Peptide (PNA) World?
Thioester World?
Clay World?
Molecular and metabolic evolution
may be relatively simple and rapid
Chance affects diversity and abundance
Necessity 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
mRNA provides the message to
link amino acids into proteins
His Ala Tyr Val Thr Val Arg Leu Gly
How does a computer
“design” its own software?
U G CAU GC GUAU GU UACAGU C C GAC UAG GAU GA
How does information evolve?
U G CAU GC GUAU GU UACAGU C C GAC UAG GAU GA
1
2
3
4
1
2
2
3
5
duplication
4
1
2
3
1
2
3
1
2
3
5
How does information evolve?
U G CAU GC GUAU GU UACAGU C C GAC UAG GAU GA
1
2
3
4
1
2
2
3
5
deletion and insertion
1
4
2
3
1
2
3
1
2
3
5