rfield website
Global Evolution Timeline
Global models and database
The Sun and Solid Earth
Atmosphere and Oceans
Organisms and Ecosystems
Molecules and Cells
© Bob Field 2007
1. Develop a global evolution website that features a
five billion year timeline of the natural history of
planet Earth.
2. Develop global models and a database of system
properties and processes for the OASES and the
biosphere.
3. Develop exhibits, indoor and outdoor informal
science education programs, and academic courses.
4. Organize global evolution study groups to develop
the global evolution timeline, database, and models.
1. Global Evolution Website: The GEEP shall develop and maintain a website for use by middle school to
graduate school students and educators and professionals as well as the general public. The website will highlight the
nearly five billion year natural history of planet Earth timeline of globally important physical and biological events. The
website will apply Dr. Sam Ham’s principles of thematic interpretation to the greatest story rarely told: the remarkable
four billion year sequence of events that preceded the Cambrian Explosion. The website will also include major elements
of the global evolution models and other educational resources described below.
2. Global Evolution Models and Database: The GEEP will develop a time dependent preliminary global
evolution model (PGEM) based on these events and a database of system properties and processes. The model will
characterize the evolving structure and energy flow of the oceans, atmosphere, solid Earth, Sun, molecules, cells,
organisms, and ecosystems in nominal 100 million year time intervals. The model will include surface processes as well
as deep terrestrial and non-terrestrial sources of energy and materials. This effort emphasizes secondary research and
heuristic models that have educational value. The global evolution website shall include a user-friendly database of
system properties and processes that clarify the interactions of energy and matter based on the PGEM.
3. Educational resources and programs: The GEEP shall develop, conduct, and evaluate academic courses
and projects and informal science educational programs. The programs will be based on the natural history timeline and
global evolution models described above. The projects may be held in indoor and/or outdoor venues and may include
nature walks and talks as well as virtual, permanent, temporary, and traveling exhibits for museums, nature venues,
schools, and libraries. The programs will also be based on the principles of thematic interpretation and may emphasize
the origins and relationships between physical and biological systems. They may examine the impact of global change on
the natural history of the California Coast as a lead-in to the five billion year natural history timeline. The interpretation
should be geocentric not anthropocentric and emphasize deep time not current human issues, although the latter may be
used to generate interest and improve understanding.
4. Global Evolution Study Group: The GEEP shall organize an informal cross-disciplinary Global Evolution
Study Group under the direction of the professor of global evolution studies. The group will identify and sequence the
major globally important physical and biological events in the nearly five billion year natural history of planet Earth. The
group will develop a time dependent preliminary global evolution model (PGEM) based on these events and the
underlying system properties and processes. The group will address the standard W5H questions (who what when where
why and how) in plain English.
DR. BOB FIELD
Adjunct Physics Professor
Research Scholar in Residence
I develop and supervise natural science
projects for students in physics, physical
science, chemistry, biology, math, K-16 and
environmental education. My number one
interest is Global Evolution Studies. I also
develop natural history programs primarily
for the local state parks and the Morro Bay
State Park Museum of Natural History. I
have a brief biographical sketch. Contact me
at rfield at my calpoly.edu email address.
My extensive website has three parts:
NATURAL
SCIENCE
GLOBAL
EVOLUTION
NATURAL
HISTORY
drbobfield bobfield64
The only good is knowledge and the only evil is ignorance (Socrates)
Return to Physics Department Home Page
GLOBAL EVOLUTION STUDIES
The National Academy of Science says that it is the role of science is to provide plausible natural explanations of
natural phenomena. The Natural History of Planet Earth is the product of nearly five billion years of global
evolutionary processes that followed the first nine billion years of cosmic evolution. Complexity grows when energy
flows in natural systems because simple building blocks evolve into complex materials and processes. The structure
and evolution of the OASES (oceans, atmosphere, solid Earth, and Sun) and the biosphere (molecules, cells,
organisms, and ecosystems) depend on interactions of energy and matter. The origin, evolution, diversity, abundance,
and distribution of life are emergent properties of increasing environmental complexity.
I am developing indoor and outdoor science education programs for youth
and for the adults that influence them by applying Dr. Sam Ham’s
principles of thematic interpretation to the greatest story rarely told: the
remarkable four billion year sequence of globally important physical and
biological events and processes that preceded the Cambrian Explosion. My
goal is to secure an endowment for an organization to develop and
maintain a global evolution website and related educational resources.
Students, volunteers, educators, and other professionals can help by
participating in and evaluating the intellectual merit and potential audience
impact of the following projects:
Global Evolution Endowment
NHOPE Timeline.xls
PGEM Events.doc
PGEM Database.ppt
OASESMCOE.doc
NHOPE ISE project proposal
1. Develop a global evolution website that features a five billion year timeline of the natural history of planet Earth.
2. Develop global models and a database of system properties and processes for the OASES and the biosphere.
3. Develop exhibits, indoor and outdoor informal science education programs, and academic courses.
4. Organize global evolution study groups to develop the global evolution timeline, database, and models.
go to natural science projects, natural history programs, globalevolution, or rfield home page
Global Evolution
© Mike Baird
Sun
impact
atmosphere
biosphere
oceans
upper crust
lower crust
sediments
Natural History of the California Coast
Natural History of Planet Earth
subcontinental
lithosphere
oceanic
crust
oceanic lithosphere
upper mantle
click on any figure
lower mantle
core
Solar and Global Evolution Models
How do global changes
impact the California coast?
The Natural History of the California Coast poster
exhibition planned for the summer of 2009 may be seen by
90,000 visitors to the Hearst Castle National Geographic
Theater lobby. It illustrates the impact of global evolutionary
processes by relating local natural history to global natural
systems themes from Dr. Art Sussman’s Guide to Planet
Earth using Dr. Sam Ham’s principles of thematic
interpretation.
Plausible Natural History publications
birds, marine mammals, Monarch Butterflies, tide pools,
kelp forests, coral reefs, lichen, algae, fungus, trees,
wildflowers, mountains, molecules, cells, Planet Earth,
The Facts of Life: From the Oceans to the Stars, etc.
Living Natural History programs
Montana de Oro State Park, Museum of Natural History,
Pismo State Beach, Elfin Forest, Morro Bay Estuary, Oso
Flaco State Park, Lopez Lake, Big Sur, Point Lobos,
Yosemite, Monterey Bay Aquarium, Wild Animal Park,
Sea World, etc.
Shared Reading Program (PREFACE?)
High Tide author Mark Lynas travels around the world to
investigate local impacts of global warming
These eight guiding questions are common to all of our
informal science education programs:
1. What do you see (observations and descriptions)?
2. What are natural systems made out of (composition and
structure)?
3. How do natural systems work (material properties and
interactions with energy)?
4. How do natural systems change over time (evolutionary
processes)?
5. Where do natural systems come from (origin and/or
formation from building blocks)?
6. What are the relationships between the parts of a system
(interactions and/or common origins)?
7. What are the relationships between natural systems
(interactions and/or common origins)?
8. How do natural systems become more complex over time
(entropy decreases)?
I want to form an informal cross-disciplinary Global Evolution Study Group to
identify and sequence globally important physical and biological events in the
nearly five billion year natural history of the planet.
The group can also help develop a database of system properties and processes,
global evolution models, a global evolution website, natural history exhibits,
academic courses, and indoor and outdoor informal science education projects.
The Global Evolution Study Group will meet once or twice a month to define
questions and to share information that we collect from books, journals,
websites, and experts at museums and universities like UCSB, etc.
Students and faculty in physics, chemistry, biology, math, engineering,
education, and liberal arts are welcome to participate. Global evolution involves
the Sun, solid Earth, oceans, atmosphere, molecules, cells, organisms, and
ecosystems. If you have any interest in one or more of these subjects, send an
email to rfield at the email address at calpoly.edu.
© Bob Field 2007
The Natural History of Planet Earth Timeline:
Five Billion Years of Solar and Global Evolution
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now
oceans
and
atmosphere
solid Earth
and
Sun
molecules
and
cells
PreHadean
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Archaean
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ZAMS
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4000
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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
What do we know about the natural history of planet Earth?
Our planet formed from dust left over when a massive cloud of cold dilute gas and dust
condensed to form the Sun 4.6 billion years ago. The Moon formed from remnants of a
collision between Orpheus and the Earth after the Great Iron Catastrophe formed the
Earth's core. Our planet's surface was initially too hot to form a crust. Four billion years
ago, the Earth was still heavily bombarded by a flux of extraterrestrial objects.
Continents did not exist when the Earth first formed but grew over time.
Most of the water on Earth is in liquid oceans, but much of it has at times been buried in
the land, vaporized into the atmosphere, or frozen solid. Life existed before DNA,
proteins, chlorophyll, and rhodopsin evolved. The solar flux incident on the top of the
atmosphere has increased by 40% over the history of the Earth. During the Proterozoic
Era, photosynthetic bacteria helped remove most of the carbon dioxide from the
atmosphere and released oxygen which was toxic to most bacteria at the time.
Eukaryotes evolved by serial endosymbiosis several times. Eukaryotes are masters of
multicellularity whereas bacteria are masters of metabolic diversity. Plants and animals
are relatively recent evolutionary developments. Invertebrates ventured out of the seas
before vertebrates invaded the land. Whales and other marine mammals are recent
© Bob Field 2007
additions to the oceans.
Geologic Time Scale
Geological Time Scale copyright 2005 - geology.com
http://www.geology.com/
http://geology.com/time.htm
Geological Timeline
Era/Period/Epoch
Time
(Myr ago)
Archaeozoic (Archean) era
5000-1500
Proterozoic era
1500-545
Cambrian period
545-505
Ordovician period
505-438
Silurian period
438-410
Devonian period
410-355
Carboniferous (Mississipian/Pennsylvanian) period
355-290
Permian period
290-250
Triassic period
250-205
Jurassic period
205-135
Cretaceous period
135-65
Paleozoic era
Mesozoic era
Tertiary period
Cenozoic era
"Recent Life"
Quarternary period
www.talkorigins.org/origins/geo_timeline.html
Paleocene epoch
65-55
Eocene epoch
55-38
Oligocene epoch
38-26
Miocene epoch
26-6
Pliocene epoch
6-1.8
Pleistocene epoch
1.8-0.01
(Lower Paleolithic)
0.50-0.25
(Middle Paleolithic)
0.25-0.06
(Upper Paleolithic)
0.06-0.01
Holocene epoch
0.01-0
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
200
Pangaea starts to break apart
200
Primitive crocodiles have evolved
200
Appearance of mammals
145
Archaeopteryx walks the Earth
136
Primitive kangaroos have evolved
100
Primitive cranes have evolved
90
Modern sharks have evolved
65
K-T Boundary--extinction of the dinosaurs and beginning of the reign of mammals
60
Rats, mice, and squirrels have evolved
60
Herons and storks have evolved
55
Rabbits and hares have evolved
50
Primitive monkeys have evolved
28
Koalas have evolved
20
Parrots and pigeons have evolved
20-12
The chimpanzee and hominid lines evolve
10-4
Ramapithecus exist
www.talkorigins.org/origins/geo_timeline.html
Time MYA
545
Event
Cambrian explosion of hard-bodied organisms
528-526
Fossilization of the Chengjiang site
517-515
Fossilization of the Burgess Shale
500-450
Rise of the fish--first vertebrates
430
Waxy coated algae begin to live on land
420
Millipedes have evolved--first land animals
375
The Appalachian mountains are formed via a plate tectonic collision between North
America, Africa, and Europe
375
Appearance of primitive sharks
350-300
Rise of the amphibians
350
Primitive insects have evolved
350
Primitive ferns evolve--first plants with roots
300-200
Rise of the reptiles
300
Winged insects have evolved
280
Beetles and weevils have evolved
250
Permian period mass extinction
230
Roaches and termites have evolved
225
Modern ferns have evolved
225
Bees have evolved
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 develop
3500-2800
Beginning of photosynthesis by blue-green algae 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
1500-600
Rise of multicellular organisms
580-545
Fossils of Ediacaran organisms are made
www.talkorigins.org/origins/geo_timeline.html
Solar and Global Evolution
are parts of Cosmic Evolution
~ age (BY)
generic structure
12
10
5
3
0.01
0.001
0.0000001
galaxies
stars
planets
plants
animals
brains
society
table from Chaisson139
image from Science Yearbook
average power
density (W/kg)
0.00005
0.0002
0.01
0.1
2
15
50
when energy flows, complexity grows
Interactions between
Earth systems
sun
impact
atmosphere
biosphere
oceans
upper crust
lower crust
sediments
subcontinental
lithosphere
oceanic lithosphere
upper mantle
lower mantle
Condie33
Fig 1.33
oceanic
crust
core
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
}
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
Sun
creates
energy
as
a
Stars build
bigproduct
atoms
Sunlight
is the
waste
product
when
from
small
onesit fuses
of “hydrogen
burning”
1
4
and helium
the “spent
4 H is →
He fuel”
The Sun
internal structure and size of layers
density, mass, gravity, pressure, volume
temperature
internal energy distribution
energy sources: fusion energy, gravitational contraction
composition – hydrogen, helium, “metals”, free electrons
material properties
energy transport: convection, conduction, radiation
mass flow in convection
evolution of the Sun – composition ,density, temperature, fusion rate, luminosity
formation of the Sun
zone
fusion core r < ¼
radiative
volume
~r3
1/64
r < 0.7
1/3
Hot and Heavy
convective r > 0.7
2/3
fusion
core
Sun’s
structure
radiative zone
convective zone
total
mass
energy
1/2
2/3
1/2
1/3
1/80
1/100
relative values used in our LANL solar evolution cases
metals composition
Mg 0.000492
Ne 0.000129
C 0.002272
N 0.000697
O 0.006323
relative volume
relative mass
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
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
local gravity g (cm/s2)
250000
local gravity g
200000
g(R) = GM(R)/R2
150000
100000
50000
Earth surface gravity g = 981 cm/s2
0
0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10
radius (cm)
Guzik + Field
4BY Enclosed H and He Mass
1.5E+33
enclosed H mass (g)
1.0E+33
enclosed He mass (g)
5.0E+32
0.0E+00
0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10
radius (cm)
Guzik + Field
Stellar Opacity
5
-4
X=0.7
Z=0.02
4
3
log K (cm2/g)
-2
2
0
1
2
0
-10
-8
-6
-1
-2
4
5
6
7
8
log T (K)
Rosseland mean opacity
curves are labeled by log density (g/cm-3)
Ostlie & Carroll 275
Luminosity Gradient
5E23
4E23
dL/dR = 4πR2ρε
3E23
2E23
1E23
0E00
0E+00
1E+10
2E+10
3E+10
4E+10
5E+10
6E+10
7E+10
radius (cm)
Guzik + Field
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
Luminosity vs. Radius
metal content influences solar luminosity and lifetime
8E+33
4.5 BY Z=0.01
Luminosity (ergs)
7E+33
3 BY Z=0.01
6E+33
1.5 BY Z=0.01
ZAMS Z=0.01
5E+33
4.5 BY Z=0.02
3 BY Z=0.02
4E+33
1.5 BY Z=0.02
3E+33
ZAMS Z=0.02
2E+33
1E+33
0E+00
0E+00
2E+10
4E+10
Radius (cm)
6E+10
8E+10
Guzik Field Lopez x70y28z02 112005
luminosity increases as core hydrogen is depleted
Luminosity vs. Radius
X=.70, Y=.28, Z=.02
Luminosity (ergs/s)
7E+33
6E+33
5E+33
4E+33
9 BY
3E+33
7.5 BY
2E+33
4.5 BY
6 BY
3 BY
1E+33
1.5 BY
ZAMS
0E+00
0E+00
2E+10
4E+10
6E+10
8E+10
Radius (cm)
Guzik Field Lopez x70y28z02 112005
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
Equations of Stellar Structure
dhillon phy213 website
The Solid Earth
size of layers
density, mass, gravity, pressure, volume
composition – iron silicon oxygen magnesium nickel
material properties
temperature
thermal energy distribution
heat flow sources
radioactive decay of U, Th, and K
heat loss as Earth cools
gravitational energy released as Earth cools
latent heat released as inner core freezes
energy transport: convection, conduction, radiation
mass flow in convection
evolution of the Earth’s structure
formation of the Earth
Zeroth order model of the Earth has three layers
mantle
atmosphere
crust
mantle
core
core
First order model of the Earth shows layers
Seismic studies reveal density variations due to composition and phase differences.
atmosphere - radiation
lithosphere - conduction
upper mantle - convection
lower mantle - convection
D” - conduction
convection is powered by
radiogenic heat sources and
produces chemical evolution
outer core – convection?
inner core - conduction
ICB
CMB
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
Whole Earth Element Mass Percent
Ca
17
Al S
16 6
Cr
5
Ni
18
other
5
Fe
O
Si
Fe
320
Mg
154
Mg
Ni
Ca
Si
161
Al
S
O
297
Cr
other
McDonough
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
Relative Mass Abundance of Elements on Earth
zeroth order model - composition
layers
core
mantle
lithosphere
whole Earth
layers
core
mantle
lithosphere
whole Earth
Fe
855
63
63
320
O
0
440
440
297
Si
60
210
210
161
Mg
0
228
228
154
Ni
52
2
2
18
Ca
0
25
25
17
Al
0
24
24
16
S
19
0
0
6
Cr
9
3
3
5
other
5
6
6
5
McDonough
Element Density (kg/m^3)
Element Density (kg/m^3)
14E+03
Core
boundaries
Fe
O
Si
Mg
Density (kg/m^3)
12E+03
10E+03
ICB
8E+03
CMB
6E+03
Mantle
4E+03
2E+03
000E+00
0E+0
1E+6
2E+6
3E+6
4E+6
5E+6
6E+6
7E+6
radius (m)
based on McDonough
Major Elements in Crust and Mantle (%)
(not counting oxygen)
Major Elements (%)
30
25
Crust
Upper Mantle
20
Lower Mantle
Crust + Mantle
15
10
5
0
Mg *
Al *
Si *
Ca *
Fe *
Elements
Elements 2006-07-18 mfischer b revision
Temperature (K)
6000
Liquid Outer Core
Mantle
Temperature (K)
5000
4000
ICB
3000
2000
CMB
boundaries
Temperature (K)
1000
0
0E+0
solidus temperature (K)
1E+6
2E+6
3E+6
4E+6
5E+6
6E+6
7E+6
radius (m)
based on Stacey Appendix G
heat density (J/m^3)
45E+09
Core
heat density (J/m^3)
40E+09
35E+09
ICB
30E+09
25E+09
Mantle
20E+09
CMB
15E+09
10E+09
5E+09
000E+00
0E+0
1E+6
2E+6
3E+6
4E+6
radius (m)
5E+6
6E+6
7E+6
enclosed heat (J)
18E+30
Mantle
enclosed heat (J)
16E+30
14E+30
12E+30
10E+30
8E+30
6E+30
4E+30
Core
2E+30
00E+0
0E+0
1E+6
2E+6
3E+6
4E+6
radius (m)
5E+6
6E+6
7E+6
Stacey Table 6.4 Heat Loss Budget (TW)
INCOME
8.2 Crust radioactivity
19.9 Mantle radioactivity
1.2 Latent heat and gravitational energy released by core evolution
0.6 Gravitational energy of mantle differentiation
2.1 Gravitational energy released by thermal contraction
32 TW TOTAL
EXPENDITURE
8.2 Crust heat loss
30.8 Mantle heat loss
3.0 Core heat loss
42 TW TOTAL
10 TW NET LOSS OF HEAT
radiogenic heat flow (W)
radiogenic heat flow (W)
30E+12
Mantle
25E+12
20E+12
19.9 TW in mantle
8.2 TW in crust……
28.1 TW whole Earth
15E+12
10E+12
5E+12
00E+0
0E+0
Core
1E+6
2E+6
CMB
3E+6
4E+6
5E+6
6E+6
7E+6
radius (m)
based on Stacey
latent heat flow (W)
latent heat flow (W)
4E+12
1 BY
3E+12
2 BY
2E+12
Core
ICB
3 BY
Mantle
1E+12
4 BY
000E+00
0E+0
1E+6
2E+6
3E+6
4E+6
5E+6
6E+6
7E+6
radius (m)
based on Stacey
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 heat flow
1000
1000
800
809
600
617
heat flow in
ocean crust
vs.
continental crust?
400
200
23
49
inner core
outer core
0
lower
mantle
upper
mantle
lithosphere
Absolute and Relative Energy, Heat, and Heat Flow
first order model – composition and phase
layers
inner core
outer core
lower mantle
upper mantle
lithosphere
whole Earth
continental crust
ocean crust
internal
energy (J)
3.15E+29
5.35E+30
9.12E+30
2.09E+30
1.20E+29
1.70E+31
heat
sources
(W)
9.85E+11
1.11E+12
2.43E+13
8.22E+12
8.17E+12
4.28E+13
total heat
flow (W)
9.85E+11
2.10E+12
2.64E+13
3.46E+13
4.28E+13
4.28E+13
relative
internal
energy
19
315
537
123
7
1000
relative
heat
relative
sources heat flow
23
23
26
49
568
617
192
809
191
1000
1000
1000
zeroth order model - composition
layers
core
mantle
lithosphere
whole Earth
internal
energy (J)
5.67E+30
1.12E+31
1.20E+29
1.70E+31
heat
sources
(W)
2.10E+12
3.25E+13
8.17E+12
4.28E+13
total heat
flow (W)
2.10E+12
3.46E+13
4.28E+13
4.28E+13
relative
internal
energy
333
659
7
1000
relative
heat
relative
sources heat flow
49
49
760
809
191
1000
1000
1000
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
first order model – composition and phase
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
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
energy (J)
3.15E+29
5.35E+30
9.12E+30
2.09E+30
1.20E+29
1.70E+31
zeroth order model - composition
layers
core
mantle
lithosphere
whole Earth
volume
(m^3)
1.77E+20
8.66E+20
4.03E+19
1.08E+21
mass (kg)
1.93E+24
3.88E+24
1.25E+23
5.94E+24
average
density
(kg/m^3)
1.19E+04
4.24E+03
3.11E+03
5.48E+03
internal
energy (J)
5.67E+30
1.12E+31
1.20E+29
1.70E+31
heat
sources
(W)
9.85E+11
1.11E+12
2.43E+13
8.22E+12
8.17E+12
4.28E+13
total heat
flow (W)
9.85E+11
2.10E+12
2.64E+13
3.46E+13
4.28E+13
4.28E+13
heat
sources
(W)
2.10E+12
3.25E+13
8.17E+12
4.28E+13
total heat
flow (W)
2.10E+12
3.46E+13
4.28E+13
4.28E+13
Relative Volume, Mass, Energy, Heat, and Heat Flow
first order model – composition and phase
layers
inner core
outer core
lower mantle
upper mantle
lithosphere
whole Earth
continental crust
ocean crust
relative
volume
7
156
554
246
37
1000
relative
mass
17
308
492
162
21
1000
relative
internal
energy
19
315
537
123
7
1000
relative
heat
relative
sources heat flow
23
23
26
49
568
617
192
809
191
1000
1000
1000
zeroth order model - composition
layers
core
mantle
lithosphere
whole Earth
relative
volume
163
800
37
1000
relative
mass
325
654
21
1000
relative
internal
energy
333
659
7
1000
relative
heat
relative
sources heat flow
49
49
760
809
191
1000
1000
1000
convection model for an ideal gas
force / area = viscosity x velocity gradient
constant P = (ρ-Δρ)k(T+ΔT)/mp
force = Δρ(πru2 ΔR)gR
ΔR
cylinder area = 2πruΔR
Δρ(πru
2 ΔR)g
R/(2πruΔR)
= η Δvmass/Δr
Δr
vmass
ru
Δρ ru gR / 2 = η Δvmass/Δr
vmass = Δρ ru gR Δr / 2η
what if you have molten rocks?
Typical Cartoon of Mantle Convection and Plumes
Stacey318
Radiogenic Heat Flow (W)
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
Thermally important radioactive elements in the Earth
μW/kg
estimated
total
energy/atom μW/kg of
isotope
of
total Earth
heat
(MeV)
isotope
element content (kg) (1012 W)
total heat
4.5 BYA
(1012 W)
238U
47.7
95
94.35
13.15x1016
12.5
25.1
235U
43.9
562
4.05
0.0954x1016
0.54
45.1
232Th
40.5
26.6
26.6
47.2x1016
12.56
15.7
0.0035
7.14x1020
(total K)
2.5
30.2
28.1
117.3
40K
total
0.71
30
These energies include all series decays to final daughter products. Average locally
absorbed energies are considered; neutrino energies are ignored. (after Stacey Table 6.2)
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
latent heat flow (W)
latent heat flow (W)
4E+12
3E+12
2E+12
Core
ICB
Mantle
2 BYA after 2 BY of freezing
1E+12
now after 4 BY of freezing
000E+00
0E+0
1E+6
2E+6
3E+6
4E+6
5E+6
6E+6
7E+6
radius (m)
based on Stacey
before and after the Great Iron Catastrophe
enclosed GBE vs. volume
2.5E+32
enclosed GBE (J)
GBE (joules)
2.E+32
"average density" enclosed GBE (J)
almost
exactly
3GM2/5R
1.5E+32
1.E+32
5.E+31
0.E+00
0.E+0
2.E+20 4.E+20 6.E+20 8.E+20 1.E+21 1.2E+21
volume (m3)
before and after the Great Iron Catastrophe
shell ΔT vs. volume
40000
If iron accretes first, core is much hotter and
mantle much cooler than if uniform composition
accretes. (if layers retain all GBE)
shell ΔT (K)
20000
0
-20000
-40000
0.E+0
2.E+20
4.E+20
6.E+20
8.E+20
volume (m3)
1.E+21 1.2E+21
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
The Atmosphere
size of layers
density, mass, gravity, pressure, volume
composition – nitrogen oxygen water argon carbon dioxide aerosols
material properties
temperature
global energy budget and distribution – latitude season altitude
heat flow sources
absorbed sunlight
Earth’s radiated energy
air-sea interactions
energy transport: convection, conduction, radiation
mass flow in convection
evolution of the atmosphere – composition structure density circulation
origin of the atmosphere
Average Global Energy Budget (W/m2)
343
planet (21 + 69 + 16) + (22 + 90 + 125) = 343
incident
reflected
outgoing
shortwave flux
shortwave flux
longwave flux
343
21 69 16
22
90
125
surfaceatmosphere
heat transfer
atmosphere
emitted
by clouds
back
scattered
by air
absorbed
by clouds
emitted by
surface
reflected
by clouds
20
emitted
by H2O, CO2,
aerosols
12
0
absorbed
absorbed
by H2O, CO2,
by clouds
aerosols
48
absorbed
by H2O, O3,
aerosols
emitted
by H2O, CO2,
aerosols
reflected
by surface
169
390
327
24
8
16
sensible
heat
flux
16
90
latent
heat
flux
90
surface
(20 + 48) + (120 + 248 + 16 + 90) = 542
after Salby45, etc.
atmosphere
(90 + 125) + 327 = 542
169 + 327 = 496 surface 390 + 16 + 90 = 496
atmospheric composition (fraction by volume)
Methane (CH4) 0.000001745
Helium (He) 0.00000524
values are for dry air
water vapor is shown as
an additional 1% but
varies enormously
Krypton (Kr) 0.00000114
Neon (Ne) 0.00001818
Carbon dioxide (CO2)
0.000381
Argon (Ar) 0.00934
Nitrogen (N2)
Oxygen (O2)
Argon (Ar)
Oxygen (O2)
0.20946
Carbon dioxide (CO2)
Neon (Ne)
Helium (He)
Nitrogen (N2)
0.78084
Methane (CH4)
Krypton (Kr)
Hydrogen (H2)
Water vapor (H2O)
composition
by mass?
Hydrogen (H2) 0.00000055
Water vapor (H2O)
0.01
Temperature vs. Altitude
f
Sun
Thermosphere
Temperature
of the atmosphere
-130F
60 miles
50
Mesosphere
40
30 miles
-70F
75% of air
32F
ozone
layer
Stratosphere
20
10
Troposphere
60F
sea level
ocean
After Tarbuck
temperature (K)
400
300
200
100
0
0
20000
40000
80000
60000
altitude (m)
100000
120000
temperature (K)
300
290
280
270
260
250
240
230
220
210
200
~6.6 K per kilometer
0
2000
6000
4000
altitude (m)
8000
10000
Density (kg/m3)
Density (kg/m3)
1E+0
1E-1
~10X decrease per 15-20 km ascent
1E-2
density (kg/m3)
calculated density (kg/m3)
1E-3
1E-4
0
10000 20000 30000 40000 50000 60000 70000 80000
altitude (m)
Calculated Enclosed Mass (kg)
Enclosed Mass (kg)
5E+18
half of the mass of the atmosphere
is below an altitude of 6 km and
is enclosed in a volume of
500 million km2 x 6 km
or 3 billion km3
or 3x1018 m3
4E+18
3E+18
2E+18
1E+18
0E+00
0
10000 20000 30000 40000 50000 60000 70000 80000
altitude (m)
0.12
Equinox
Solar Flux vs. Time of Day
Equator
0.1
Tropic
of
Cancer
0.08
0.06
0.04
Arctic Circle
0.02
North Pole
0
0
midnight
4
8
6 am
12
Noon
16
20
6 pm
24
midnight
0.12
Summer Solstice
Solar Flux vs. Time of Day
Tropic
of
Cancer
0.1
0.08
0.06
North Pole
0.04
0.02
0
24
2
Midnight
4
6
6 am
8
10
12
Noon
14
16
18
6 pm
20
22
24
Midnight
2000
Spectrum of Sunlight observed on Earth
visible
window
scattering by N2, O2 and aerosols
Intensity
1500
sun is directly overhead
no clouds
direct beam only
absorption by ozone,
water, and CO2
1000
500
0
0.3
0.5
UV Visible
1
1.5
Infrared
2
2.5
Wavelength
3
Ultraviolet Average Flux at 35N on Summer Solstice
Absorption Losses
Scattering Losses
Flux at Surface
50
Flux (W/m^2)
40
30
20
10
0
cda
cma
dda
atmospheres
dma
Field - solar flux code
Visible
Solar
Energy
0.5 micron peak
Sun is 6000K
Sun
2 Blackbodies
1 Greenhouse
CO2 and H2O gases
absorb far infrared
atmosphere transparent
to visible light
Earth
Far Infrared
Energy
10 micron peak
Earth is 300K
Blackbody Radiation
300
5800K
solar energy
absorbed
by Earth
Intensity
250
200
373K
water
boils
150
100
273K
water
freezes
255K
atmosphere
50
0
0
5
10
Wavelength
15
20
25
30
l
Greenhouse Gases Absorb Blackbody Radiation
30
288K Earth's surface
Intensity
25
20
CO2
O3
15
H2O
10
255K
atmosphere
5
0
0
5
10
15
Wavelength (microns)
20
25
30
l
f
Sun
Average Visible Reflectances
of common substances
Clouds
50%
Sand
40%
Water
8%
Plants
15%
Soil
20%
Snow
60%
Energy Transfer in a Day
0.12
What is the
hottest time
of day?
0.1
0.08
heat
gain
desert
heat loss
0.06
ocean
heat loss
0.04
land
heat loss
0.02
0
24
2
Midnight
4
6
6 am
8
10
12
Noon
14
16
18
6 pm
20
22
24
Midnight
atmospheric circulation
bottom heated
absorbed heat peaks at Equator
no rotation
with rotation
Average Global Energy Budget (W/m2)
343
incident
shortwave flux
343
planet
(90 + 16) + (22 + 215) = 343
reflected
outgoing
shortwave flux longwave flux
90 16
22
215
absorbed and
reflected by
clouds, H2O, O3,
aerosols
atmosphere
emitted by
surface
368
368
surfaceatmosphere
heat transfer
absorbed and
emitted by
clouds, H2O,
CO2, aerosols
106
106
68
68
latent and
sensible heat
flux
reflected
by surface
169
390
327
106
surface
(68) + (368 + 106) = 542
after Salby45, etc.
atmosphere
(215) + 327 = 542
169 + 327 = 496 surface 390 + 106 = 496
OASES HW #2B
incident SW flux W/m2 use global 343
averageuse global average
=90/343
gas SW reflection
0.262
=68/343
gas SW absorption
0.198
=368/390
gas LW absorption
0.944
surface SW reflection
0.086
surface SW absorption
0.914
surface latent and sensible heat
0.214
surface LW net absorption
0.786
=16/(169+16)
=1-C6
=106/(169+327)
=1-C8
fraction of unity
343
©Bob Field 2006
fraction of unity
HW2B
=C4*C2
above
absorbs from above
gas SW absorption W/m2 only absorbs
68fromonly
=C5*C16
gas LW absorption W/m2
=C10+C11
gas W/m2
368
not counting436
non-radiative
flux non-radiative flux
not counting
=C7*(1-C3-C4)*C2
surface SW absorption W/m2
169
=E14*(C12+C17)
surface LW absorption W/m2
+LH+SH
327
=C13+C14
surface W/m2
496
=C15-C17
radiating flux W/m2
390
=C8*C15
latent and sensible heat W/m2
106
=(C16/0.0000000567)^0.25
surface temperature K
+LH+SH
0.603
=327/(327+215)
E14
fillfill
in in
E14
!!! !!!
LW down
LW down
welling
fraction
welling
fraction
gasgas
to Earth
from
to
Earth
288
Use the information in the diagram
Use the information in the diagram of a simplified global ener
Every row is a fra
Use
physics
andsens
com
Use physics
and
common
SW
is short wavelen
SW is short
wavelength
as in
Hintto
- Be
Hint - Be sure
accs
bonus
gas temperature K
=((C12+C17)*(1-$E$14)/0.0000000567)^0.25planet temperature K
=(((C12+C17)*(1-$E$14)+(C16-C11))/0.0000000567)^0.25
248
254
The Oceans
size of layers
density, mass, gravity, pressure, volume
composition – water salt dissolved gases and organics particulates organisms
material properties
temperature
global energy budget and distribution – latitude season altitude
heat flow sources
absorbed sunlight
air-sea interactions
energy transport: convection, conduction, radiation
mass flow in convection
evolution of the ocean – salt ice evaporation flow patterns depth area
origin of the ocean
Elemental composition of sea water (by mass)
Sulfur 0.0885
Magnesium 0.135
Sodium 1.05
Calcium 0.04
Potassium 0.038
Bromine 0.0065
Chlorine 1.9
Carbon 0.0026
Oxygen
Hydrogen
Hydrogen 10.8
Chlorine
Sodium
Magnesium
Sulfur
Calcium
Potassium
Oxygen 85.7
Bromine
Carbon
wikipedia
Abundance of
Dissolved Gases
Ratio of Total
Amount in Ocean
Gas Dry Air Sea Water to Atmosphere
N2
78%
12 ppm
0.004
O2
21%
7 ppm
0.01
CO2 0.036%
90 ppm
62
H2O 0.3%
97%
100,000
vapor transport
10
precipitation
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
Sea Water & Fresh Water
Oceans hold 97.4% of Earth’s water
with a sphere depth of 1.7 miles
Reservoir
Fresh%
Sphere Depth
Atmosphere
0.04
1 inch
Lakes
0.4
1 foot
Ground Water
25
60 feet
Polar Caps & Ice
75
180 feet
from Stowe
500 million square km area x 3 km depth = 1.5x109 km3
volume of stored water
Reservoir
Oceans
Ice caps & glaciers
Groundwater
Lakes
Soil moisture
Atmosphere
Streams & rivers
Biosphere
volume of water
(106 km³)
1370
29
9.5
0.125
0.065
0.013
0.0017
0.0006
1408.7047
Percent of total
97.25
2.05
0.68
0.01
0.005
0.001
0.0001
0.00004
1.4x109 km3 volume x 1000 kg/m3 x 109 m3/km3 = 1.4x1021 kg
wikipedia
Average reservoir
residence times
Reservoir
Oceans
Glaciers
Seasonal snow cover
Soil moisture
Groundwater: shallow
Groundwater: deep
Lakes
Rivers
Atmosphere
Average residence
time (years)
3,200 years
20 to 100 years
2 to 6 months
1 to 2 months
100 to 200 years
10,000 years
50 to 100 years
2 to 6 months
9 days
wikipedia
Ocean and Atmosphere simplified heuristic models
1. An Earthlike planet rotates on its axis. There is no atmosphere. The planet is dry except for an
ocean located on the Equator in a canal that is three kilometers deep and 3000 km wide (or less)
and encircles the planet. Ignore any non-uniform heating effects from the Sun. I claim that the
steady state solution is that the ocean water moves with the Earth so that an observer on Earth
sees no currents in the ocean. True or False?
2. Would the same argument also apply if the entire featureless planet were covered with 3 km
deep water? The equatorial bulge of the Earth due to its rotation will also appear in the global
ocean so that the water depth would be 3 km at all latitudes. Since no water is flowing between
latitudes, no Coriolis effects will appear even though water at different latitudes has different
velocities but the same angular velocity. Therefore I claim that on a water covered planet, an
observer would observe no currents in the ocean relative to the sea floor. True or False?
3. The same argument applies to the atmosphere of a featureless planet whether or not there is an
ocean covering it. No winds appear as long as the planet is uniformly heated. If the ocean is top
heated uniformly and the atmosphere is bottom heated uniformly, then the ocean will still have
no currents, but the atmosphere will have a vertical air flow (thermals) that resembles Benard
cells, but no Hadley cells between latitudes. True or False?
4. Do local perturbations produce transient flow patterns due to flow instabilities particularly in
the lower viscosity atmosphere?
5. In the case of non-uniform heating, fluids flow between latitudes and the velocity differences
between masses of air (and water) at different latitudes produce Coriolis effects. True or False?
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
surface currents are driven by winds which result from
non-uniform heating of the globe
Keith Stowe, Exploring Ocean Science
Sun
pelagic zone
(water column)
Ocean Zones
pelagic / benthic
plankton
& nekton
Sun
10%
50'
0' 300'
40'
15'
2'
UV V B G Y O R IR
photic zone
(light)
Ocean Zones
aphotic zone
photic / aphotic
(dark)
f
Sun
pelagic zone
(water column)
Ocean Zones
pelagic / benthic
photic / aphotic
photic zone
(light)
aphotic zone
(dark)
f
Nereus & 50 Nereid
Sun
neritic province
oceanic province
(above continental shelf) (beyond continental shelf)
pelagic zone
(water column)
Ocean Zones
pelagic / benthic
photic / aphotic
neritic / oceanic
photic zone
(light)
aphotic zone
(dark)
f
space and Sun Sun
water world
atmosphere
photic zone
(light)
pelagic zone
(water column)
aphotic zone
(dark)
“continental crust”
oceanic crust
Sun
atmosphere
ocean
continental crust
oceanic crust
f
Sun
atmosphere
upwelling
continental crust
ocean
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
absorption and scattering coefficients of air and water
10
10
actual curves of components
depend on concentrations
 ( l  0)
 ( l  0 )  ( l  0 )
1
p ( l  1 )  (  ( l  0 )  ( l  0 ) )
y ( l  2 )  (  ( l  0 )  ( l  0 ) )
g( l  3 )  (  ( l  0 )  ( l  0 ) )
air( l )  air( l )
air( l )  air( l )  (  ( l  0)  ( l  0) ) 0.1
0.01 0.01
30 0
l1
35 0
40 0
45 0
50 0
55 0
l
60 0
65 0
70 0
75 0
80 0
l2
Field - solar sea flux code
transmitted sunlight in pure water vs. depth
(0, 1, 3, 10, 30, 100 meters)
max
0.8
0.6
Tz    l  z k  0 
Hy ( l )
0.4
0.2
0
0
30 0
l1
35 0
40 0
45 0
50 0
55 0
l  Hx( l )
60 0
65 0
70 0
75 0
80 0
l2
Field - solar sea flux code
zone areas
surface area (m2)
disk area (m2)
3E+14
2.6E+14
2E+14
1.3E+14
1E+14
1.0E+14
6.4E+13
3.1E+13
3.1E+13
0E+00
torrid
temperate
2.1E+13
1.8E+12
frigid
hemisphere
zone temperatures
average temperature (K)
noon peak temperature (K)
400
350
361
361
353
300
287
250
269
255
250
200
195
150
100
50
0
torrid
temperate
frigid
hemisphere
required latitudinal heat outflow (W)
7E+15
6E+15
5E+15
4E+15
3E+15
2E+15
1E+15
0E+00
0
10
20
30
40
50
latitude (degrees)
60
70
80
90
hypothetical air speed or water speed (m/s)
1.5
air speed (m/s)
water speed (m/s)
1.0
air
delta T = 40 K
4000 m high column
density = 1.228 kg/m3
specific heat = 1000 J/kg-K
0.5
water
delta T = 10 K
10 m deep column
density = 1000 kg/m3
specific heat = 4186 J/kg-K
0.0
0
10
20
30
40
50
latitude (degrees)
60
70
80
90
water 1/mfp (1/m) vs. wavelength
1E+4
1E+3
1E+2
1E+1
1E+0
1E-1
1E-2
300 400 500 600 700 800 900 1000 1100 1200 1300 1400
wavelength (nm)
Flux absorbed per meter (W/m3)
flux absorbed per meter vs. depth (m)
200
150
100
50
0
0
5
10
15
depth (m)
20
25
30
Organisms
and
Ecosystems
1700 pounds of particulate is detritus
240 pounds phytoplankton
60 pounds zooplankton
1 pound of large animals
Sun
ocean
60 tons of organic matter in ocean is
dissolved organic molecules
(yellow matter)
one ton of organic matter in ocean is
particulate
after Stowe
86% of particulate is detritus = 30 gC/m2
12% is phytoplankton = 4 gC/m2
3% is zooplankton = 1 gC/m2
0.05% is large animals = 0.02 gC/m2
Sun
ocean
98.3% of all organic matter in ocean is
dissolved organic molecules = 2000 gC/m2
1.7% of all organic matter in ocean is
particulate = 35 gC/m2
after Stowe
Distribution of Animal Species
200,000 ocean animal species
(98% benthic)
4,000
pelagic
animal
species
one million land animal species
(75% insects)
Plant Production
Open
Ocean
Ocean Fish Production
Land
Upwelling
Coastal
Upwelling
The land is over three times more productive per square mile than the oceans.
There is more carbon production on land (25 billion tons per year)
Open Ocean
than the much greater oceans (20 billion tons per year), even though the Earth is 72% ocean.
In the oceans, the coastal areas account for 18% of the plant production but only 10% of the area.
Upwelling areas account for 0.5% of the production but only 0.1% of the area.
after Keith Stowe, Exploring Ocean Science
Ocean Fish
Productivity/Area
Plant Productivity/Area
200
175
150
100
75
50
Upwelling
125
150
Land
Upwelling
200
100
Coastal
waters
Open
Ocean
50
Coastal Open
waters Ocean
25
0
0
Tjeerd van Andel, Science at Sea: Tales of an Old Ocean
considerations
universe
requirement
oceans
recycles per year
steps of bacterial
decompostion*
nitrogen phosphorus
200
15
1
1
6
1
10
4
3
1
*before sinking below the photic zone
from Stowe & Thurman
Seasonal Abundance of Sunlight,
Nutrients, Phytoplankton, Grazers
Nutrients
Phytoplankton
Jan
Sunlight
Grazers
Feb March April May
June
July
Aug
Sept
Oct
Nov
Dec
After Stowe 276
productivity (gC/m /day)
2
0.9
continental
shelf
0.6
0.3
central
ocean
0
Jan
Feb
Mar
Apr
May June July
Aug
Sep
Oct
Nov
Dec
after Keith Stowe, Exploring Ocean Science
high latitudes
productivity (gC/m /day)
2
0.9
temperate
0.6
0.3
central
ocean
0
Jan
Feb
Mar Apr
May
June
July
Aug
Sep Oct
Nov
Dec
after Keith Stowe, Exploring Ocean Science
continental
shelf
Sun
annual carbon cycle in the atmosphere
110
93
109
+1
7
-7
90
ocean
billions of tons of carbon
+3
Sun
where is the carbon?
(billions of metric tons) carbon dioxide gas
in atmosphere 700
humus
2000
sediments
20,000,000
photosynthesis removes
4 billion tons of carbon
from atmosphere per year
Dissolved organic matter ~2000
fossil fuels
5000?
from Biology of plants 5th Ed. by Raven et al. page 115
dissolved gas 40,000
ocean
deep ocean
38,000,000
Molecules
and
Cells
What do cells do?
Modern cells are chemical factories:
complex, highly efficient, self-replicating.
Cells store and release energy to build up and
break down biomolecules...
Store, exchange, and transform:
matter
energy
information
The Origin of Life
Complex molecules form and evolve
Simple proto-cells form and evolve
Modern cells evolve and diversify
All living things are related to a common ancestor
5 kingdoms:
bacteria
algae
fungus
plant
animal
Trefil and Hazen
The Sciences:
An Integrated Approach
The
natural
of molecules
is the
The
cell is selection
the building
block of life.
essence
of the
origin
and evolution
of life.
All cells
are
descended
from cells.
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%
2.7
0.3
CHO
0.08
-
many common molecules
are made from CHONSP
C
H
O
O
H
H O
C
S
N
H
O
H
O
C
H
O
P
N
O
O
O
O
H
H
O
O
N
H
P
H
H
O
N
H
O
N
H
S
C
H
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
CHONSP molecules are abundant in space:
100 tons per year of IPDs 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)
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 ....
.
O
O
O
O
H
H O
O
O
O
O
H
H
O
O
O
6 O2
H
C
O H
H
H
C
C
O
O
C
H
H
C
C
O
O
H
H
glucose
O
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
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
1
H2O
H2O
H2O
2
3
H2O
4
H2O
5
H2O
6
H2O
7
H2O
8
9
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
ribosomes reuse tRNA and mRNA
not necessarily an intelligent design
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
H
H O C H
H
C
O
H
C O H
H
H
C
O
H
H
C
O
H
H
C
O
H H O
H N C C O H
H H C H
H CCC C
C H
H C CC N
H
H
The Facts of Life
All cells come from other cells
All cells have membranes, proteins, carbs, & DNA
All cells use similar metabolic processes
All cells use the same genetic code for replication
C C C C C C C C
His Ala Tyr Val Thr Val Arg Leu Gly
All 1cells
descended from a last common ancestor
2
R
Pi
C C C C
The first cells came from non-cellular materials
and were much simpler than any modern cells
D
A
G UA C G C
AU G CAU G C G UAU G U UACAG U C C GAC UAG GAU GA
Pi
D
T
Pi
D
C
Pi
D
Pi
A
R
A
D
Pi
G
Pi
Pi
Pi
Let me be crystal clear:
Complex patterns
do not require
intelligent designers!
http://www.its.caltech.edu/~atomic/snowcrystals/photos/photos.htm
Eukaryotes are world champs of
multicellularity and cell differentiation
Identical Cells Multiply by Dividing
Identical cells differentiate to
develop into a multicellular organism
protocells feed on molecules
replication
processes evolve
LCA
bacteria
metabolic processes evolve
archaea
eucarya
sulfur
hotter
hot
salt
sun
methane
lateral and vertical
proto
gene transfer cell
Last common ancestor appears
LCA branches into
The first eukaryote
grew
archaebacteria,
eubacteria,
and
10,000 times
larger than
eukaryote
predecessors
other bacteria
because
its
metabolic
processes
diversify
membrane
lostevolve
its cell wall.
autotrophs
Multicellularity
(the labeled branches)
evolved independently
a number of times
Animals
Fungi
Red algae
Green algae
Plants
Brown algae
Diatoms
Eukarya
Ciliates
Sorogena
last
common
ancestor
Myxomycetes
Cellular slime molds
Foraminifera
A molecular phylogeny of the major groups of
organisms, showing that multicellularity (the labeled
branches) evolved independently a number of times.
The tree is based on a small subunit of the ribosomal
RNA. The rectangles indicate terrestrial groups.
Methanosarcina
Myxobacteria
Cyanobacteria
Actinomycetes
Archaea
Bacteria
2
2
4
8
8
32
16
128