rfield website Global Evolution Timeline Global models and database The SunThe Sun and Solid...

rfield website

Global Evolution Timeline

Global models and databaseThe 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 FIELDAdjunct Physics Professor

Research Scholar in ResidenceI 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

http://www.calpoly.edu/~phys

GLOBAL EVOLUTION STUDIESThe 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.

go to natural science projects, natural history programs, globalevolution, or rfield home page

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:

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.

Global Evolution Endowment

NHOPE Timeline.xls

PGEM Events.doc

PGEM Database.ppt

OASESMCOE.doc

NHOPE ISE project proposal

Natural History of the California Coast

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere

subcontinentallithosphere

sedimentslower crust

upper crust

impact

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere



upper crust

impact

Solar and Global Evolution Models

Sun

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere



upper crust

impact

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere



upper crust

impact

Solar and Global Evolution Models

Sun

click on any figure

Natural History of Planet EarthNatural History of Planet Earth

Global Evolution© Mike Baird

How do global changesimpact 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 publicationsbirds, 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 programsMontana 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

from MY

to MY

MYA Eraoceans

and atmosphere

solid Earth and Sun

molecules and cells

organisms and

ecosystems-300 -200 -4900-200 -100 -4800-100 0 -4700

ZAMS 100 -4600100 200 -4500200 300 -4400300 400 -4300400 500 -4200500 600 -4100600 700 -4000700 800 -3900800 900 -3800900 1000 -37001000 1100 -36001100 1200 -35001200 1300 -34001300 1400 -33001400 1500 -32001500 1600 -31001600 1700 -30001700 1800 -29001800 1900 -28001900 2000 -27002000 2100 -26002100 2200 -25002200 2300 -24002300 2400 -23002400 2500 -22002500 2600 -21002600 2700 -20002700 2800 -19002800 2900 -18002900 3000 -17003000 3100 -16003100 3200 -15003200 3300 -14003300 3400 -13003400 3500 -12003500 3600 -11003600 3700 -10003700 3800 -9003800 3900 -8003900 4000 -7004000 4100 -6004100 4200 -5004200 4300 -4004300 4400 -3004400 4500 -2004500 4600 -1004600 4700 now

Phaner- ozoic

Pro

tero

zoic

The Natural History of Planet Earth Timeline: Five Billion Years of Solar and Global Evolution

Had

ean

Pre-Hadean

Arc

hae

anName ten or more

globally important eventsin any column.

Think about the W5H:whowhatwhenwherewhyhow

Emphasis onconnections not collections

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 additions to the oceans. © Bob Field 2007

Geologic Time Scale

Geological Time Scale copyright 2005 - geology.com http://www.geology.com/ http://geology.com/time.htm

Era/Period/Epoch Time

(Myr ago)

Archaeozoic (Archean) era 5000-1500

Proterozoic era 1500-545

Paleozoic era

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

Mesozoic era

Triassic period 250-205

Jurassic period 205-135

Cretaceous period 135-65

Cenozoic era"Recent Life"

Tertiary period

Paleocene epoch 65-55

Eocene epoch 55-38

Oligocene epoch 38-26

Miocene epoch 26-6

Pliocene epoch 6-1.8

Quarternary period

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 0.01-0www.talkorigins.org/origins/geo_timeline.html

Geological Timeline

Time MYA Event

4 Development of hominid bipedalism

4-1 Australopithecus exist

3.5 The Australopithecus Lucy walks the Earth

2 Widespread use of stone tools

2-0.01 Most recent ice age

1.6-0.2 Homo erectus exist

1-0.5 Homo erectus tames fire

0.3Geminga supernova explosion at a distance of roughly 60 pc--roughly as bright as the Moon

0.2-0.03 Homo sapiens neanderthalensis exist

0.050-0 Homo sapiens sapiens exist

0.04-0.012Homo sapiens sapiens enter Australia from southeastern Asia and North America from northeastern Asia

0.025-0.010 Most recent glaciation--an ice sheet covers much of the northern United States

0.020 Homo sapiens sapiens paint the Altamira Cave

0.012 Homo sapiens sapiens have domesticated dogs in Kirkuk, Iraq

0.01 First permanent Homo sapiens sapiens settlements

0.01 Homo sapiens sapiens learn to use fire to cast copper and harden pottery

0.006 Writing is developed in Sumeria

www.talkorigins.org/origins/geo_timeline.html

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


Time MYA Event

545 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

375The 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


Time MYA Event

4600 Formation of the approximately homogeneous solid Earth by planetesimal accretion

4300Melting of the Earth due to radioactive and gravitational heating which leads to its differentiated interior structure as well as outgassing of molecules such as water, methane, ammonia, hydrogen, nitrogen, and carbon dioxide

4300Atmospheric water is photodissociated by ultraviolet light to give oxygen atoms which are incorporated into an ozone layer and hydrogen molecules which escape into space

4000 Bombardment of the Earth by planetesimals stops

3800 The Earth's crust solidifies--formation of the oldest rocks found on Earth

3800 Condensation of atmospheric water into oceans

3500-2800 Prokaryotic cell organisms develop

3500-2800Beginning 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

2400Rise in the concentration of oxygen molecules stops the deposition of uraninites (since they are soluble when combined with oxygen) and starts the deposition of banded iron formations

1600The last reserves of reduced iron are used up by the increasing atmospheric oxygen--last banded iron formations

1500 Eukaryotic cell organisms develop

1500-600 Rise of multicellular organisms

580-545 Fossils of Ediacaran organisms are made


Solar and Global Evolutionare parts of Cosmic Evolution

~ age (BY) generic structureaverage power density (W/kg)

12 galaxies 0.00005

10 stars 0.0002

5 planets 0.01

3 plants 0.1

0.01 animals 2

0.001 brains 15

0.0000001 society 50

table from Chaisson139image from Science Yearbook

when energy flows, complexity grows

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere



upper crust

impactInteractions between

Earth systems

Condie33Fig 1.33

sun

C6 12

N7 14

O8 16

H1 1

He2 4Periodic Table of

Chemical Elements

92% ~8%

0.07%0.04%0.02%0.01%

Abundance in Universe in %0.1% }

Ne10 20

Na11 23

Mg12 24

Al13 27

Si14 28

P15 31

S16 32

Cl17 35

Ar18 40

K19 39

Ca20 40

Cr24 62

Mn25 55

Fe26 56

Ni28 59

0.02% everything else

Stars build big atoms from small ones

Sunlight is the productof “hydrogen burning”

and helium is the “spent fuel”

Sun creates energy as a waste product when it fuses

4 H1 → He4

The Suninternal structure and size of layersdensity, mass, gravity, pressure, volumetemperatureinternal energy distributionenergy sources: fusion energy, gravitational contractioncomposition – hydrogen, helium, “metals”, free electronsmaterial propertiesenergy transport: convection, conduction, radiationmass flow in convectionevolution of the Sun – composition ,density, temperature, fusion rate, luminosityformation of the Sun

convective zone

radiative zone

fusioncore

Hot and Heavy

Sun’sstructure

zonevolume

~r3 masstotal

energy

fusion core r < ¼ 1/64 1/2 2/3

radiative r < 0.7 1/3 1/2 1/3

convective r > 0.7 2/3 1/80 1/100

metals composition

C 0.002272

N 0.000697

O 0.006323

Ne 0.000129

Mg 0.000492

relative values used in our LANL solar evolution cases

relative volume

fusion core 16

radiative zone 343

convective zone 641

relative mass

fusion core 481radiative

zone 492

convective zone 27

relative heat flow

1000988

1000

0

200

400

600

800

1000

fusion core radiative zone convective zone

relative total energy

radiative zone 356

fusion core 637

convective zone 7

relative fusion power

convective zone 0

fusion core 988

radiative zone 12

layers volume (cm3) mass (g)average density

(g/ cm3)

relative volume

relative mass

relative average density

fusion core 2.22E+31 9.57E+32 43.19 16 481 30784

radiative zone 4.86E+32 9.79E+32 2.01 343 492 1434

convective zone 9.10E+32 5.37E+31 0.06 641 27 42

whole Sun 1.42E+33 1.99E+33 1.40 1000 1000 1000

layerstotal

energy (ergs)

fusion power

(erg/ s)

luminosity (erg/ s)

relative total

energy

relative fusion power

relative heat flow

fusion core 1.95E+48 3.80E+33 3.80E+33 637 988 988

radiative zone 1.09E+48 4.62E+31 3.85E+33 356 12 1000

convective zone 2.00E+46 0.00E+00 3.85E+33 7 0 1000

whole Sun 3.06E+48 3.85E+33 3.85E+33 1000 1000 1000

Density (g/cm^3)

0

20

40

60

80

100

120

140

160

0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10

radius (cm)

Guzik - LANL solar evolution code

local gravity g (cm/s2)

0

50000

100000

150000

200000

250000

0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10

radius (cm)

loca

l gra

vity

g

Earth surface gravity g = 981 cm/s2

g(R) = GM(R)/R2

Guzik + Field

4BY Enclosed H and He Mass

0.0E+00

5.0E+32

1.0E+33

1.5E+33

0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10

radius (cm)

enclosed H mass (g)

enclosed He mass (g)

Guzik + Field

Ostlie & Carroll 275

5

4

3

2

1

0

-1

-24 5 6 7 8

log

K (

cm2 /

g)

log T (K)

-10 -8 -6

-2

0

-4

2

X=0.7Z=0.02

Rosseland mean opacitycurves are labeled by log density (g/cm-3)

Stellar Opacity

Luminosity Gradient

0E00

1E23

2E23

3E23

4E23

5E23

0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10

radius (cm)

Guzik + Field

dL/dR = 4πR2ρε

Solar Evolution

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1.0

0E+00 1E+09 2E+09 3E+09 4E+09Time (years)

Re

lati

ve

Va

lue

T/Tsun

R/Rsun

L/Lsun

cycle 17

L = 4πR2·σT4

Guzik + Field

Luminosity vs. Radius

0E+00

1E+33

2E+33

3E+33

4E+33

5E+33

6E+33

7E+33

8E+33

0E+00 2E+10 4E+10 6E+10 8E+10

Radius (cm)

Lu

min

osi

ty (

erg

s)

4.5 BY Z=0.01

3 BY Z=0.01

1.5 BY Z=0.01

ZAMS Z=0.01

4.5 BY Z=0.02

3 BY Z=0.02

1.5 BY Z=0.02

ZAMS Z=0.02

Guzik Field Lopez x70y28z02 112005

metal content influences solar luminosity and lifetime

Luminosity vs. RadiusX=.70, Y=.28, Z=.02

0E+00

1E+33

2E+33

3E+33

4E+33

5E+33

6E+33

7E+33

0E+00 2E+10 4E+10 6E+10 8E+10

Radius (cm)

Lu

min

osi

ty (

erg

s/s)

9 BY

7.5 BY

6 BY

4.5 BY

3 BY

1.5 BY

ZAMS


luminosity increases as core hydrogen is depleted

surfa

ce ra

dius

H Mass Fraction (X) vs. RadiusX=.70, Y=.28, Z=.02

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0E+00 2E+10 4E+10 6E+10 8E+10

Radius (cm)

X

ZAMS X

1.5 BY X

3 BY X

4.5 BY X

6 BY X

7.5 BY X

9 BY X


dhillon phy213 website

Equations of Stellar Structure

The Solid Earthsize of layersdensity, mass, gravity, pressure, volumecomposition – iron silicon oxygen magnesium nickel material propertiestemperaturethermal energy distributionheat flow sources

radioactive decay of U, Th, and Kheat loss as Earth coolsgravitational energy released as Earth coolslatent heat released as inner core freezes

energy transport: convection, conduction, radiationmass flow in convectionevolution of the Earth’s structureformation of the Earth

Zeroth order model of the Earth has three layers

core

mantle

core

mantle

crust

atmosphere

First order model of the Earth shows layersSeismic studies reveal density variations due to composition and phase differences.

ICB

CMB

inner core - conduction

outer core – convection?

lower mantle - convection

D” - conduction

upper mantle - convection

lithosphere - conduction

atmosphere - radiation

convection is powered by radiogenic heat sources and produces chemical evolution

Density (kg/m^3)

0

2000

4000

6000

8000

10000

12000

14000

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

Den

sity

(kg

/m^

3)

inner core R < 1221.5 km

outer core R < 3480 km

lower mantle R < 5701 km

D” R < 3630 km

upper mantle R < 6291 km

lithosphere R < 6371 km

ICB

CMB

Mantle

Core

Whole Earth Element Mass Percent

other5

Mg154

Si161

O297

Fe320

Cr5

Ni18

S6Ca

17

Al16

Fe

O

Si

Mg

Ni

Ca

Al

S

Cr

other

McDonough

Whole Earth, Crust, Mantle, Core Element Mass Percent

Fe85.5

O44

Si21

Mg22.8

Fe32.0

O29.7

Si16.1

Mg15.4

Ni5.2

Ca2.53

Al2.35

Fe6.26

Al8.41

Ca5.29

Fe7.07

O45.3Si

26.77

Mg3.2

Ni1.8

Ca1.7

Al1.6

Fe

O

Si

Mg

Ni

Ca

Al

S

Cr

Si6

Whole Earth CrustMantleCore

layers Fe O Si Mg Nicore 855 0 60 0 52mantle 63 440 210 228 2lithosphere 63 440 210 228 2whole Earth 320 297 161 154 18

layers Ca Al S Cr othercore 0 0 19 9 5mantle 25 24 0 3 6lithosphere 25 24 0 3 6whole Earth 17 16 6 5 5

zeroth order model - composition

Relative Mass Abundance of Elements on Earth

McDonough

Element Density (kg/m^3)

000E+00

2E+03

4E+03

6E+03

8E+03

10E+03

12E+03

14E+03

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

Ele

men

t D

ensi

ty (

kg/m

^3) boundaries

Fe

O

Si

Mg

Density (kg/m^3)

ICB

CMB Mantle

Core

based on McDonough

Major Elements in Crust and Mantle (%)(not counting oxygen)

0

5

10

15

20

25

30

Mg * Al * Si * Ca * Fe *

Elements

Maj

or

Ele

men

ts (

%) Crust

Upper Mantle

Lower Mantle

Crust + Mantle

Elements 2006-07-18 mfischer b revision

Temperature (K)

0

1000

2000

3000

4000

5000

6000

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

Tem

per

atu

re (

K)

boundaries

Temperature (K)

solidus temperature (K)

ICB

CMB

Liquid Outer CoreMantle

based on Stacey Appendix G

heat density (J/m^3)

000E+00

5E+09

10E+09

15E+09

20E+09

25E+09

30E+09

35E+09

40E+09

45E+09

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

hea

t d

ensi

ty (

J/m

^3) ICB

CMB

Mantle

Core

enclosed heat (J)

00E+0

2E+30

4E+30

6E+30

8E+30

10E+30

12E+30

14E+30

16E+30

18E+30

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

encl

ose

d h

eat

(J)

Mantle

Core

Stacey Table 6.4 Heat Loss Budget (TW)INCOME 8.2 Crust radioactivity19.9 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 loss30.8 Mantle heat loss 3.0 Core heat loss

42 TW TOTAL

10 TW NET LOSS OF HEAT

radiogenic heat flow (W)

00E+0

5E+12

10E+12

15E+12

20E+12

25E+12

30E+12

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

rad

iog

enic

hea

t fl

ow

(W

)

CMB

19.9 TW in mantle 8.2 TW in crust……28.1 TW whole Earth

Mantle

Core

based on Stacey

latent heat flow (W)

000E+00

1E+12

2E+12

3E+12

4E+12

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

late

nt

hea

t fl

ow

(W

)

ICBMantleCore

based on Stacey

4 BY

3 BY

2 BY

1 BY

total heat flow (W)

00E+0

5E+12

10E+12

15E+12

20E+12

25E+12

30E+12

35E+12

40E+12

45E+12

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

tota

l hea

t fl

ow

(W

)

boundaries

current total heat flow (W)

radiogenic heat flow (W)

current lost heat flow (W)

current ΔGBE heat flow (W)


CMB

Mantle

Core

relative heat flow

23 49

1000

809

617

0

200

400

600

800

1000

inner core outer core lowermantle

uppermantle

lithosphere

heat flow inocean crust

vs.continental crust?

layersinternal

energy (J )

heat sources

(W)total heat flow (W)

relative internal energy

relative heat

sourcesrelative

heat flowinner core 3.15E+29 9.85E+11 9.85E+11 19 23 23outer core 5.35E+30 1.11E+12 2.10E+12 315 26 49lower mantle 9.12E+30 2.43E+13 2.64E+13 537 568 617upper mantle 2.09E+30 8.22E+12 3.46E+13 123 192 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000continental crustocean crust

layersinternal

energy (J )

heat sources



relative heat

sourcesrelative

heat flowcore 5.67E+30 2.10E+12 2.10E+12 333 49 49mantle 1.12E+31 3.25E+13 3.46E+13 659 760 809lithosphere 1.20E+29 8.17E+12 4.28E+13 7 191 1000whole Earth 1.70E+31 4.28E+13 4.28E+13 1000 1000 1000

first order model – composition and phase


Absolute and Relative Energy, Heat, and Heat Flow


lithosphere7

lower mantle537

upper mantle123

outer core315

inner core19

relative mass

lithosphere21

lower mantle492

upper mantle162

outer core308

inner core17

relative volume

lower mantle554

upper mantle246

outer core156

lithosphere37

inner core7

relative total heat sources

lithosphere191

lower mantle568

upper mantle192

outer core26

inner core23

relative heat flow

23 49

1000

809

617

0

200

400

600

800

1000

inner core outer core lowermantle

uppermantle

lithosphere

layersvolume (m^3) mass (kg)

average density

(kg/ m^3)internal

energy (J )

heat sources


inner core 7.63E+18 9.83E+22 1.29E+04 3.15E+29 9.85E+11 9.85E+11outer core 1.69E+20 1.83E+24 1.08E+04 5.35E+30 1.11E+12 2.10E+12lower mantle 6.00E+20 2.92E+24 4.87E+03 9.12E+30 2.43E+13 2.64E+13upper mantle 2.67E+20 9.63E+23 3.61E+03 2.09E+30 8.22E+12 3.46E+13lithosphere 4.03E+19 1.25E+23 3.11E+03 1.20E+29 8.17E+12 4.28E+13whole Earth 1.08E+21 5.94E+24 5.48E+03 1.70E+31 4.28E+13 4.28E+13continental crustocean crust

layersvolume (m^3) mass (kg)

average density

(kg/ m^3)internal

energy (J )

heat sources


core 1.77E+20 1.93E+24 1.19E+04 5.67E+30 2.10E+12 2.10E+12mantle 8.66E+20 3.88E+24 4.24E+03 1.12E+31 3.25E+13 3.46E+13lithosphere 4.03E+19 1.25E+23 3.11E+03 1.20E+29 8.17E+12 4.28E+13whole Earth 1.08E+21 5.94E+24 5.48E+03 1.70E+31 4.28E+13 4.28E+13



Volume, Mass, Density, Energy, Heat, and Heat Flow

layersrelative volume

relative mass


relative heat

sourcesrelative

heat flowinner core 7 17 19 23 23outer core 156 308 315 26 49lower mantle 554 492 537 568 617upper mantle 246 162 123 192 809lithosphere 37 21 7 191 1000whole Earth 1000 1000 1000 1000 1000continental crustocean crust

layersrelative volume

relative mass


relative heat

sourcesrelative

heat flowcore 163 325 333 49 49mantle 800 654 659 760 809lithosphere 37 21 7 191 1000whole Earth 1000 1000 1000 1000 1000



Relative Volume, Mass, Energy, Heat, and Heat Flow

ru

ΔR

vmass

Δr

convection model for an ideal gasforce / area = viscosity x velocity gradient

constant P = (ρ-Δρ)k(T+ΔT)/mp

force = Δρ(πru2 ΔR)gR

cylinder area = 2πruΔR

Δρ(πru2 ΔR)gR/(2πruΔR) = η Δvmass/Δr

Δρ ru gR / 2 = η Δvmass/Δr

vmass = Δρ ru gR Δr / 2ηwhat if you have molten rocks?

Stacey318

Typical Cartoon of Mantle Convection and Plumes

Radiogenic Heat Flow (W)

0000E+00

20E+12

40E+12

60E+12

80E+12

100E+12

120E+12

-5 -4 -3 -2 -1 0Time (BY)

Rad

iog

enic

Hea

t F

low

(W

)

Total

U-235

K-40

U-238

Th-232

isotopeenergy/

atom (MeV)μW/kg of isotope

μW/kg of

element

estimated total Earth content (kg)

total heat

(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

40K 0.71 30 0.00357.14x1020 (total K)

2.5 30.2

total 28.1 117.3

Thermally important radioactive elements in the Earth

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)

0

1000

2000

3000

4000

5000

6000

0E+00 1E+06 2E+06 3E+06 4E+06 5E+06 6E+06 7E+06Radius (m)

Te

mp

era

ture

(K

)

boundaries

4 BYA

2 BYA

0 BYA

assume temperature changes linearly with time

Mantle

Core


000E+00

1E+12

2E+12

3E+12

4E+12

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6

radius (m)

late

nt

hea

t fl

ow

(W

)

ICBMantleCore

based on Stacey

now after 4 BY of freezing

2 BYA after 2 BY of freezing

before and after the Great Iron Catastropheenclosed GBE vs. volume

0.E+00

5.E+31

1.E+32

1.5E+32

2.E+32

2.5E+32

0.E+0 2.E+20 4.E+20 6.E+20 8.E+20 1.E+21 1.2E+21

volume (m3)

GB

E (

jou

les)

enclosed GBE (J)

"average density" enclosed GBE (J)

almost exactly

3GM2/5R

before and after the Great Iron Catastropheshell ΔT vs. volume

-40000

-20000

0

20000

40000

0.E+0 2.E+20 4.E+20 6.E+20 8.E+20 1.E+21 1.2E+21

volume (m3)

shel

l ΔT

(K

)

If iron accretes first, core is much hotter and mantle much cooler than if uniform composition

accretes. (if layers retain all GBE)

models of growth of continental volume (%)

4 3 2 1 0BYA

100

75

50

25

0

1992

geo

chem

ical

Van Andel

linear re

ference

1992 geochemicalBYA: % 0: 100 0.6: 90 2.6: 10 3.6: 0 4.5: 0

from VanAndel Fig. 13.6

The Atmospheresize of layersdensity, mass, gravity, pressure, volumecomposition – nitrogen oxygen water argon carbon dioxide aerosols material propertiestemperatureglobal energy budget and distribution – latitude season altitudeheat flow sources

absorbed sunlightEarth’s radiated energyair-sea interactions

energy transport: convection, conduction, radiationmass flow in convectionevolution of the atmosphere – composition structure density circulationorigin of the atmosphere

120

120

248

248

90902020

4848

surface

incidentshortwave flux

343

reflectedshortwave flux

21 69 16

outgoinglongwave flux

22 90 125

after Salby45, etc.

169 390 327 16 90

16

atmosphere

absorbedby clouds

absorbedby H2O, O3,

aerosols

reflectedby clouds

reflectedby surface

backscattered

by air

emittedby clouds

emittedby H2O, CO2,

aerosols

emitted bysurface

absorbedby clouds

absorbedby H2O, CO2,

aerosols

emittedby H2O, CO2,

aerosols

sensibleheatflux

latentheatflux

surface-atmosphereheat transfer

Average Global Energy Budget (W/m2)

169 + 327 = 496 surface 390 + 16 + 90 = 496

343 planet (21 + 69 + 16) + (22 + 90 + 125) = 343

(20 + 48) + (120 + 248 + 16 + 90) = 542 atmosphere (90 + 125) + 327 = 542

atmospheric composition (fraction by volume)

Water vapor (H2O) 0.01

Hydrogen (H2) 0.00000055

Oxygen (O2) 0.20946

Nitrogen (N2) 0.78084

Neon (Ne) 0.00001818

Krypton (Kr) 0.00000114

Carbon dioxide (CO2) 0.000381

Methane (CH4) 0.000001745

Argon (Ar) 0.00934

Helium (He) 0.00000524

Nitrogen (N2)

Oxygen (O2)

Argon (Ar)

Carbon dioxide (CO2)

Neon (Ne)

Helium (He)

Methane (CH4)

Krypton (Kr)

Hydrogen (H2)

Water vapor (H2O)

values are for dry airwater vapor is shown as

an additional 1% but varies enormously

compositionby mass?

Temperatureof the atmosphere

ocean

60 miles

50

40

30 miles

20

10

sea level

Thermosphere

Mesosphere

Stratosphere

Troposphere75% of air

Temperature vs. Altitude Sun

-130F

-70F 32F

60F

ozonelayer

After Tarbuck

temperature (K)

0

100

200

300

400

0 20000 40000 60000 80000 100000 120000

altitude (m)

temperature (K)

200

210

220

230

240

250

260

270

280

290

300

0 2000 4000 6000 8000 10000

altitude (m)

~6.6 K per kilometer

Density (kg/m3)

1E-4

1E-3

1E-2

1E-1

1E+0

0 10000 20000 30000 40000 50000 60000 70000 80000altitude (m)

Den

sity

(kg

/m3)

density (kg/m3)

calculated density (kg/m3)

~10X decrease per 15-20 km ascent

Calculated Enclosed Mass (kg)

0E+00

1E+18

2E+18

3E+18

4E+18

5E+18

0 10000 20000 30000 40000 50000 60000 70000 80000altitude (m)

En

clo

sed

Mas

s (k

g)

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

0

0.02

0.04

0.06

0.08

0.1

0.12

24201612840

Equator

midnight midnightNoon

EquinoxSolar Flux vs. Time of Day

Tropicof

Cancer

Arctic Circle

North Pole

6 am 6 pm

12108642240

0.02

0.04

0.06

0.08

0.1

0.12

NoonMidnight 6 am14 16 18 20 22 24

Noon Midnight6 pm

Summer SolsticeSolar Flux vs. Time of Day

Equator

Tropicof

Cancer

Arctic Circle

North Pole

absorption by ozone, water, and CO2

scattering by N2, O2 and aerosols

0.3 0.5 1 1.5 2 2.5 30

500

1000

1500

2000

Wavelength

Inte

nsit

yvisible

window

UV Visible Infrared

sun is directly overheadno clouds

direct beam only

Spectrum of Sunlight observed on Earth

Ultraviolet Average Flux at 35N on Summer Solstice

0

10

20

30

40

50

cda cma dda dmaatmospheres

Flu

x (W

/m^

2)Absorption LossesScattering LossesFlux at Surface

Field - solar flux code

CO2 and H2O gasesabsorb far infrared

2 Blackbodies1 Greenhouse

atmosphere transparentto visible light

EarthFar Infrared

Energy

10 micron peakEarth is 300K

Sun

0.5 micron peakSun is 6000K

VisibleSolar

Energy

0 5 10 15 20 25 300

50

100

150

200

250

300

Blackbody Radiation

Wavelength

Inte

nsi

ty

373Kwaterboils

5800Ksolar energyabsorbedby Earth

255Katmosphere

273Kwater

freezes

288K Earth's surface

0 5 10 15 20 25 300

5

10

15

20

25

30

Greenhouse Gases Absorb Blackbody Radiation

Wavelength (microns)

Inte

nsi

ty

O3

CO2

H2O255K

atmosphere

Plants 15%

Soil20%

Sand40%

Average Visible Reflectancesof common substances

Sun

Clouds 50%

Snow 60%

Water8%

12108642240

0.02

0.04

0.06

0.08

0.1

0.12

NoonMidnight 6 am14 16 18 20 22 24

Noon Midnight6 pm

Energy Transfer in a Day

What is the hottest time

of day?

heatgain

oceanheat loss land

heat loss

desertheat loss

atmospheric circulationbottom heated

absorbed heat peaks at Equator

no rotation with rotation

368368 106106

6868

surface


343


90 16

outgoinglongwave flux22 215

after Salby45, etc.

169 390 327 106

atmosphere

absorbed and reflected by

clouds, H2O, O3, aerosols

reflectedby surface

emitted bysurface

absorbed and emitted by

clouds, H2O, CO2, aerosols

latent and sensible heat

flux



169 + 327 = 496 surface 390 + 106 = 496

343 planet (90 + 16) + (22 + 215) = 343

(68) + (368 + 106) = 542 atmosphere (215) + 327 = 542

HW2B OASES HW #2B ©Bob Field 2006

incident SW flux W/m2 343 use global average

gas SW reflection 0.262

gas SW absorption 0.198

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

gas SW absorption W/m2 68 only absorbs from above

gas LW absorption W/m2 368

gas W/m2 436 not counting non-radiative flux

surface SW absorption W/m2 169

surface LW absorption W/m2 327 +LH+SH 0.603

surface W/m2 496 fill in E14 !!!

radiating flux W/m2 390

latent and sensible heat W/m2 106

surface temperature K 288

bonus

gas temperature K 248planet temperature K 254

SW is short wavelength as in sunlight. LW is long wavelength as in infrared radiated by the Earth.

LW down welling fraction

from gas to Earth

Hint - Be sure to account for all fluxes absorbed from all sources (except C10).

fra

ctio

n o

f u

nit

y

Use the information in the diagram of a simplified global energy budget model to fill in C2 -C 9 and cell E14. Every row is a fraction of unity except the first row. C14 depends on E14.

Use physics and common sense to construct equations for C10, C11, C13, C14, C16, C17, and C18.

368368 106106

6868

surface


343


90 16


after Salby45, etc.

169 390 327 106

atmosphere



reflectedby surface

emitted bysurface




flux



169 + 327 = 496 surface 390 + 106 = 496

343 planet (90 + 16) + (22 + 215) = 343

(68) + (368 + 106) = 542 atmosphere (215) + 327 = 542

343 use global average

=90/343

=68/343

=368/390

=16/(169+16)

=1-C6

=106/(169+327)

=1-C8

=C4*C2 only absorbs from above

=C5*C16

=C10+C11

=C7*(1-C3-C4)*C2

=E14*(C12+C17) +LH+SH =327/(327+215)

=C13+C14 fill in E14 !!!

=C15-C17

=C8*C15

=(C16/0.0000000567)^0.25

=((C12+C17)*(1-$E$14)/0.0000000567)^0.25

=(((C12+C17)*(1-$E$14)+(C16-C11))/0.0000000567)^0.25

Use the information in the diagram of a simplified global energy budget model to fill in C2 -C 9 and cell E14. Every row is a fraction of unity except the first row. C14 depends on E14.

368368 106106

6868

surface


343


90 16


after Salby45, etc.

169 390 327 106

atmosphere



reflectedby surface

emitted bysurface




flux



169 + 327 = 496 surface 390 + 106 = 496

343 planet (90 + 16) + (22 + 215) = 343

(68) + (368 + 106) = 542 atmosphere (215) + 327 = 542

The Oceanssize of layersdensity, mass, gravity, pressure, volumecomposition – water salt dissolved gases and organics particulates organismsmaterial propertiestemperatureglobal energy budget and distribution – latitude season altitudeheat flow sources

absorbed sunlightair-sea interactions

energy transport: convection, conduction, radiationmass flow in convectionevolution of the ocean – salt ice evaporation flow patterns depth areaorigin of the ocean

Elemental composition of sea water (by mass)

Oxygen 85.7

Hydrogen 10.8

Chlorine 1.9

Sodium 1.05

Sulfur 0.0885

Magnesium 0.135

Carbon 0.0026

Bromine 0.0065

Potassium 0.038

Calcium 0.04

Oxygen

Hydrogen

Chlorine

Sodium

Magnesium

Sulfur

Calcium

Potassium

Bromine

Carbon

wikipedia

Gas

N2

O2

CO2

Dry Air

78%

21%

0.036%

Sea Water

12 ppm

7 ppm

90 ppm

Ratio of TotalAmount in Ocean

to Atmosphere

0.004

0.01

62

Abundance ofDissolved Gases

H2O 0.3% 97% 100,000

global average of 40 inches of precipitation per year

recycles 120,000 cubic miles of water

percolation

precipitation

27

vapor transport10

groundwater flow

return flow10

precipitation

94

After Stowe

oceans hold340 M cubic miles

units - 1000 cubic miles/year

evaporation & transpiration

17 evaporation

104

from Stowe

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

Reservoirvolume of water

(106 km³)Percent of total

Oceans 1370 97.25Ice caps & glaciers 29 2.05

Groundwater 9.5 0.68Lakes 0.125 0.01

Soil moisture 0.065 0.005Atmosphere 0.013 0.001

Streams & rivers 0.0017 0.0001Biosphere 0.0006 0.00004

1408.7047

volume of stored water500 million square km area x 3 km depth = 1.5x109 km3

wikipedia

1.4x109 km3 volume x 1000 kg/m3 x 109 m3/km3 = 1.4x1021 kg

ReservoirAverage residence

time (years)Oceans 3,200 yearsGlaciers 20 to 100 years

Seasonal snow cover 2 to 6 monthsSoil moisture 1 to 2 months

Groundwater: shallow 100 to 200 yearsGroundwater: deep 10,000 years

Lakes 50 to 100 yearsRivers 2 to 6 months

Atmosphere 9 days

Average reservoir residence times

wikipedia

Ocean and Atmosphere simplified heuristic models1. 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?

Thermohaline (temperature- and salinity-controlled density) circulation of the oceans can be simplistically defined by a great conveyor belt. In this model, warm, salty surface water is chilled and sinks in the North Atlantic to flow south towards Antarctica. There, it is cooled further to flow outward at the bottom of the oceans into the Atlantic, Indian, and Pacific basins. After upwelling primarily in the Pacific and Indian Oceans, the water returns as surface flow to the North Atlantic. While traveling deep in the ocean the originally nutrient-depleted water becomes increasingly enriched by organic matter decomposition in important nutrients (e.g., phosphate, nitrate, silicate) and dissolved CO2. Figure courtesy of Jim Kennett and Jeff Johnson, University of California Santa Barbara.

http://seis.natsci.csulb.edu/rbehl/ConvBelt.htm

ocean conveyor belt

deep

deep

shallow

Ocean currents distribute nutrients and moderate temperatures by transferring tropical heat to arctic

Keith Stowe, Exploring Ocean Science

surface currents are driven by winds which result from non-uniform heating of the globe

pelagic zone(water column)

benthic zone

(seafloor)Ocean Zonespelagic / benthic sediments

sedimentsplankton& nekton

Sun

photic zone(light)

aphotic zone(dark)

Ocean Zonesphotic / aphotic

Sun

V B G Y O R IRUV

10% 50' 0' 300' 40' 15' 2'

photic zone(light)

aphotic zone(dark)


benthic zone

(seafloor)Ocean Zonespelagic / benthic

photic / aphotic

Sun

photic zone(light)

aphotic zone(dark)

neritic province(above continental shelf)

oceanic province(beyond continental shelf)


benthic zone

(seafloor)Ocean Zonespelagic / benthic

photic / aphotic

neritic / oceanic

Nereus & 50 Nereid

Sun

space and Sun

atmospherewater world

“continental crust”oceanic crust

photic zone(light)

aphotic zone(dark)


benthic zone(seafloor)

Sun

intertidalorlittoral zone

atmosphere

ocean

continental crust

oceanic crust

sediments

sediments

Sun

atmosphere

ocean

continental crust

sediments

sediments upwelling

Sun

blackbody radiation reduced by inverse square

distance

atmospheric absorption and scattering losses

reflection losses and refraction at air-sea surface

seawater absorption and scattering losses

horizontal receiving surface

stellar temperature

stellar radius

radius of planetary

orbit

wavelengths

polarizations

atmospheric composition: absorbers &

scatterers

flux above atmosphere

flux above sea surface

flux spectrum incident on horizontal surface

flux spectrum absorbed in last meter

flux spectrum scattered in last meter

flux reflected by air-sea interface

SolarSeaFlux Flow Chart

transmission angle

seawater composition: absorbers &

scatterers

incidence angle

seawater depth

©Bob Field 2003

300 350 400 450 500 550 600 650 700 750 8000.01

0.1

1

1010

0.01

0( )

0( ) 0( )

p 1( ) 0( ) 0( )( )

y 2( ) 0( ) 0( )( )

g 3( ) 0( ) 0( )( )

air ( ) air ( )

air ( ) air ( ) 0( ) 0( )( )

21

Field - solar sea flux code

absorption and scattering coefficients of air and water

actual curves of components depend on concentrations

300 350 400 450 500 550 600 650 700 750 8000

0.2

0.4

0.6

0.8

max

0

Tz z k 0 Hy ( )

21 Hx ( )

Field - solar sea flux code

transmitted sunlight in pure water vs. depth(0, 1, 3, 10, 30, 100 meters)

zone areas

1.0E+14

1.3E+14

2.1E+13

2.6E+14

3.1E+13 3.1E+13 1.8E+12

6.4E+13

0E+00

1E+14

2E+14

3E+14

torrid temperate frigid hemisphere

surface area (m2) disk area (m2)

zone temperatures

269250

195

255

361 353

287

361

0

50

100

150

200

250

300

350

400

torrid temperate frigid hemisphere

average temperature (K) noon peak temperature (K)

required latitudinal heat outflow (W)

0E+00

1E+15

2E+15

3E+15

4E+15

5E+15

6E+15

7E+15

0 10 20 30 40 50 60 70 80 90

latitude (degrees)

hypothetical air speed or water speed (m/s)

0.0

0.5

1.0

1.5

0 10 20 30 40 50 60 70 80 90

latitude (degrees)

air speed (m/s)

water speed (m/s)

waterdelta T = 10 K

10 m deep columndensity = 1000 kg/m3

specific heat = 4186 J/kg-K

airdelta T = 40 K

4000 m high columndensity = 1.228 kg/m3

specific heat = 1000 J/kg-K

water 1/mfp (1/m) vs. wavelength

1E-2

1E-1

1E+0

1E+1

1E+2

1E+3

1E+4

300 400 500 600 700 800 900 1000 1100 1200 1300 1400

wavelength (nm)

flux absorbed per meter vs. depth (m)

0

50

100

150

200

0 5 10 15 20 25 30

depth (m)

Flu

x ab

sorb

ed p

er m

eter

(W

/m3)

Organismsand

Ecosystems

ocean

sediments

sediments60 tons of organic matter in ocean is

dissolved organic molecules(yellow matter)

one ton of organic matter in ocean isparticulate

1700 pounds of particulate is detritus

240 pounds phytoplankton 60 pounds zooplankton

1 pound of large animals

after Stowe

Sun

ocean

sediments

sediments98.3% of all organic matter in ocean is

dissolved organic molecules = 2000 gC/m2

1.7% of all organic matter in ocean isparticulate = 35 gC/m2

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

after Stowe

Sun

one million land animal species(75% insects)

4,000pelagicanimalspecies

200,000 ocean animal species(98% benthic)

Distribution of Animal Species

Plant Production

Upwelling

Coa

stal

wat

ers

OpenOcean

Land

after Keith Stowe, Exploring Ocean Science

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)

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.

Ocean Fish Production

Open Ocean

Coastal

Upwelling

Tjeerd van Andel, Science at Sea: Tales of an Old Ocean

0

50

100

150

200

Ocean FishProductivity/Area

Up

wel

ling

Coastalwaters

OpenOcean

0

25

50

75

100

125

150

175

200

Plant Productivity/AreaU

pw

ellin

g

Coastalwaters

OpenOcean

Land

from Stowe & Thurman

*before sinking below the photic zone

recycles per year

steps of bacterialdecompostion*

considerations

requirement

10

3

4

1

nitrogen

15

phosphorus

1

universe 200 1

oceans 6 1

Seasonal Abundance of Sunlight,Nutrients, Phytoplankton, Grazers

SunlightGrazers

Phytoplankton

Nutrients

Jan Feb March April May June July Aug Sept Oct Nov Dec

After Stowe 276

productivity (gC/m2/day)

continentalshelf

centralocean

high latitudes

Jan Feb Mar Apr May June July Aug Sep Oct Nov Dec

0.9

0.6

0.3

0

afte

r K

eith

Sto

we,

Exp

lori

ng

Oce

an S

cien

ce

temperate

continentalshelf

centralocean

Jan Feb Mar Apr May June July Aug Sep Oct Nov Dec

0.9

0.6

0.3

0

afte

r K

eith

Sto

we,

Exp

lori

ng

Oce

an S

cien

ce

productivity (gC/m2/day)

annual carbon cycle in the atmosphere

ocean

110

109

90

93

+1

+3billions of tons of carbon

Sun

7

-7

where is the carbon?(billions of metric tons)

ocean

Sun

from Biology of plants 5th Ed. by Raven et al. page 115

sediments20,000,000

deep ocean38,000,000

carbon dioxide gasin atmosphere 700

Dissolved organic matter ~2000humus2000

fossil fuels5000?

photosynthesis removes4 billion tons of carbonfrom atmosphere per year

dissolved gas 40,000

Moleculesand

Cells

What do cells do?

Store, exchange, and transform: matterenergy

information

Modern cells are chemical factories: complex, highly efficient, self-replicating.

Cells store and release energy to build up and break down biomolecules...

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

The cell is the building block of life.All cells are descended from cells.

The natural selection of molecules is the essence of the origin and evolution of life.

Trefil and HazenThe Sciences:

An Integrated Approach

5 kingdoms:bacteria

algaefungusplant

animal

What are the building blocks of molecules?

A, B, and C are all about 97% CHO

OC SH N P

Life’s Origin page 15by Walter Schopf A B C

Hydrogen 61 63 56

Oxygen 26 29 31

Carbon 10.5 6.4 10

Mammal

Nitrogen 2.4 1.4 2.7

Sulfur 0.13 0.06 0.3

Phosphorus 0.13 0.12 0.08

Calcium 0.23 - -

Bacteria Comet

H

H

O

O

O

O

P

N

NC H

H

H

H

C

O

O

SH

H

N

H

HH O ON

OO

H

H

O

O

OC SH N P

many common molecules are made from CHONSP

C

O

S

Methane can form new molecules O

H C H

H

H

O

methanolmethane

formaldehyde

formic acid biochemists give big names to

small molecules

OH C H

H

H

OH C H

H

H

C

H

H

C C C C C C C C C C CH N

CC CH N

C

H

H OH

H

H

H

C OC

CH N

CC NNC

H

N

H

N

CHONSP molecules are abundant in space:100 tons per year of IPDs land on Earth

(interplanetary dust particles) Cradle of Life pages 133-5 by William Schopf

C

H

H S

Organic molecules have many variations on a few themes

backbone of

phospholipid (H and O not shown)

CO, H2, PO4 are building blocks of phospholipids found in cell membranes

RC C C C C C C C

PiC C C C C

CC

C

fatty membrane spheresform naturally in meteors

C

H

O

HC

H

C

H O

C

H

H

OC

H

H

O

H

H

O

C

H

H

O

C

H

H O C

H

H O

C

H

H O

C

H

H O

C

H

H O C

H

H O

6 CH2O+ energy+ catalyst

C

O

C

H

O

C H

H

O

glucose is a building block of carbohydrates

glucose

C

H

O

HC

H

C

H O

C

H

H

OC

H

H

O

H

H

O

C

H

H

O

Sunlight

photosynthesis makes glucose from sunlight, carbon dioxide, and water

C

O H

H

O

O

6 H2O

H

H

O

H

H

O H

H

O

H

H

O H

H

O

C

O

O

C

O

O

C

O

O

C

O

O

C

O

O

6 CO26 O2glucose

C

O

C

H

O

C H

H

O

C

O

C

H

O

C H

H

O

glucose supplies energy to make ATP

C3H3O3

C

H

O

HC

H

C

H O

C

H

H

OC

H

H

O

H

H

O

C

H

H

O

C3H3O3

glucose

ATP

ATP

aerobic fermentation makes 2 more ATP

ATP

ATP

C

H

O

HC

H

C

H O

C

H

H

OC

H

H

O

H

H

O

C

H

H

O

respiration liberates energy by oxidizing glucose into .... .

O

O

O

O

O

O

O

O

O

O

O

O

6 O2glucose

C

H

O

HC

H

C

H O

C

H

H

OC

H

H

O

H

H

O

C

H

H

O

respiration liberates energy by oxidizing glucose into carbon dioxide and water

C

O H

H

O

O

6 H2O

H

H

O

H

H

O H

H

O

H

H

O H

H

O

C

O

O

C

O

O

C

O

O

C

O

O

C

O

O

6 CO2

ATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATPATP ATP ATP ATP

C

H

O

H C

H

C

H O

C

H

H

OC

H

H O

H

H

O

C

H

H

O

C

H

H O C

H

H O

C

H

H O

C

H

H O

C

H

H O C

H

H O


fructose is an isomer of glucose: table sugar forms by joining them

G G G G G G G

G F

simple sugar building blocks combine to form carbohydrates

when water is squeezed out

table sugar

cellulose

H2O

H2O H2O H2O H2O H2O H2O

C

H

H

O

C

H

H

O

C

H

H O

C

H

H

O

C

H

H

O

ribose is a building block of ATP, RNA..

C

H

H O C

H

H O

C

H

H O

C

H

H O

C

H

H O


deoxyriboseribose

H

N

N NCN

C HC

H

C

H

CHN

CH N

CH N

nucleic acids are building blocks for energy and information in ATP, RNA...

CH N

CH N CH N

5 HCN+ energy+ catalyst

adenine

RPiPi Pi

Nucleotides are combinations of nucleic acids,

ribose sugar, and inorganic phosphate

A

PiPi Pi

RH2O

H2O

UGCT

D

triphosphates transport energy for transfer RNAs, membrane synthesis, and sugar synthesis.

monophosphates relay signals within a cell

nucleotide building blocks combine to form RNA and DNA

when water is squeezed out

R

A

Pi R

U

Pi R

C

Pi R

A

Pi R

G

Pi

H2O H2O H2O H2O

C

H

H

O

C

H

H

O

C

H

H O

C

H

H

O

C

H

H

O

OC

H

N

O

CH

H

H

H

CH N

amino acids are readily made fromsimple molecules by adding energy

C

H

H O

O

H

Hwater

formaldehyde

hydrogen cyanide

glycine

OC

H

N

O

CH

H

H

H

CH N

amino acids are readily made fromsimple molecules by adding energy

C

R

H O

O

H

Hwater

“R”-aldehydehydrogen cyanide

genericamino acid

OC SH N

amino acids are building blocks of proteins that function as enzymes and structures

OC

H

N

O

CH

H

H

H

C

OC

H

N

O

CH

H

H

H

H H

C

N

C

OC

H

N

O

CH H

H

H H

C

C

CC

CC

C

H

H

HH

HH

all 20 amino acids have the same backboneand all have H and OH on the ends

ribosomes synthesize proteins by translating mRNA to tRNAs that are attached to amino acids

21

A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A

3 4 5 6 7 8 9

A C UC C UG A UG C UC A GU G UC A AA U AC G CG U A

H2O H2OH2O H2O H2O H2O H2O H2O

after Trefil and HazenThe Sciences:


not necessarily an intelligent designribosomes reuse tRNA and mRNA

A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G AA C UC C UG A UG C UC A GU G UC A AA U AC G CG U A



AlaHis Tyr Val Thr Val Arg Leu GlyH2O H2O

H2O H2O H2O H2O H2O H2O

some of the 20 amino acids are represented by more than one of

the 64 triplet codons

Catalysts are vital to many processes:Proteins help produce complex molecules



Modern cellular processes are highly regulated

DNA+RNA+Protein WorldRNA+Protein World

RNA World

Peptide (PNA) World?Thioester World?

Clay World?

Which self-replicating molecules came first?

no record of early biochemistry

Molecular and metabolic evolution may be relatively simple and rapid

Chance affects diversity and abundanceNecessity provides natural selection

All inheritable biological changes are based on molecular evolution

D

A

Pi D

T

Pi D

C

Pi D

A

Pi D

G

Pi

mRNA provides the message to link amino acids into proteins


How does a computer “design” its own software?

AlaHis Tyr Val Thr Val Arg Leu Gly

1

52 321


How does information evolve?

21 3 4

2 3

21 3

21 3

4 5

duplication

4 5

1

52 321


How does information evolve?

21 3 4

2 321 3 21 3

deletion and insertion

AlaHis Tyr Val Thr Val Arg Leu Gly

D

A

Pi D

T

Pi D

C

Pi D

A

Pi D

G

Pi

RC C C C C C C C

Pi

C C C C CC

CC

C

HO

HCH

C

H O

C

H

H

OC

H

H

O

H

H

O

CH

HO

R

A

Pi Pi Pi

CN

C

OCH

N

O

CH H

H

H H

C

C

CC

C C

CH

H

HH

HH

21

A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G AC G CG U A

The Facts of LifeAll 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

All cells descended from a last common ancestor

The first cells came from non-cellular materials and were much simpler than any modern cells

http://www.its.caltech.edu/~atomic/snowcrystals/photos/photos.htm

Let me be crystal clear:

Complex patternsdo not require

intelligent designers!

Eukaryotes are world champs of multicellularity and cell differentiation

Identical cells differentiate to develop into a multicellular organism

Identical Cells Multiply by Dividing

Last common ancestor appearsLCA branches into

archaebacteria, eubacteria, and eukaryote predecessors

metabolic processes diversifyautotrophs evolve

hot The first eukaryote grew 10,000 times larger than

other bacteria because its membrane lost its cell wall.

methane

hotter salt

sun

sulfur

bacteria

archaeaeucarya

LCA

lateral and vertical gene transfer proto

cell

protocells feed on moleculesreplication processes evolvemetabolic processes evolve

Eukary

a

ArchaeaBacteria

Eukarya

Multicellularity(the labeled branches)evolved independentlya number of times

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.

Archaea

Bacteria

Animals

Fungi

Red algaeGreen algaePlants

Brown algaeDiatoms

CiliatesSorogena

MyxomycetesCellular slime molds

Foraminifera

MethanosarcinaMyxobacteria

Cyanobacteria

Actinomycetes

lastcommonancestor

2

8

32

128

2

4

8

16

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