Life on Our Evolving Planet slides

Life on Our Evolving Planetoptical physicist in aerospace for twenty years

designed and analyzed laser optical systems

Informal science educator in Morro Bay State ParkMuseum of Natural History for ten years

5 global evolution walks in parks12 animated slide shows in museum3 poster exhibits in museum and at Cal Poly

Cal Poly adjunct physics professor for seven yearsand research scholar in residence

4 senior projects Phys 461-4648 summer student projects13 special problems projects (Phys, Geol, Bio, Chem 200 or 400)Phys470 Advanced Topics: Solar and Global Evolution

visit my website at www.calpoly.edu/~rfield

Bob Field

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

What is a system?

Is the system open or closed?

a system has parts that interactand may have emergent properties

Dr Art Sussman’s Guide to Planet Earthenergy flows, matter cycles, web of life

energy

matter

energy

matter

How did a giant cloud of cold dilute gas and

dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star?

The ultimate question for Earth System History is:

Life on Our Evolving Planet

The National Academy of Sciences says thatit is the role of science to provide

plausible natural explanations of natural phenomena

Simple building blocksevolve into complex systems

when energy flowsEverything Evolves

oceans and atmospheresolid Earth and Sunmolecules and cells

organisms and ecosystems

C6 12

N7 14

O8 16

H1 1

He2 4Periodic Table of

Chemical Elements

92% ~8%0.07%0.04%0.02%0.01%

Abundance in Universe in %0.1% }

Ne10 20

Na11 23

Mg12 24

Al13 27

Si14 28

P15 31

S16 32

Cl17 35

Ar18 40

K19 39

Ca20 40

Cr24 62

Mn25 55

Fe26 56

Ni28 59

0.02% everything else

Big stars build big atomsSunlight is the waste product

Sun fuses 4 H1 → He4

composition in our LANL solar evolution code

sunsolar composition

"metals", 1

Helium, 28

Hydrogen, 71

solar "metals" composition

Nitrogen, 7.0

Magnesium, 5.0other, 1.3

Carbon, 22.9Oxygen, 63.9

composition by mass

about 93% CHO by mass

ancient atmosphere ??? 2CO2+CH4+NH3+4H2O

Carbon, 18.7

Nitrogen, 7.3

Oxygen, 66.3

Hydrogen, 7.8

Simple building blocks

comet volatiles composition

Nitrogen, 5.2

Sulfur, 1.3 Phosphorus, 0.3

Carbon, 16.6

Hydrogen, 7.8

Oxygen, 68.7

about 97% CHO by mass

Complex Systems

bacteria composition

Oxygen, 73.8

Hydrogen, 10.0

Carbon, 12.2

Nitrogen, 3.1Sulfur, 0.3

Phosphorus, 0.6

mammal composition

Hydrogen, 9.3

Oxygen, 63.6

Carbon, 19.3

Calcium, 1.4

Nitrogen, 5.1

Phosphorus, 0.6Sulfur, 0.6

wikipedia

elemental composition of the ocean and the atmosphere

seawater

Hydrogen, 10.8

Oxygen, 85.7

Sodium, 1.05Chlorine, 1.9

Carbon, 0.0026other, 0.308

atmosphere

Carbon, 0.01

Nitrogen, 78

Argon, 1.1

Oxygen, 20.9

Hydrogen, 0.01

composition by mass

McDonough

Elemental Composition of the Earth

whole EarthSulfur, 0.6

Chromium, 0.5

Calcium, 1.7other, 0.5Aluminum, 1.6

Silicon, 16.1

Magnesium, 15.4

Nickel, 1.8

Oxygen, 29.7

Iron, 32

Continental Crust

Calcium, 5.29

other, 4Aluminum, 8.41

Silicon, 26.77

Magnesium, 3.2

Oxygen, 45.3

Iron, 7.07

composition by mass

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

HN

H

N

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

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

C

H

H S

Organic molecules have many variations on a few themes

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

all cells are descended from a common ancestor

What do cells do?

Modern cells are chemical factories that store, exchange, and transform

matter, energy, and information

prokaryote

eukaryote

5 kingdoms:bacteria

algaefungusplant

animal

energy

matter

energy

matter

What are the building blocks of molecules?

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

OC SH N PLife’s Origin page 15

by Walter Schopf A B CHydrogen 61 63 56Oxygen 26 29 31Carbon 10.5 6.4 10

Mammal

Nitrogen 2.4 1.4 2.7Sulfur 0.13 0.06 0.3

Phosphorus 0.13 0.12 0.08Calcium 0.23 - -

Bacteria Comet

composition by number of atoms

atoms can share or transfer electronsH – 1He – 0O – 2C – 4N – 3S – 2

P – 3 or 5

H

H

O

O

O

O

P

N

NC H

H

H

H

C

O

O

SH

H

N

H

HH O ON

OO

H

H

O

O

OC SH N P

many common molecules are made from CHONSP

C

O

S

Methane can form new molecules O

H C H

H

H

O

methanolmethane

formaldehyde

formic acid biochemists give big names to

small molecules

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 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

low tide in Corallina Cove - Montana de Oro

Bob Field 2000

Moon

core

lower mantle

upper mantle

oceanic lithosphere

oceaniccrust

oceans

biosphere

atmosphere

subcontinentallithosphere

sedimentslower crust

upper crust

impactsInteractions

between Earth systems

Condie33Fig 1.33

sunw

hen

ener

gy fl

ows,

com

plex

ity g

row

s

Solar and Global Evolutionare parts of Cosmic Evolution

generic system average power density (W/kg)

galaxies 0.00005stars 0.0002

planets 0.01plants 0.1

animals 2brains 15society 50

table from Chaisson139 when energy flows, complexity grows

The Facts of Life: From the Oceans to the Stars

I. Oceans and Atmosphere Evolve 1. Voracious Predators 2. Luke Skylighter and Dark Weighter 3. Fire and Ice

II. The Solid Earth and Sun Evolve 4. Toxic Flying Insects 5. Global Cooling 6. Solar Heating

III. The Biosphere Evolves 7. Bacteria and Viruses 8. Gaia and Hypersea 9. Asteroids and Astronauts

IV. Intelligent Life Evolves 10. Cosmo Sapiens 11. Sustainability 12. The Quest for HOPE

Appendices A. Five Billion Year Global Evolution Timelines B. Earth Systems Database

1. Oceans and Atmosphere 2. Sun and Solid Earth 3. Biosphere

©Bob Field 2007

The National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? Global evolution studies explore five kingdoms of life and the five billion years of physical, chemical, and biological evolution that have shaped the solid Earth, hydrosphere, atmosphere, and biosphere (including its molecules, cells, organisms, and ecosystems).

This is the dust cover of a book that I want to write.

I have been researching the subject for years.

I am seeking students and faculty to help me develop a

global evolution website featuring:

1. a five-billion-year timeline of globally important events in 100 million year intervals

2. a database of properties and processes of the Sun and the Earth and its subsystems

3. time dependent math models of solar and global system structures and flows of energy and material

4. constructivist thematic educational resources for students, educators, and the public

Global Evolution: The First Five Billion YearsThe National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? The short answer is when energy flows, complexity grows.The fact is that the solid Earth, hydrosphere, atmosphere, and biosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems, a process that I call global evolution. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of a complex natural system.

Solar SystemSun

Solid Earth

HydrosphereAtmosphere

Geobiosphere

Molecules and CellsOrganisms and Ecosystems

AstronautsGlobal Evolution Timelines Earth Systems Data Base

The Structure and Evolution of the Solar System including the Sun and the Solid Earth

The first section investigates the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of the solar system including the Sun and the Solid Earth.

Solar System Sun Solid Earth

The Structure and Evolution of the Hydrosphere, Atmosphere, and Geobiosphere

The fact is that the hydrosphere, atmosphere, and geobiosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems, a process that I call global evolution. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of these global systems.

Hydrosphere Atmosphere Geobiosphere

percolation

precipitation

27

vapor transport10

groundwater flow

return flow10

percolation

precipitation

27

vapor transport10

groundwater flow

return flow10

precipitation

94

precipitation

94

After Stowe

oceans hold340 M cubic miles

units - 1000 cubic miles/year

evaporation & transpiration

17 evaporation

104


17 evaporation

104

Average Global Energy Budget

50

100

20

30

incidentsunlight

absorb

scatteredsunlight

absorb

sea + land

atmosphere

Sun

30

30

evap

condense

90

65

155

absorb

radiate

radiate

5

110

105

radiate

absorb

radiated heatLWIR

30

30

evap

condense

90

65

155

absorb

radiate

radiate

5

110

105

radiate

absorb

radiated heatLWIR

The Structure and Evolution of molecules, cells, organisms, ecosystems, and even astronauts

How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting a star? The short answer is when energy flows, complexity grows.The fact is that the solid Earth, hydrosphere, atmosphere, and biosphere have undergone nearly five billion years of physical, chemical, and/or biological evolution because of the flows of energy and/or matter into and/or out of these systems. Each section addresses the structures, functions, composition, interactions and flows of energy and matter, and origin and evolution of a complex natural system.

Molecules and Cells Organisms and Ecosystems Astronauts

A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G AA C UA C UC C UC C UG A UG A UG C UG C UC A GC A GU G UU G UC A AC A AA U AA U AC G CC G CG U AG U A

after Trefil and HazenThe Sciences:

An Integrated Approach

AlaHis Tyr Val Thr Val Arg Leu GlyH2OH2O H2OH2O

H2OH2O H2OH2O H2OH2O H2OH2O H2OH2O H2OH2O

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

Global Evolution Timelines:Can you identify and sequence the globally important events in the natural history of the oceans, atmosphere, solid Earth, Sun, molecules, cells, organisms, and ecosystems?

from MY

to MY MYA Era

oceans 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

Prot

eroz

oic

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

Had

ean

Pre-Hadean

Arc

haea

n

Earth Systems Database: The SunThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.

Solar Evolution

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1.0

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

Rel

ativ

e Va

lue

T/Tsun

R/Rsun

L/Lsun

cycle 17

relative volume

fusion core 16

radiative zone 343

convective zone 641

relative mass

fusion core 481radiative

zone 492

convective zone 27

relative heat flow

1000988 1000

0

200

400

600

800

1000

fusion core radiative zone convective zone

relative total energy

radiative zone 356

fusion core 637

convective zone 7

relative fusion power

convective zone 0

fusion core 988

radiative zone 12

Sun layers volume (cm3) mass (g)average density (g/ cm3)

relative volume

relative mass

relative average density

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

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

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

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

layerstotal

energy (ergs)

fusion power

(erg/ s)

luminosity (erg/ s)

relative total

energy


relative heat flow

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

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

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

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

layers volume (cm3) mass (g)average density (g/ cm3)

relative volume

relative mass


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



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 heat flow

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



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

Earth Systems Database: The Solid EarthThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.

layersinternal

energy (J )

heat sources

(W)total heat flow (W)

relative internal energy

relative heat

sourcesrelative

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

layersinternal

energy (J )

heat sources



relative heat

sourcesrelative

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

layersvolume (m^3) mass (kg)

average density

(kg/ m^3)relative volume

relative mass


inner core 7.63E+18 9.83E+22 1.29E+04 7 17 2348outer core 1.69E+20 1.83E+24 1.08E+04 156 308 1977lower mantle 6.00E+20 2.92E+24 4.87E+03 554 492 889upper mantle 2.67E+20 9.63E+23 3.61E+03 246 162 658lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000continental crustocean crust


average density


relative mass


core 1.77E+20 1.93E+24 1.19E+04 163 325 2162mantle 8.66E+20 3.88E+24 4.24E+03 800 654 773lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000

layersinternal

energy (J )

heat sources



relative heat

sourcesrelative


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


average density


relative mass




average density


relative mass


core 1.77E+20 1.93E+24 1.19E+04 163 325 2162mantle 8.66E+20 3.88E+24 4.24E+03 800 654 773lithosphere 4.03E+19 1.25E+23 3.11E+03 37 21 567whole Earth 1.08E+21 5.94E+24 5.48E+03 1000 1000 1000


lithosphere7

lower mantle537

upper mantle123

outer core315

inner core19

relative mass

lithosphere21

lower mantle492

upper mantle162 outer core

308

inner core17

relative volume

lower mantle554

upper mantle246

outer core156

lithosphere37

inner core7

relative total heat sources

lithosphere191

lower mantle568

upper mantle192

outer core26

inner core23

relative heat flow

23 49

1000

809

617

0

200

400

600

800

1000

inner core outer core lowermantle

uppermantle

lithosphere

models of growth of continental volume (%)

4 3 2 1 0BYA

100

75

50

25

0

1992 g

eochem

ical

Van Andel

linear reference

1992 geochemicalBYA: %

0: 1000.6: 902.6: 103.6: 04.5: 0

4 3 2 1 0BYA

100

75

50

25

0

1992 g

eochem

ical

Van Andel

linear reference


0: 1000.6: 902.6: 103.6: 04.5: 0

4 3 2 1 0BYA

100

75

50

25

0

1992 g

eochem

ical

Van Andel

linear reference


0: 1000.6: 902.6: 103.6: 04.5: 0

from VanAndel Fig. 13.6

Radiogenic Heat Flow (W)

0000E+00

20E+12

40E+12

60E+12

80E+12

100E+12

120E+12

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

Rad

ioge

nic

Hea

t Flo

w (W

)

TotalU-235K-40U-238Th-232

Earth Systems Database: The HydrosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.

Percent of total

97.25

2.050.68

0.01 0.0050.001

0.0001 0.000040.000010.00010.0010.010.1

110

100

Oce

ans

Ice

caps

&gl

acie

rs

Gro

undw

ater

Lake

s

Soil

moi

stur

e

Atm

osph

ere

Stre

ams

&riv

ers

Bio

sphe

re

reservoir

stored water

wikipedia

average rate (10³ km³/year)

10771 36

398434

0

100

200

300

400

500

Precipitationover land

Evaporationfrom land

Runoff &groundwater

from land

Precipitationover oceans

Evaporationfrom oceans

water fluxwikipedia

transmission vs. depth

0

50

100

150

200

250

300

350

0 1 3 10 30 100depth (m)

pure

particulate

DOM

chlorophyll

Field - solar sea flux code

300 350 400 450 500 550 600 650 700 750 8000

0.2

0.4

0.6

0.8

max

0

Tz z k 0 Hy ( )

21 Hx ( )

Field - solar sea flux code

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

Earth Systems Database: The AtmosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.

Average Flux for Clean, Dry Air at 35 N

0

100

200

300

400

500

Total UV Visible Infrared

0.3-3.0 0.3-0.4 0.4-0.7 0.7-3.0Spectral Band (microns)

Flux

(W/m

^2)

Scattering Losses

Absorption Losses

Flux at Surface

Field - solar flux code

cloudfree sky

12108642240

0.02

0.04

0.06

0.08

0.1

0.12

NoonMidnight 6 am14 16 18 20 22 24

Noon Midnight6 pm

Summer SolsticeSolar Flux vs. Time of Day

EquatorEquator

Tropicof

Cancer

Tropicof

Cancer

Arctic CircleArctic Circle

North PoleNorth Pole


50

100

20

30

incidentsunlight

absorb

scatteredsunlight

absorb

sea + land

atmosphere

Sun

30

30

evap

condense

90

65

155

absorb

radiate

radiate

5

110

105

radiate

absorb

radiated heatLWIR

30

30

evap

condense

90

65

155

absorb

radiate

radiate

5

110

105

radiate

absorb

radiated heatLWIR

Thermal Structure of Troposphere

0123456789

10

210 220 230 240 250 260 270 280 290 300 310 320Temperature (K)

altit

ude

(km

)

downwelling temperature (K)upwelling temperature (K)

Salby237

Earth Systems Database: The BiosphereThese databases document the structures, functions, composition, interactions and flows of energy and matter in the Sun, solid Earth, hydrosphere, atmosphere, and biosphere.

carbon (Gt) on a logarithmic scale

1E+0

1E+1

1E+2

1E+3

1E+4

1E+5

1E+6

1E+7

1E+8

1E+9

Atmosp

here

CO2 (at

pre-in

dustr

ial 28

0 ppm

v)

Ocean

Dissolv

ed in

organ

ic (D

IC)

Dissolv

ed or

ganic

(DOC)

Particu

late o

rganic

(POC)

Ocean b

iota

Land b

iota

Phyto

mass

Bacter

ia an

d fun

gi

Land A

nimals

Land

Soil h

umus

Reacti

ve fr

action

of hu

mus

Dead or

ganic

matt

er, lit

ter, p

eat

Inorga

nic so

il (CaC

O3)

Sedim

ents

Carbon

ate se

dimen

ts

Organic

matt

er sed

imen

ts

Contin

ental

crust

Oceanic

crust

Upper

mantle

Flux Carbon Gt/year

gross primary production 203from atmosphere to land biota 110

from ocean to ocean biota 93respiration 89.5

from land biota to atmosphere 46.9from ocean biota to ocean 42.6

Net primary production (NPP) 113.5from atmosphere to land biota 63.1

from ocean to ocean biota 50.4Volatilization from soil organic matter to atmosphere 62.5Net exchange from atmosphere to land 0.6Weathering consumption of CO2 from atmosphere to sediments 0.26Net exchange to atmosphere from ocean 0.51

dissolution from atmosphere to ocean 96evasion to atmosphere from ocean 96.51

River input of dissolved C (DIC + DOC) to ocean 0.6DIC 0.38DOC 0.22POC 0.19PIC 0.18

Oceanic sediment long-term storage 0.28Carbonates 0.22

Organic matter 0.06Volcanism, metamorphism, hydrothermal from land to atmosphere 0.22Uplift 0.4

bacteria composition

Oxygen, 73.8

Hydrogen, 10.0

Carbon, 12.2

Nitrogen, 3.1Sulfur, 0.3

Phosphorus, 0.6

mammal composition

Hydrogen, 9.3

Oxygen, 63.6

Carbon, 19.3

Calcium, 1.4

Nitrogen, 5.1

Phosphorus, 0.6Sulfur, 0.6

Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et alin Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003

4 MY

4 BYhttp

://ge

olog

y.w

r.usg

s.gov

/par

ks/g

time/

Gtim

esca

le.p

df

Time MYA Event4 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

0.3 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 Cave0.012 Homo sapiens sapiens have domesticated dogs in Kirkuk, Iraq 0.01 First permanent Homo sapiens sapiens settlements 0.01 Homo sapiens sapiens learn to use fire to cast copper and harden pottery

0.006 Writing is developed in Sumeria

www.talkorigins.org/origins/geo_timeline.html

Time MYA Event

4600 Formation of the approximately homogeneous solid Earth by planetesimal accretion

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

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

4000 Bombardment of the Earth by planetesimals stops

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

3800 ? Condensation of atmospheric water into oceans

3500-2800 Prokaryotic cell organisms (eubacteria and archaebacteria) develop

3500-2800Beginning of photosynthesis by cyanobacteria which releases oxygen molecules into the atmosphere and steadily works to strengthen the ozone layer and change the Earth's chemically reducing atmosphere into a chemically oxidizing one

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

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

1500 Eukaryotic cell organisms develop (common ancestors of algae, fungi, plants, animals)

1500-600 Rise of multicellular organisms (algae, fungi, plants, animals)

580-545 Fossils of Ediacaran organisms are made (biomineralized bodies)www.talkorigins.org/origins/geo_timeline.html

from MY

to MY MYA Era

oceans 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

Prot

eroz

oic

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

Had

ean

Pre-Hadean

Arc

haea

nName ten or more

globally important eventsin any column.

Think about the W5H:whowhatwhenwherewhyhow

Emphasis onconnections not collections

Senior Projects, Summer Projects, non-thesis Masters Projects, or Special Problems BIO, CHEM, or GEOL 200 or 400

Students may do library research (books, journals, websites), original thinking, and/or data analysis.

Five Billion Years of Global EvolutionIdentify and sequence globally important physical, chemical, and/or biological events and processes in the five billion year history of the solid Earth, hydrosphere, atmosphere, and/or biosphere (molecules, cells, organisms, and ecosystems) with emphasis on Pre-Cambrian eras.

Prokaryote and Eukaryote EvolutionStudy the structure and evolution of prokaryotes, eukaryotes, biologically

important molecules, and/or metabolic processes. Emphasis is on Pre-Cambrian cladograms based on molecular clocks and fossil records.

Biochemical and Geochemical EvolutionStudy biochemical, geochemical, and/or biogeochemical properties and

processes from cellular to global scales in Hadean, Archaean, Proterozoic, and/or Phanerozoic Eras.

http://en.wikipedia.org/wiki/Bacterium

Prokaryote and

Eukaryote Evolution

Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et alin Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003

4112

Arc

haea

3977

Aqu

ifex

3644

The

rmot

oga

3096

Chl

orob

ium

Cya

noba

cter

ia26

88 F

irm

icut

es29

23 F

usob

acte

rium

2800

Pro

teob

acte

ria

1351

Ani

mal

s14

58 F

ungi

1558

Alg

ae

1609

Alg

fung

imal

1513

Fun

gim

al

2309

Euk

aryo

tes

2100

? R

espi

rato

rs

Evaluate accuracy of molecular timescales

Identify and describe node organisms and characters

Provide common names for each label

Enter data into my 5 BY timeline

Investigate environmental and ecological causes

Examine environmental and ecological impacts

Describe ecosystems prevalent in each era

Create separate charts for each geologic era

global average of 40 inches of precipitation per year

recycles 120,000 cubic miles of water and transfers heat

percolation

precipitation

27

vapor transport10

groundwater flow

return flow10

precipitation

94

After Stowe

oceans hold340 M cubic miles

units - 1000 cubic miles/year


17 evaporation

104

Biochemical and

Geochemical Evolution

photic zone(light)

aphotic zone(dark)

Sun

V B G Y O R IRUV

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

solid Earth Ocean

atmosphere

where is the biosphere?

oceans and atmosphere scatter, absorb, and transfer

energy

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

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

Temperatureof the atmosphere

ocean

10 km

sea level

Stratosphere

Troposphere has 75% of airdensity and temperature

decrease with altitudetemperaturevs. altitude

Sun

cool-70F

warm60F

ozone layer

After Tarbuck


50

100

20

30

incidentsunlight

absorb

scatteredsunlight

absorb

sea + land

atmosphere

Sun

30

30

evap

condense

90

65

155

absorb

radiate

radiate

5

110

105

radiate

absorb

radiated heatLWIR

annual carbon cycle in the atmosphere

ocean

90

R

Ph

93

Ph

110109

R

+1

+3billions of tons of carbon

Sun

7

ff

-7

where is the carbon?(billions of metric tons)

Sun

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

sediments20,000,000

deep ocean38,000,000

carbon dioxide gasin atmosphere 700

Dissolved organic matter ~2000

humus2000 fossil fuels

5000?

dissolved gas 40,000

Hea

ling

Gai

a by

Jam

es L

ovel

ock

p139

BIO 200 Special Problems in Biological Sciences for lower division undergraduates

Joshua Yang - Carbon in the Geobiosphere

Tim Tappscott - Prokaryote Evolution

Raechel Harnoto – Astrobiology and Global Evolution

BIO 100 Orientation to Biological SciencesIntroduction to Biological Sciences faculty, department and campus resources, research opportunities, possible careers, studying science, and current topics in biology.

convective zone

fusioncore

The Sun creates, stores, and radiates energy

radiative zone

zone volume ~r3 mass total

energyfusion core r < ¼ 1/64 1/2 2/3

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

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

The Sun evolves because fusion changes the composition of the core which changes density, temperature, and luminosity

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+10Radius (cm)

X

ZAMS X1.5 BY X3 BY X4.5 BY X6 BY X7.5 BY X9 BY X

Guzik Field Lopez x70y28z02 112005

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+10radius (cm)

Guzik - LANL solar evolution code

Temperature (K)

00E+0

2E+6

4E+6

6E+6

8E+6

10E+6

12E+6

14E+6

16E+6

0E+00 1E+10 2E+10 3E+10 4E+10 5E+10 6E+10 7E+10radius (cm)

Guzik - LANL solar evolution code

Solar Evolution

0.00.10.20.30.40.50.60.70.80.91.0

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

Rel

ativ

e Va

lue

T/Tsun

R/Rsun

L/Lsun

cycle 17

L = 4πR2·σT4

Guzik + Field

dhillon phy213 website

Equations of Stellar Structure

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


convective zone 0

fusion core 988

radiative zone 12

Sun

layers volume (cm3) mass (g)average density (g/ cm3)

relative volume

relative mass


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



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 heat flow

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



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

greatly simplified

H1 + H1 → H2 + e+ + υ

H2 + H1 → He3 + γ

nucleosynthesis: billion years or seconds?

e+ + e- → γ + γ

photons lose energy quickly

neutrino escapes from Sun

proton turns into neutron

million years He3 + He3 → He4 + H1 + H1

http://theory.uwinnipeg.ca/mod_tech/node209.html

Electrical forces keep protons apartbecause like charges repel

CoulombBarrier

attr

activ

ere

puls

ive

YukawaAttractiveNuclearPotential

The rich get richer.If you can climb the rim,

you can drop in the craterand gain kinetic energy.

1

2

Never gonna happen, my friend!

Proton needs 1000 times more thermal energy

than average

1

2

Tunneling happens all the time!

Thermonuclear fusion generates energy to replace energy radiated into space,

but it takes energy to get started

How did the Sun get hot originally?

As cold gases condense to form the Sun, they get hot and lose energy

This stage lasts 100,000 years.The Sun was 1000 times brighter.

gravitational attraction

Solar FormationHow did a cold dilute gas contract under gravitational attraction and produce a core hot enough and dense enough to sustain thermonuclear fusion?My simplified but detailed explanation of solar formation is more complete than most non-mathematical discussions.1. Enormous molecular clouds resist gravitational contraction for billions of years with the help of kinetic energy, rotational energy, and magnetic fields until an external perturbation alters the properties of a portion of the cloud enough to trigger free fall contraction as gravitational attraction dominate other influences.2. My simple explanation of solar formation will ignore rotation and magnetic effects and will assume the cloud is a cold dilute self-gravitating gas with uniform composition, density, and temperature and the mass of the Sun.3. Gas particles in the cloud accelerate as they fall toward the center of mass because there is no hydrostatic support.4. Gas density remains uniform as it increases because all particles have the same free fall time since velocity and acceleration increase linearly with radius since a = GM/r2 = G(4πρr/3).5. Collisions in the center raise the temperature, internal energy, and pressure producing temperature and pressure gradients as the opacity increases.6. The developing pressure gradient provides some hydrostatic support for the increasingly dense core gases.7. Falling particles continue to compress the core, increasing its density, pressure, and temperature.8. The differential pressure reduces the contraction near the center producing a density gradient.9. Gas opacity initially increases with density and temperature, trapping radiant energy in the interior.10. Surface cooling by radiative transport also increases the interior temperature gradient.11. The high opacity of the interior maintains the increased temperature gradient.12. A convection instability forms and convection transports trapped interior heat from the core to the surface.13. At very high temperature, opacity decreases as bound electrons are freed.14. The core density increases enough to fuse hydrogen nuclei.15. Radiative energy transport replaces convective energy transport except for the outer gases.

Solar EvolutionHow can the Sun grow brighter over time while the

core hydrogen abundance decreases?1. Energy generated by fusion replaces energy diffusing from the core to the surface.

2. Nucleosynthesis reduces the core hydrogen abundance and particle density.

3. Some core electrons are annihilated by positrons produced during nucleosynthesis.

4. Core opacity decreases as temperature rises and density of core electrons decrease.

5. The decrease in core particles does not decrease the local energy density or pressure.

6. The core temperature rises as the average energy per particle rises.

7. Decreases in core hydrogen abundance reduce protons available for fusion, but fusion rate increases slightly due to the increased core temperature.

8. Luminosity increases as the temperature and temperature gradient increase and opacity decreases.

9. Increased luminosity increases energy density and pressure at larger radii.

10. Pressure increase expands envelope and forces more particles into core.

11. Core contraction maintains the pressure gradient required for hydrostatic support.

12. Gravitational contraction increases core density, pressure, temperature, and energy density.

13. Fusion rate increases with core density and temperature – enough to sustain higher luminosity.

14. Solar envelope expands as its temperature rises, increasing the surface radius and temperature.

15. The Sun’s luminosity increases as its surface radius and temperature grow over billions of years.

Earth creates, stores, and radiates energy

ICB

CMB

inner core - conductionouter core – convection?

lower mantle - convectionD” - conduction

upper mantle - convectionlithosphere - conductionatmosphere - radiation

convection is powered by radiogenic heat sources and produces chemical evolution

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

ioge

nic

Hea

t Flo

w (W

)

TotalU-235K-40U-238Th-232

Earth’s composition evolves as rare but critical elements decay

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

Al8.41Ca

5.29

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

models of growth of continental volume (%)

4 3 2 1 0BYA

100

75

50

25

0

1992

geoch

emical

Van Andel

linear reference

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

from VanAndel Fig. 13.6

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+6radius (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

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)

Tem

pera

ture

(K)

boundaries4 BYA2 BYA0 BYA

assume temperature changes linearly with time

Mantle

Core

total heat flow (W)

00E+05E+12

10E+1215E+1220E+1225E+1230E+1235E+1240E+1245E+12

0E+0 1E+6 2E+6 3E+6 4E+6 5E+6 6E+6 7E+6radius (m)

tota

l hea

t flo

w (W

) boundaries

current total heat flow (W)

radiogenic heat flow (W)

current lost heat flow (W)

current ΔGBE heat flow (W)

latent heat flow (W)

CMB

Mantle

Core


lithosphere7

lower mantle537

upper mantle123

outer core315

inner core19

relative mass

lithosphere21

lower mantle492

upper mantle162 outer core

308

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

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

layersinternal

energy (J )

heat sources



relative heat

sourcesrelative



average density


relative mass



visibleradiation

optical absorption impedes energy flow

From where we sit, brighter than a

thousand suns briefly

transparentplanet

thermalconduction

thermal scattering impedes energy flow 5000°F

2.5°F/mile or 0.001°F/foot

solidplanet

thermalconvection

viscosity and density affect energy flow

moltenplanet

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

CH

CH N

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

CN

C

OC

H

N

O

CH H

H

H H

C

C

CC

C C

CH

H

HH

HH

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

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

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

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

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

How does a computer “design” its own software?

AlaHis Tyr Val Thr Val Arg Leu Gly

1

52 321


How does information evolve?

21 3 4

2 3

21 3

21 34 5

duplication

4 5

1

52 321


How does information evolve?

21 3 4

2 321 3 21 3

deletion and insertion

Documents

Life on Our Evolving Planet slides