2. rfield website Global Evolution Timeline Global models and database The SunThe Sun and Solid EarthSolid Earth AtmosphereAtmosphere and OceansOceans Organisms and Ecosystems Molecules and Cells © Bob Field 2007

3. 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.

4. 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.timelineevents 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.database 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.programs 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.

5. DR. BOB FIELD Adjunct Physics Professor Research Scholar in Residence I develop and supervise natural science projects for students in physics, physical science, chemistry, biology, math, K-16 and environmental education. My number one interest is Global Evolution Studies. I also develop natural history programs primarily for the local state parks and the Morro Bay State Park Museum of Natural History. I have a brief biographical sketch. Contact me at rfield at my calpoly.edu email address.natural science projectsGlobal Evolution Studiesnatural history programsbiographical sketch My extensive website has three parts: NATURAL SCIENCE GLOBAL EVOLUTIONGLOBAL EVOLUTION NATURAL HISTORY drbobfield bobfield64 The only good is knowledge and the only evil is ignorance (Socrates) Return to Physics Department Home Page

6. GLOBAL EVOLUTION STUDIES The National Academy of Science says that it is the role of science is to provide plausible natural explanations of natural phenomena. The Natural History of Planet Earth is the product of nearly five billion years of global evolutionary processes that followed the first nine billion years of cosmic evolution. Complexity grows when energy flows in natural systems because simple building blocks evolve into complex materials and processes. The structure and evolution of the OASES (oceans, atmosphere, solid Earth, and Sun) and the biosphere (molecules, cells, organisms, and ecosystems) depend on interactions of energy and matter. The origin, evolution, diversity, abundance, and distribution of life are emergent properties of increasing environmental complexity. go to natural science projects, natural history programs, globalevolution, or rfield home pagenatural science projectsnatural history programsglobalevolutionrfield 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

7. click on any figure Natural History of Planet Earth Global Evolution © Mike Baird

8. How do global changes impact the California coast? The Natural History of the California Coast poster exhibition planned for the summer of 2009 may be seen by 90,000 visitors to the Hearst Castle National Geographic Theater lobby. It illustrates the impact of global evolutionary processes by relating local natural history to global natural systems themes from Dr. Art Sussman’s Guide to Planet Earth using Dr. Sam Ham’s principles of thematic interpretation.

9. Plausible Natural History publications birds, marine mammals, Monarch Butterflies, tide pools, kelp forests, coral reefs, lichen, algae, fungus, trees, wildflowers, mountains, molecules, cells, Planet Earth, The Facts of Life: From the Oceans to the Stars, etc. Living Natural History programs Montana de Oro State Park, Museum of Natural History, Pismo State Beach, Elfin Forest, Morro Bay Estuary, Oso Flaco State Park, Lopez Lake, Big Sur, Point Lobos, Yosemite, Monterey Bay Aquarium, Wild Animal Park, Sea World, etc. Shared Reading Program (PREFACE?) High Tide author Mark Lynas travels around the world to investigate local impacts of global warming

10. 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)?

11. 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

12. Name ten or more globally important events in any column. Think about the W5H: who what when where why how Emphasis on connections not collections

13. 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

15. Era/Period/Epoch Time (Myr ago) Archaeozoic (Archean) era5000-1500 Proterozoic era1500-545 Paleozoic era Cambrian period545-505 Ordovician period505-438 Silurian period438-410 Devonian period410-355 Carboniferous (Mississipian/Pennsylvanian) period355-290 Permian period290-250 Mesozoic era Triassic period250-205 Jurassic period205-135 Cretaceous period135-65 Cenozoic era "Recent Life" Tertiary period Paleocene epoch65-55 Eocene epoch55-38 Oligocene epoch38-26 Miocene epoch26-6 Pliocene epoch6-1.8 Quarternary period Pleistocene epoch1.8-0.01 (Lower Paleolithic)0.50-0.25 (Middle Paleolithic)0.25-0.06 (Upper Paleolithic)0.06-0.01 Holocene epoch0.01-0 www.talkorigins.org/origins/geo_timeline.html Geological Timeline

16. Time MYAEvent 4Development of hominid bipedalism 4-1Australopithecus exist 3.5The Australopithecus Lucy walks the Earth 2Widespread use of stone tools 2-0.01Most recent ice age 1.6-0.2Homo erectus exist 1-0.5Homo erectus tames fire 0.3 Geminga supernova explosion at a distance of roughly 60 pc--roughly as bright as the Moon 0.2-0.03Homo sapiens neanderthalensis exist 0.050-0Homo sapiens sapiens exist 0.04-0.012 Homo sapiens sapiens enter Australia from southeastern Asia and North America from northeastern Asia 0.025-0.010Most recent glaciation--an ice sheet covers much of the northern United States 0.020Homo sapiens sapiens paint the Altamira Cave 0.012Homo sapiens sapiens have domesticated dogs in Kirkuk, Iraq 0.01First permanent Homo sapiens sapiens settlements 0.01Homo sapiens sapiens learn to use fire to cast copper and harden pottery 0.006Writing is developed in Sumeria www.talkorigins.org/origins/geo_timeline.html

17. Time MYAEvent 200Pangaea starts to break apart 200Primitive crocodiles have evolved 200Appearance of mammals 145Archaeopteryx walks the Earth 136Primitive kangaroos have evolved 100Primitive cranes have evolved 90Modern sharks have evolved 65K-T Boundary--extinction of the dinosaurs and beginning of the reign of mammals 60Rats, mice, and squirrels have evolved 60Herons and storks have evolved 55Rabbits and hares have evolved 50Primitive monkeys have evolved 28Koalas have evolved 20Parrots and pigeons have evolved 20-12The chimpanzee and hominid lines evolve 10-4Ramapithecus exist www.talkorigins.org/origins/geo_timeline.html

18. Time MYAEvent 545Cambrian explosion of hard-bodied organisms 528-526Fossilization of the Chengjiang site 517-515Fossilization of the Burgess Shale 500-450Rise of the fish--first vertebrates 430Waxy coated algae begin to live on land 420Millipedes have evolved--first land animals 375 The Appalachian mountains are formed via a plate tectonic collision between North America, Africa, and Europe 375Appearance of primitive sharks 350-300Rise of the amphibians 350Primitive insects have evolved 350Primitive ferns evolve--first plants with roots 300-200Rise of the reptiles 300Winged insects have evolved 280Beetles and weevils have evolved 250Permian period mass extinction 230Roaches and termites have evolved 225Modern ferns have evolved 225Bees have evolved www.talkorigins.org/origins/geo_timeline.html

19. Time MYAEvent 4600Formation of the approximately homogeneous solid Earth by planetesimal accretion 4300 Melting of the Earth due to radioactive and gravitational heating which leads to its differentiated interior structure as well as outgassing of molecules such as water, methane, ammonia, hydrogen, nitrogen, and carbon dioxide 4300 Atmospheric water is photodissociated by ultraviolet light to give oxygen atoms which are incorporated into an ozone layer and hydrogen molecules which escape into space 4000Bombardment of the Earth by planetesimals stops 3800The Earth's crust solidifies--formation of the oldest rocks found on Earth 3800Condensation of atmospheric water into oceans 3500-2800Prokaryotic cell organisms develop 3500-2800 Beginning of photosynthesis by blue-green algae which releases oxygen molecules into the atmosphere and steadily works to strengthen the ozone layer and change the Earth's chemically reducing atmosphere into a chemically oxidizing one 2400 Rise in the concentration of oxygen molecules stops the deposition of uraninites (since they are soluble when combined with oxygen) and starts the deposition of banded iron formations 1600 The last reserves of reduced iron are used up by the increasing atmospheric oxygen--last banded iron formations 1500Eukaryotic cell organisms develop 1500-600Rise of multicellular organisms 580-545Fossils of Ediacaran organisms are made www.talkorigins.org/origins/geo_timeline.html

20. Solar and Global Evolution are parts of Cosmic Evolution ~ age (BY)generic structure average power density (W/kg) 12galaxies0.00005 10stars0.0002 5planets0.01 3plants0.1 0.01animals2 0.001brains15 0.0000001society50 table from Chaisson139 image from Science Yearbook when energy flows, complexity grows

21. core lower mantle upper mantle oceanic lithosphere oceanic crust oceans biosphere atmosphere subcontinental lithosphere sediments lower crust upper crust impact Interactions between Earth systems Condie33 Fig 1.33 sun

22. C 6 12 N 7 14 O 8 16 H 1 He 2 4 Periodic Table of Chemical Elements 92%~8% 0.07% 0.04% 0.02% 0.01% Abundance in Universe in % 0.1% } Ne 10 20 Na 11 23 Mg 12 24 Al 13 27 Si 14 28 P 15 31 S 16 32 Cl 17 35 Ar 18 40 K 19 39 Ca 20 40 Cr 24 62 Mn 25 55 Fe 26 56 Ni 28 59 0.02% everything else Stars build big atoms from small ones Sunlight is the product of “hydrogen burning” and helium is the “spent fuel” Sun creates energy as a waste product when it fuses 4 H 1 → He 4

23. The Sun internal structure and size of layers density, mass, gravity, pressure, volume temperature internal energy distribution energy sources: fusion energy, gravitational contraction composition – hydrogen, helium, “metals”, free electrons material properties energy transport: convection, conduction, radiation mass flow in convection evolution of the Sun – composition,density, temperature, fusion rate, luminosity formation of the Sun

24. convective zone radiative zone fusion core Hot and Heavy Sun’s structure zone volume ~r 3 mass total energy fusion core r < ¼ 1/641/22/3 radiative r < 0.7 1/31/21/3 convective r > 0.7 2/31/801/100

25. relative values used in our LANL solar evolution cases

28. Guzik - LANL solar evolution code

29. g (R) = GM(R)/R 2 Guzik + Field

31. Ostlie & Carroll 275 5 4 3 2 1 0 -2 4 5 6 7 8 log K (cm 2 /g) log T (K) -10 -8-6 -2 0 -4 2 X=0.7 Z=0.02 Rosseland mean opacity curves are labeled by log density (g/cm-3) Stellar Opacity

32. Guzik + Field dL/dR = 4πR 2 ρε

33. L = 4πR 2 ·σT 4 Guzik + Field

34. Guzik Field Lopez x70y28z02 112005 metal content influences solar luminosity and lifetime

35. Guzik Field Lopez x70y28z02 112005 luminosity increases as core hydrogen is depleted surface radius

36. Guzik Field Lopez x70y28z02 112005

37. dhillon phy213 website Equations of Stellar Structure

38. The Solid Earth size of layers density, mass, gravity, pressure, volume composition – iron silicon oxygen magnesium nickel material properties temperature thermal energy distribution heat flow sources radioactive decay of U, Th, and K heat loss as Earth cools gravitational energy released as Earth cools latent heat released as inner core freezes energy transport: convection, conduction, radiation mass flow in convection evolution of the Earth’s structure formation of the Earth

39. Zeroth order model of the Earth has three layers core mantle core mantle crust atmosphere

40. First order model of the Earth shows layers Seismic 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

41. inner core R < 1221.5 km outer coreR < 3480 km lower mantleR < 5701 km D”R < 3630 km upper mantleR < 6291 km lithosphereR < 6371 km ICB CMB Mantle Core

42. McDonough

43. Whole Earth Crust Mantle Core

44. zeroth order model - composition Relative Mass Abundance of Elements on Earth McDonough

45. ICB CMB Mantle Core based on McDonough

46. Elements 2006-07-18 mfischer b revision

47. ICB CMB Liquid Outer Core Mantle based on Stacey Appendix G

48. ICB CMB Mantle Core

49. Mantle Core

50. Stacey Table 6.4 Heat Loss Budget (TW) INCOME 8.2 Crust radioactivity 19.9 Mantle radioactivity 1.2 Latent heat and gravitational energy released by core evolution 0.6 Gravitational energy of mantle differentiation 2.1 Gravitational energy released by thermal contraction 32 TW TOTAL EXPENDITURE 8.2 Crust heat loss 30.8 Mantle heat loss 3.0 Core heat loss 42 TW TOTAL 10 TW NET LOSS OF HEAT

51. CMB 19.9 TW in mantle 8.2 TW in crust…… 28.1 TW whole Earth Mantle Core based on Stacey

52. ICB MantleCore based on Stacey 4 BY 3 BY 2 BY 1 BY

53. CMB Mantle Core

54. heat flow in ocean crust vs. continental crust?

55. first order model – composition and phase zeroth order model - composition Absolute and Relative Energy, Heat, and Heat Flow

57. first order model – composition and phase zeroth order model - composition Volume, Mass, Density, Energy, Heat, and Heat Flow

58. first order model – composition and phase zeroth order model - composition Relative Volume, Mass, Energy, Heat, and Heat Flow

59. ruru ΔR v mass Δr convection model for an ideal gas force / area = viscosity x velocity gradient constant P = (ρ-Δρ)k(T+ΔT)/m p force = Δρ(πr u 2 ΔR)g R cylinder area = 2πr u ΔR Δρ(πr u 2 ΔR)g R /(2πr u ΔR) = η Δv mass /Δr Δρ r u g R / 2 = η Δv mass /Δr v mass = Δρ r u g R Δr / 2η what if you have molten rocks?

60. Stacey318 Typical Cartoon of Mantle Convection and Plumes

62. isotope energy/atom (MeV) μ W/kg of isotope μ W/kg of element estimated total Earth content (kg) total heat (10 12 W) total heat 4.5 BYA (10 12 W) 238 U 47.79594.3513.15x10 16 12.525.1 235 U 43.95624.050.0954x10 16 0.5445.1 232 Th 40.526.6 47.2x10 16 12.5615.7 40 K 0.71300.0035 7.14x10 20 (total K) 2.530.2 total28.1117.3 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)

63. Mantle Core

64. ICB MantleCore based on Stacey now after 4 BY of freezing 2 BYA after 2 BY of freezing

65. before and after the Great Iron Catastrophe

67. models of growth of continental volume (%) 4 3 2 1 0 BYA 100 75 50 25 0 1992 geochemical Van Andel linear reference 1992 geochemical BYA: % 0: 100 0.6: 90 2.6: 10 3.6: 0 4.5: 0 from VanAndel Fig. 13.6

68. The Atmosphere size of layers density, mass, gravity, pressure, volume composition – nitrogen oxygen water argon carbon dioxide aerosols material properties temperature global energy budget and distribution – latitude season altitude heat flow sources absorbed sunlight Earth’s radiated energy air-sea interactions energy transport: convection, conduction, radiation mass flow in convection evolution of the atmosphere – composition structure density circulation origin of the atmosphere

69. 12 0 24 8 90 20 48 surface incident shortwave flux 343 reflected shortwave flux 21 69 16 outgoing longwave flux 22 90 125 after Salby45, etc. 1693903271690 16 atmosphere absorbed by clouds absorbed by H 2 O, O 3, aerosols reflected by clouds reflected by surface back scattered by air emitted by clouds emitted by H 2 O, CO 2, aerosols emitted by surface absorbed by clouds absorbed by H 2 O, CO 2, aerosols emitted by H 2 O, CO 2, aerosols sensible heat flux latent heat flux surface- atmosphere heat transfer Average Global Energy Budget (W/m 2 ) 169 + 327 = 496surface390 + 16 + 90 = 496 343planet(21 + 69 + 16) + (22 + 90 + 125) = 343 (20 + 48) + (120 + 248 + 16 + 90) = 542atmosphere(90 + 125) + 327 = 542

70. composition by mass?

71. Temperature of the atmosphere f ocean 60 miles 50 40 30 miles 20 10 sea level Thermosphere Mesosphere Stratosphere Troposphere 75% of air Temperature vs. Altitude Sun -130F -70F 32F 60F ozone layer After Tarbuck

73. ~6.6 K per kilometer

74. ~10X decrease per 15-20 km ascent

75. half of the mass of the atmosphere is below an altitude of 6 km and is enclosed in a volume of 500 million km 2 x 6 km or 3 billion km 3 or 3x10 18 m 3

76. 0 0.02 0.04 0.06 0.08 0.1 0.12 24 201612840 Equator midnight Noon Equinox Solar Flux vs. Time of Day Tropic of Cancer Arctic Circle North Pole 6 am6 pm

77. 1210864224 0 0.02 0.04 0.06 0.08 0.1 0.12 Noon Midnight 6 am 141618202224 Noon Midnight 6 pm Summer Solstice Solar Flux vs. Time of Day Equator Tropic of Cancer Arctic Circle North Pole

78. absorption by ozone, water, and CO 2 scattering by N 2, O 2 and aerosols 0.3 0.511.522.53 0 500 1000 1500 2000 Wavelength Intensity visible window UV VisibleInfrared sun is directly overhead no clouds direct beam only Spectrum of Sunlight observed on Earth

79. Field - solar flux code

80. CO 2 and H 2 O gases absorb far infrared 2 Blackbodies 1 Greenhouse atmosphere transparent to visible light Earth Far Infrared Energy 10 micron peak Earth is 300K Sun 0.5 micron peak Sun is 6000K Visible Solar Energy

81. 05 10 15202530 0 50 100 150 200 250 300 Blackbody Radiation Wavelength Intensity 373K water boils 5800K solar energy absorbed by Earth 255K atmosphere 273K water freezes

82. 288K Earth's surface 05 10 15202530 0 5 10 15 20 25 30 Greenhouse Gases Absorb Blackbody Radiation Wavelength (microns) Intensity O3O3 CO 2 H2OH2O 255K atmosphere

83. Plants 15% Soil 20% Sand 40% f Average Visible Reflectances of common substances Sun Clouds 50% Snow 60% Water 8%

84. 1210864224 0 0.02 0.04 0.06 0.08 0.1 0.12 Noon Midnight 6 am 141618202224 Noon Midnight 6 pm Energy Transfer in a Day What is the hottest time of day? heat gain ocean heat loss land heat loss desert heat loss

85. atmospheric circulation bottom heated absorbed heat peaks at Equator no rotationwith rotation

88. HW2B

89. The Oceans size of layers density, mass, gravity, pressure, volume composition – water salt dissolved gases and organics particulates organisms material properties temperature global energy budget and distribution – latitude season altitude heat flow sources absorbed sunlight air-sea interactions energy transport: convection, conduction, radiation mass flow in convection evolution of the ocean – salt ice evaporation flow patterns depth area origin of the ocean

90. wikipedia

91. Gas N 2 O 2 CO 2 Dry Air 78% 21% 0.036% Sea Water 12 ppm 7 ppm 90 ppm Ratio of Total Amount in Ocean to Atmosphere 0.004 0.01 62 Abundance of Dissolved Gases H 2 O 0.3% 97% 100,000

92. global average of 40 inches of precipitation per year recycles 120,000 cubic miles of water percolation precipitation 27 vapor transport 10 groundwater flow return flow 10 precipitation 94 After Stowe oceans hold 340 M cubic miles units - 1000 cubic miles/year evaporation & transpiration 17 evaporation 104

93. 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 Atmosphere0.04 1 inch Lakes0.4 1 foot Ground Water 25 60 feet Polar Caps & Ice 75180 feet

94. 500 million square km area x 3 km depth = 1.5x10 9 km 3 wikipedia 1.4x10 9 km 3 volume x 1000 kg/m 3 x 10 9 m 3 /km 3 = 1.4x10 21 kg

95. wikipedia

96. Ocean and Atmosphere simplified heuristic models 1.An Earthlike planet rotates on its axis. There is no atmosphere. The planet is dry except for an ocean located on the Equator in a canal that is three kilometers deep and 3000 km wide (or less) and encircles the planet. Ignore any non-uniform heating effects from the Sun. I claim that the steady state solution is that the ocean water moves with the Earth so that an observer on Earth sees no currents in the ocean. True or False? 2.Would the same argument also apply if the entire featureless planet were covered with 3 km deep water? The equatorial bulge of the Earth due to its rotation will also appear in the global ocean so that the water depth would be 3 km at all latitudes. Since no water is flowing between latitudes, no Coriolis effects will appear even though water at different latitudes has different velocities but the same angular velocity. Therefore I claim that on a water covered planet, an observer would observe no currents in the ocean relative to the sea floor. True or False? 3.The same argument applies to the atmosphere of a featureless planet whether or not there is an ocean covering it. No winds appear as long as the planet is uniformly heated. If the ocean is top heated uniformly and the atmosphere is bottom heated uniformly, then the ocean will still have no currents, but the atmosphere will have a vertical air flow (thermals) that resembles Benard cells, but no Hadley cells between latitudes. True or False? 4.Do local perturbations produce transient flow patterns due to flow instabilities particularly in the lower viscosity atmosphere? 5.In the case of non-uniform heating, fluids flow between latitudes and the velocity differences between masses of air (and water) at different latitudes produce Coriolis effects. True or False?

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

98. Keith Stowe, Exploring Ocean Science surface currents are driven by winds which result from non-uniform heating of the globe

99. pelagic zone (water column) benthic zone (seafloor) Ocean Zones pelagic / benthic sediments plankton & nekton Sun

100. photic zone (light) aphotic zone (dark) Ocean Zones photic / aphotic Sun V B GYORIRUV 10% 50' 0' 300' 40' 15' 2'

101. f photic zone (light) aphotic zone (dark) pelagic zone (water column) benthic zone (seafloor) Ocean Zones pelagic / benthic photic / aphotic Sun

102. f photic zone (light) aphotic zone (dark) neritic province (above continental shelf) oceanic province (beyond continental shelf) pelagic zone (water column) benthic zone (seafloor) Ocean Zones pelagic / benthic photic / aphotic neritic / oceanic Nereus & 50 Nereid Sun

103. f space and Sun atmosphere water world “continental crust” oceanic crust photic zone (light) aphotic zone (dark) pelagic zone (water column) benthic zone (seafloor) Sun

104. intertidal or littoral zone atmosphere ocean continental crust oceanic crust sediments Sun

105. f atmosphere ocean continental crust sediments upwelling Sun

106. 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

107. Field - solar sea flux code absorption and scattering coefficients of air and water actual curves of components depend on concentrations

108. Field - solar sea flux code transmitted sunlight in pure water vs. depth (0, 1, 3, 10, 30, 100 meters)

115. Organisms and Ecosystems

116. ocean sediments 60 tons of organic matter in ocean is dissolved organic molecules (yellow matter) one ton of organic matter in ocean is particulate 1700 pounds of particulate is detritus 240 pounds phytoplankton 60 pounds zooplankton 1 pound of large animals after Stowe Sun

117. ocean sediments 98.3% of all organic matter in ocean is dissolved organic molecules = 2000 gC/m 2 1.7% of all organic matter in ocean is particulate = 35 gC/m 2 86% of particulate is detritus = 30 gC/m 2 12% is phytoplankton = 4 gC/m 2 3% is zooplankton = 1 gC/m 2 0.05% is large animals = 0.02 gC/m 2 after Stowe Sun

118. one million land animal species (75% insects) 4,000 pelagic animal species 200,000 ocean animal species (98% benthic) Distribution of Animal Species

119. Plant Production Upwelling Coastal waters Open Ocean 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

120. Tjeerd van Andel, Science at Sea: Tales of an Old Ocean 0 50 100 150 200 Ocean Fish Productivity/Area Upwelling Coastal waters Open Ocean 0 25 50 75 100 125 150 175 200 Plant Productivity/Area Upwelling Coastal waters Open Ocean Land

121. from Stowe & Thurman *before sinking below the photic zone recycles per year steps of bacterial decompostion* considerations requirement 10 3 4 1 nitrogen 15 phosphorus 1 universe 200 1 oceans 6 1

122. Seasonal Abundance of Sunlight, Nutrients, Phytoplankton, Grazers Sunlight Grazers Phytoplankton Nutrients JanFebMarchAprilMayJuneJulyAugSeptOctNovDec After Stowe 276

123. productivity (gC/m 2 /day) continental shelf central ocean high latitudes JanFebMarApr MayJuneJuly AugSepOctNovDec 0.9 0.6 0.3 0 after Keith Stowe, Exploring Ocean Science

124. temperate continental shelf central ocean JanFeb MarApr MayJuneJulyAug SepOct NovDec 0.9 0.6 0.3 0 after Keith Stowe, Exploring Ocean Science productivity (gC/m 2 /day)

125. annual carbon cycle in the atmosphere ocean 110 109 90 93 +1 +3 billions of tons of carbon Sun 7 -7

126. where is the carbon? (billions of metric tons) ocean Sun from Biology of plants 5th Ed. by Raven et al. page 115 sediments 20,000,000 deep ocean 38,000,000 carbon dioxide gas in atmosphere 700 Dissolved organic matter ~2000 humus 2000 fossil fuels 5000? photosynthesis removes 4 billion tons of carbon from atmosphere per year dissolved gas 40,000

127. Molecules and Cells

128. What do cells do? Store, exchange, and transform: matter energy information Modern cells are chemical factories: complex, highly efficient, self-replicating. Cells store and release energy to build up and break down biomolecules...

129. The Origin of Life Complex molecules form and evolve Simple proto-cells form and evolve Modern cells evolve and diversify

130. 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 Hazen The Sciences: An Integrated Approach 5 kingdoms: bacteria algae fungus plant animal

131. What are the building blocks of molecules? A, B, and C are all about 97% CHO O C SH N P Life’s Origin page 15 by Walter Schopf ABC Hydrogen616356 Oxygen262931 Carbon10.56.410 Mammal Nitrogen2.41.42.7 Sulfur0.130.060.3 Phosphorus0.130.120.08 Calcium0.23-- Bacteria Comet

132. H H O O O O P N N C H H H H C O O S H H N H H H O O N O O H H O O O C SH N P many common molecules are made from CHONSP C O S atoms can share or transfer electrons H – 1 He – 0 O – 2 C – 4 N – 3 S – 2 P – 3 or 5

133. Methane can form new molecules O H C H H H O methanol methane formaldehyde formic acid biochemists give big names to small molecules

134. OH C H H H O H C H H H C H H C C C C C C C C C C C H N CCC H N C H HO H H H H C O C C H N CC N N C 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

135. backbone of phospholipid (H and O not shown) CO, H 2, PO 4 are building blocks of phospholipids found in cell membranes R C C C C C C C C PiPi C C C C C C C C fatty membrane spheres form naturally in meteors

136. C H O H C H C HO C H H O C H H O H H O C H H O C H HO C H HO C H HO C H HO C H HO C H HO 6 CH 2 O + energy + catalyst C O C H O C H H O glucose is a building block of carbohydrates glucose

137. C H O H C H C HO C H H O C 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 H 2 O 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 CO 2 6 O 2 glucose

138. C O C H O C H H O C O C H O C H H O glucose supplies energy to make ATP C3H3O3C3H3O3 C H O H C H C HO C H H O C H H O H H O C H H O C3H3O3C3H3O3 glucose ATP aerobic fermentation makes 2 more ATP ATP

139. C H O H C H C HO C H H O C 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 O 2 glucose

140. C H O H C H C HO C H H O C 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 H 2 O 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 CO 2 ATPATPATPATP

141. C H O H C H C HO C H H O C H H O H H O C H H O C H HO C H HO C H HO C H HO C H HO C H HO 6 CH 2 O + energy + catalyst fructose is an isomer of glucose: table sugar forms by joining them

142. GGGGGGG G F simple sugar building blocks combine to form carbohydrates when water is squeezed out table sugar cellulose H2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2O

143. 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 HO C H HO C H HO C H HO C H HO 5 CH 2 O + energy + catalyst deoxyribose ribose

144. H N N N C N C H C H C H C H N C H N C H N nucleic acids are building blocks for energy and information in ATP, RNA... C H N C H N C H N 5 HCN + energy + catalyst adenine

145. R Pi Nucleotides are combinations of nucleic acids, ribose sugar, and inorganic phosphate A PiPi PiPi PiPi R H2OH2OH2OH2O UGCT D triphosphates transport energy for transfer RNAs, membrane synthesis, and sugar synthesis. monophosphates relay signals within a cell

146. nucleotide building blocks combine to form RNA and DNA when water is squeezed out R A PiPi R U PiPi R C PiPi R A PiPi R G PiPi H2OH2OH2OH2OH2OH2OH2OH2O C H H O C H H O C H H O C H H O C H H O

147. O C H N O C H H H H C H N amino acids are readily made from simple molecules by adding energy C H HO O H H water formaldehyde hydrogen cyanide glycine

148. O C H N O C H H H H C H N amino acids are readily made from simple molecules by adding energy C R HO O H H water “R”-aldehyde hydrogen cyanide generic amino acid

149. O C SH N amino acids are building blocks of proteins that function as enzymes and structures O C H N O C H H H H C O C H N O C H H H H H H C N C O C H N O C H H H H H C C C C C C C H H H H H H all 20 amino acids have the same backbone and all have H and OH on the ends

150. ribosomes synthesize proteins by translating mRNA to tRNAs that are attached to amino acids 2 1 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 45 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 H2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2O after Trefil and Hazen The Sciences: An Integrated Approach

151. not necessarily an intelligent design ribosomes 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 A A C UC C UG A UG C UC A GU G UC A AA U AC G CG U A after Trefil and Hazen The Sciences: An Integrated Approach Ala His Tyr ValThr Val Arg Leu Gly H2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2OH2O some of the 20 amino acids are represented by more than one of the 64 triplet codons

152. Catalysts are vital to many processes: Proteins help produce complex molecules after Trefil and Hazen The Sciences: An Integrated Approach Modern cellular processes are highly regulated

153. DNA+RNA+Protein World RNA+Protein World RNA World Peptide (PNA) World? Thioester World? Clay World? Which self-replicating molecules came first? no record of early biochemistry

154. Molecular and metabolic evolution may be relatively simple and rapid Chance affects diversity and abundance Necessity provides natural selection All inheritable biological changes are based on molecular evolution D A PiPi D T PiPi D C PiPi D A PiPi D G PiPi

155. 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? Ala His Tyr ValThr Val Arg Leu Gly

156. 1 5 2 3 2 1 A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A How does information evolve? 2 1 3 4 2 3 2 1 3 2 1 3 4 5 duplication

157. 4 5 1 5 2 3 2 1 A U G C A U G C G U A U G U U A C A G U C C G A C U A G G A U G A How does information evolve? 2 1 3 4 2 3 2 1 3 2 1 3 deletion and insertion

158. Ala His Tyr ValThr Val Arg Leu Gly D A PiPi D T PiPi D C PiPi D A PiPi D G PiPi R C C C C C C C C PiPi C C C C C C C C C H O H C H C HO C H H O C H H O H H O C H H O R A PiPi PiPi PiPi C N C O C H N O C H H H H H C C C C C C C H H H H H H 2 1 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 C G C G U A The Facts of Life All cells come from other cells All cells have membranes, proteins, carbs, & DNA All cells use similar metabolic processes All cells use the same genetic code for replication All cells descended from a last common ancestor The first cells came from non-cellular materials and were much simpler than any modern cells

159. http://www.its.caltech.edu/~atomic/snowcrystals/photos/photos.htm Let me be crystal clear: Complex patterns do not require intelligent designers!

160. Eukaryotes are world champs of multicellularity and cell differentiation Identical cells differentiate to develop into a multicellular organism Identical Cells Multiply by Dividing

161. Last common ancestor appears LCA branches into archaebacteria, eubacteria, and eukaryote predecessors metabolic processes diversify autotrophs 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 archaea eucarya LCA lateral and vertical gene transfer proto cell protocells feed on molecules replication processes evolve metabolic processes evolve

162. Eukarya Archaea Bacteria Eukarya Multicellularity (the labeled branches) evolved independently a 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 algae Green algae Plants Brown algae Diatoms Ciliates Sorogena Myxomycetes Cellular slime molds Foraminifera Methanosarcina Myxobacteria Cyanobacteria Actinomycetes last common ancestor

163. 2 8 32 128 2 4 8 16