2. Life on Our Evolving Planet optical physicist in aerospace for twenty years designed and analyzed laser optical systems Informal science educator in Morro Bay State Park Museum of Natural History for ten years 5 global evolution walks in parks 12 animated slide shows in museum 3 poster exhibits in museum and at Cal Poly Cal Poly adjunct physics professor for seven years and research scholar in residence 4 senior projects Phys 461-464 8 summer student projects 13 special problems projects (Phys, Geol, Bio, Chem 200 or 400) Phys470 Advanced Topics: Solar and Global Evolution visit my website at www.calpoly.edu/~rfieldwww.calpoly.edu/~rfield Bob Field

3. What is a system? Is the system open or closed? a system has parts that interact and may have emergent properties Dr Art Sussman’s Guide to Planet Earth energy flows, matter cycles, web of life energy matter energy matter

4. 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 that it is the role of science to provide plausible natural explanations of natural phenomena

5. Simple building blocks evolve into complex systems when energy flows Everything Evolves oceans and atmosphere solid Earth and Sun molecules and cells organisms and ecosystems

6. 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 Big stars build big atoms Sunlight is the waste product Sun fuses 4 H 1 → He 4

7. composition in our LANL solar evolution code sun composition by mass

8. about 93% CHO by mass Simple building blocks

9. about 97% CHO by mass Complex Systems

10. wikipedia elemental composition of the oceanand the atmosphere composition by mass

11. McDonough Elemental Composition of the Earth composition by mass

12. 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 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

13. 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

14. 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 algae fungus plant animal energy matter energy matter

15. 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 composition by number of atoms

16. atoms can share or transfer electrons H – 1 He – 0 O – 2 C – 4 N – 3 S – 2 P – 3 or 5 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

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

18. 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

19. 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

20. 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

21. 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

22. low tide in Corallina Cove - Montana de Oro  Bob Field 2000

23. Moon core lower mantle upper mantle oceanic lithosphere oceanic crust oceans biosphere atmosphere subcontinental lithosphere sediments lower crust upper crust impacts Interactions between Earth systems Condie33 Fig 1.33 sun when energy flows, complexity grows

24. Solar and Global Evolution are parts of Cosmic Evolution generic system average power density (W/kg) galaxies0.00005 stars0.0002 planets0.01 plants0.1 animals2 brains15 society50 table from Chaisson139 when energy flows, complexity grows

26. 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

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

28. 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 SystemSunSolid Earth

29. 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. HydrosphereAtmosphereGeobiosphere

30. 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 CellsOrganisms and EcosystemsAstronauts

31. 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?

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

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

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

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

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

37. 4 MY 4 BY http://geology.wr.usgs.gov/parks/gtime/Gtimescale.pdf

38. 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

39. 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 3800 ?The Earth's crust solidifies--formation of the oldest rocks found on Earth 3800 ?Condensation of atmospheric water into oceans 3500-2800Prokaryotic cell organisms (eubacteria and archaebacteria) develop 3500-2800 Beginning of photosynthesis by cyanobacteria which releases oxygen molecules into the atmosphere and steadily works to strengthen the ozone layer and change the Earth's chemically reducing atmosphere into a chemically oxidizing one 2400 Rise in the concentration of oxygen molecules stops the deposition of uraninites (since they are soluble when combined with oxygen) and starts the deposition of banded iron formations 1600 The last reserves of reduced iron are used up by the increasing atmospheric oxygen--last banded iron formations 1500Eukaryotic cell organisms develop (common ancestors of algae, fungi, plants, animals) 1500-600Rise of multicellular organisms (algae, fungi, plants, animals) 580-545Fossils of Ediacaran organisms are made (biomineralized bodies) www.talkorigins.org/origins/geo_timeline.html

40. 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

41. Senior Projects, Summer Projects, non-thesis Masters Projects, or Special Problems BIO, CHEM, or GEOL 200 or 400 Students may do library research (books, journals, websites), original thinking, and/or data analysis. Five Billion Years of Global Evolution Identify and sequence globally important physical, chemical, and/or biological events and processes in the five billion year history of the solid Earth, hydrosphere, atmosphere, and/or biosphere (molecules, cells, organisms, and ecosystems) with emphasis on Pre-Cambrian eras. Prokaryote and Eukaryote Evolution Study the structure and evolution of prokaryotes, eukaryotes, biologically important molecules, and/or metabolic processes. Emphasis is on Pre-Cambrian cladograms based on molecular clocks and fossil records. Biochemical and Geochemical Evolution Study biochemical, geochemical, and/or biogeochemical properties and processes from cellular to global scales in Hadean, Archaean, Proterozoic, and/or Phanerozoic Eras.

42. http://en.wikipedia.org/wiki/Bacterium Prokaryote and Eukaryote Evolution

43. Molecular Timescale of Evolution in the Proterozoic by S. Blair Hedges et al in Neoproterozoic Geobiology and Paleobiology edited by Xiao and Kaufman 2003 4112 Archaea 3977 Aquifex 3644 Thermotoga 3096 Chlorobium Cyanobacteria 2688 Firmicutes 2923 Fusobacterium 2800 Proteobacteria 1351 Animals 1458 Fungi 1558 Algae 1609 Algfungimal 1513 Fungimal 2309 Eukaryotes 2100? Respirators 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

44. global average of 40 inches of precipitation per year recycles 120,000 cubic miles of water and transfers heat 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 Biochemical and Geochemical Evolution

45. photic zone (light) aphotic zone (dark) Sun V B GYORIRUV 10% 50' 0' 300' 40' 15' 2' solid Earth Ocean atmosphere where is the biosphere? oceans and atmosphere scatter, absorb, and transfer energy

46. 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

47. 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

48. Temperature of the atmosphere f ocean 10 km sea level Stratosphere Troposphere has 75% of air density and temperature decrease with altitude temperature vs. altitude Sun cool -70F warm 60F ozone layer After Tarbuck

49. Average Global Energy Budget 50 100 20 30 incident sunlight absorb scattered sunlight absorb sea + land atmosphere Sun 30 evap condense 90 65 155 absorb radiate 5 110 105 radiate absorb radiated heat LWIR

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

51. where is the carbon? (billions of metric tons) 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? dissolved gas 40,000

52. Healing Gaia by James Lovelock p139

53. BIO 200 Special Problems in Biological Sciences for lower division undergraduates Joshua Yang - Carbon in the Geobiosphere Tim Tappscott - Prokaryote Evolution Raechel Harnoto – Astrobiology and Global Evolution BIO 100 Orientation to Biological Sciences Introduction to Biological Sciences faculty, department and campus resources, research opportunities, possible careers, studying science, and current topics in biology.

54. convective zone fusion core The Sun creates, stores, and radiates energy radiative zone 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 The Sun evolves because fusion changes the composition of the core which changes density, temperature, and luminosity

55. Guzik Field Lopez x70y28z02 112005

56. Guzik - LANL solar evolution code

58. L = 4πR 2 ·σT 4 Guzik + Field

59. dhillon phy213 website Equations of Stellar Structure

60. Sun

62. greatly simplified H 1 + H 1 → H 2 + e + + υ H 2 + H 1 → He 3 + γ nucleosynthesis: billion years or seconds? e + + e - → γ + γ photons lose energy quickly neutrino escapes from Sun proton turns into neutron

63. million years He 3 + He 3 → He 4 + H 1 + H 1 http://theory.uwinnipeg.ca/mod_tech/node209.html

64. Electrical forces keep protons apart because like charges repel Coulomb Barrier attractiverepulsive Yukawa Attractive Nuclear Potential The rich get richer. If you can climb the rim, you can drop in the crater and gain kinetic energy.

65. 1 2 Never gonna happen, my friend! Proton needs 1000 times more thermal energy than average

66. 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?

67. 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

68. Solar Formation How did a cold dilute gas contract under gravitational attraction and produce a core hot enough and dense enough to sustain thermonuclear fusion? My simplified but detailed explanation of solar formation is more complete than most non-mathematical discussions. 1. Enormous molecular clouds resist gravitational contraction for billions of years with the help of kinetic energy, rotational energy, and magnetic fields until an external perturbation alters the properties of a portion of the cloud enough to trigger free fall contraction as gravitational attraction dominate other influences. 2. My simple explanation of solar formation will ignore rotation and magnetic effects and will assume the cloud is a cold dilute self-gravitating gas with uniform composition, density, and temperature and the mass of the Sun. 3. Gas particles in the cloud accelerate as they fall toward the center of mass because there is no hydrostatic support. 4. Gas density remains uniform as it increases because all particles have the same free fall time since velocity and acceleration increase linearly with radius since a = GM/r 2 = 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.

69. Solar Evolution How can the Sun grow brighter over time while the core hydrogen abundance decreases? 1. Energy generated by fusion replaces energy diffusing from the core to the surface. 2. Nucleosynthesis reduces the core hydrogen abundance and particle density. 3. Some core electrons are annihilated by positrons produced during nucleosynthesis. 4. Core opacity decreases as temperature rises and density of core electrons decrease. 5. The decrease in core particles does not decrease the local energy density or pressure. 6. The core temperature rises as the average energy per particle rises. 7. Decreases in core hydrogen abundance reduce protons available for fusion, but fusion rate increases slightly due to the increased core temperature. 8. Luminosity increases as the temperature and temperature gradient increase and opacity decreases. 9. Increased luminosity increases energy density and pressure at larger radii. 10. Pressure increase expands envelope and forces more particles into core. 11. Core contraction maintains the pressure gradient required for hydrostatic support. 12. Gravitational contraction increases core density, pressure, temperature, and energy density. 13. Fusion rate increases with core density and temperature – enough to sustain higher luminosity. 14. Solar envelope expands as its temperature rises, increasing the surface radius and temperature. 15. The Sun’s luminosity increases as its surface radius and temperature grow over billions of years.

70. Earth creates, stores, and radiates energy 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

71. Earth’s composition evolves as rare but critical elements decay

72. Whole Earth Crust Mantle Core

73. 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

74. 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

75. Mantle Core

76. CMB Mantle Core

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

79. visible radiation optical absorption impedes energy flow From where we sit, brighter than a thousand suns briefly transparent planet

80. thermal conduction thermal scattering impedes energy flow 5000°F 2.5°F/mile or 0.001°F/foot solid planet

81. thermal convection viscosity and density affect energy flow molten planet

82. 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

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

84. 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

85. 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

86. 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

87. 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

88. 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

89. 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

90. 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

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

92. 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

93. 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

94. 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

95. 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

96. 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

97. 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