Outline: Cosmological Origins. The true basics of life The age of Earth and the Universe The origin of the heavy elements Molecules in space

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1 Outline: Cosmological Origins The true basics of life The age of Earth and the Universe The origin of the heavy elements Molecules in space

2 Reminder: HW #1 due in one week Homework is on class webpage (under Assignments ) Due at beginning of class, Tuesday, September 16

3 What is Required for Life? Carbon? Liquid water? Rocky planets? Time? Since we don t know of other life yet, we have to be cautious. What is absolutely necessary?

4 Is Carbon Required?

Possible Carbon Alternatives? http://facstaff.

5 Possible Carbon Alternatives?

6 Example: Silicon-Based? Maybe, but Lots of sand on Earth, though, and yet no life based on silicon In future, might be artificial Si-based life

7 Is Water Required?

8 Survival of Desiccation Many creatures can survive without water However, none that we know can grow and reproduce without water Could methane (CH 4 ) or ammonia (NH 3 ) work? Bdelloid rotifer

9 Is a Rocky Planet Necessary? Surface, liquids seem nice for life But could life emerge on a star? In interstellar space? On gas giant? Elsewhere? What do you think? Life on a neutron star???

10 Are Heavy Elements Needed? A common theme here is that we need some heavy elements If silicon etc. substitute for carbon, those are still heavy If methane, ammonia, or whatever substitute for water, those still require carbon or nitrogen.

11 A Long Time? On Earth, took ~3 Gyr to go from life to multicellular life Short, fast, average??? We do know that big changes require millions of years here Reasonable to expect the same elsewhere?

12 Speedup or Slowdown of Life? Suppose Earth had fewer radioactive elements, or more protection from Sun s UV Fewer mutations Would life have progressed faster (not as many mistakes ) or slower (not as many prospects for innovation)?

13 Complex Chemistry All Earth life has H, C, N, O, P, S Is this critical? Don t know, but if we are limited to H & He, complex molecules can t form Assume need atoms heavier than He

14 A Non-Uniform Universe Completely uniform means no complexity Need some structure to distinguish parts Gravity makes dense parts denser Amazingly, this is enough to make current universe We re x average! Illustris

15 The Age of Earth and the Universe Claim: billions of years But how do we know? Oldest human ~100 yr Civilization ~10,000 yr In general, how can we measure things far outside our realm of experience?

16 Inference Outside Experience Have model for how things behave Model extensively tested in many circumstances, giving correct answer Therefore, we can believe answers in realms we don t experience directly But in such cases we need multiple checks to our answers

17 Radioactive Decay, Part 1 Atoms made of electrons and nuclei (protons, neutrons). Type of element depends only on proton number Some nuclei decay eventually into other nuclei: unstable

$against temperature, pressure, etc. Thus, fraction left acts as great clock! http://www.visionlearning.$

18 Radioactive Decay, Part 2 Decay is statistical: can t predict in advance Concept of half-life: time needed for half of nuclei to decay Half-life is robust against temperature, pressure, etc. Thus, fraction left acts as great clock!

Example: Carbon-14 Dating Normal carbon: C-12 C-14 decays to N-14 5730 yr half-life In balance for live things Decreases after death Dates calibrated variously

19 Example: Carbon-14 Dating Normal carbon: C-12 C-14 decays to N yr half-life In balance for live things Decreases after death Dates calibrated variously to >9000 yr Dendrochronology! (tree-ring dating) Useful for <50,000 yr Need something else!

20 Longer Decays: e.g., Uranium Uranium decays to thorium Half-life 4.5 billion years Well-matched to age of Earth

21 Results of Radioactive Dating Solar System is 4.55 Gyr old Low uncertainty Universe must be at least this old What other methods can we use? Chondrite, 4.55 Gyr old

biggest? Use to find age Oldest: 11-13 Gyr http://www.aetheoraem.

22 Stellar Evolution We only see snapshots of star lives, but understand them well Small stars live longer than big stars Cluster of stars Formed at same time How big is biggest? Use to find age Oldest: Gyr Globular cluster M80

23 Cooling of White Dwarfs WD: size of Earth, mass of Sun Endpoint of some stars No energy source, so they just cool forever Simple objects: measure temperature to find age Result: some >12 Gyr

24 Background Radiation Universe became transparent after expanding Radiation from then has informative bumps Tells us that the Universe is 13.8 ± 0.1 Gyr old Note: consistent with other estimates Microwave photo of sky from NASA s WMAP satellite

25 How Quickly Could Life Develop? A thousand years after Big Bang? A million? A billion? Basically, enough time was needed for molecules to form. When did this happen?

26 Is Hydrogen Enough? H can form molecules with itself: H 2 However, long H 2 chains are not stable From computer science perspective, not enough information! Needs other atoms Only possibilities: H 2

least interactive of all elements Nothing doing! http://aspire.

27 How About Helium? Even worse! Helium already fills both slots in inner electron shell It is the least interactive of all elements Nothing doing!

$the fraction of mass$

28 Lithium, Beryllium, Boron? To be open-minded, maybe these work But the fraction of mass in these atoms is tiny Look for others

29 Carbon, Nitrogen, Oxygen? Finally! These are common and have very flexible chemistry (especially carbon) We probably need them Have they existed since the beginning of the universe?

Universe Requires high temperature and density, long time à Cores of

30 Making Heavy Elements Need 3He à C, but 2He are unstable Bind temporarily, then another He comes by Nearly impossible in early Universe Requires high temperature and density, long time à Cores of massive stars

31 Heavier and Heavier Can make nitrogen, oxygen, up to iron and nickel in this way Most stars too cold Beyond iron/nickel, does not release energy Core collapses Kaboom! Supernova... Pre-supernova star

32 Getting the Lead Out All of this is very well, but need to distribute the elements for life! (and other stuff too) Stellar winds? Weak for Sun-type Stronger for massive stars Supernovae Distributes almost everything! We are made of star stuff Crab SN remnant

33 Solar Elemental Abundances Lots of H, He Main elements produced by fusion are abundant: C, N, O, Ne, Mg, Si, S, Fe Silicon and iron (make up rocky planets) are about 10-4 of H

34 Earliest Time for Life? Earliest stars: 10 8 to 10 9 yr after Big Bang Many are massive Plenty of supernovae In principle, life could have started forming around 10 Gyr before we appeared But amount of heavy elements was small on average Simulation of first star

35 Molecules in Space We argued we need complex molecules for life Is this unique to Earth, or is it elsewhere? First, how might we detect molecules in other places?

36 Spectra of Molecules We can detect atoms by their specific interactions with light Same with molecules, but lower energy Typically radio waves Stars are too hot; look at cold regions such as molecular clouds Formaldehyde

37 What Has Been Detected? H 2, easily (most common molecule) CO, SiO, OH, NaCl and many others But what about organic molecules? Have they been seen in space? Spectrum of molecular cloud

38 Organic Molecules in Space Yes!! Close to 200 so far (with up to 13 atoms) Sugars, alcohol(!) Most importantly: simplest (10 atoms) amino acid, glycine Apparently the building blocks of life are out there...

39 Summary Universe is about 13.8 Gyr old Plenty of time for life, in principle Need complex chemistry H and He not enough, need CNO Heavy elements are produced in stars In cold, dense environments, many organic molecules have been detected

The Content of the Universe, and how we get heavy elements.

The Content of the Universe, and how we get heavy elements http://www.lbl.gov/science-articles/archive/sabl/2006/jan/pie-chart.jpg 1 Outline The content of the universe How structure forms Elements heavier