In the beginning… The composition of the solar system and earth.
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Transcript of In the beginning… The composition of the solar system and earth.
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In the beginning…
The composition of the solar system and earth
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Interior of the Genesis sample collection module
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The Genesis sample collection module after ‘landing’
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Picking through the pieces
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Features that demand an explanation:• H and He are by far most abundant elements• Li, Be and B are anomalously low in abundance• Overall ~ exponential drop in abundance with increasing Z• Even Z > odd Z• Fe and neighbors are anomalously abundant
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“Hydrogen as food’ hypothesis: Burbidge et al., 1957(built on ideas of Gamow re. nucleosynthesis in big bang)
I. H burning
H + H = D + + + +
positron neutrino
photonsD +H = 3He + …
3He + 3He = 4He + 2H + …
3He + 4He = 7Be + … (and similar reactions to make Li and B)
Products quickly decay:7Be + e- = 7Li
7Li + P = 8Be8Be = 2.4He
Timescale ~ 10-16 s { Stuck; no way to elements heavier than B
(rxn. discovered by H. Bethe, 1939)
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Willie Fowler, Salpeter and Hoyle
“Would you not say to yourself, 'Some super- calculating intellect must have designed the properties of the carbon atom, otherwise the chance of my finding such an atom through the blind forces of nature would be utterly minuscule.' Of course you would . . .. A common sense interpretation of the facts suggests that a superintellect has monkeyed with physics, as well as with chemistry and biology, and that there are no blind forces worth speaking about in nature. The numbers one calculates from the facts seem to me so overwhelming as to put this conclusion almost beyond question.”
F. Hoyle
Show the solution is the following reaction in red giant stars:
4He + 4He + 4He = 12C
Opens possibility of many similar reactions:
12C + 4He = 16O16O + 4He = 20Ne
20Ne + 4He = 24Mg
Collectively referred to as ‘He burning’
“We do not argue with the critic who urges that stars are not hot enough for this process; we tell him to go and find a hotter place.”A. Eddington
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Advanced burning:
origin of the 2nd quartile of the mass range
12C + 12C = 23Na + H
16O + 16O = 28Si + 4He
CNO cycle
12C + P = 13N = 13C13C + P = 14N14N + P = 15O = 15N15N + P = 12C + 4He
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The E process (for ‘Equilibrium’): why the cores of planets are Fe-richA quasi-equilibrium between proton+neutron addition + photo-degradation
Promotes nuclei with high binding energy per nucleon
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Neutron capture as a mode of synthesizing heavy elements
Occurs in environments rich in high-energy neutrons, such as super-novae
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Features that demand an explanation:• H and He are by far most abundant elements
H primordial; He consequence of 1˚ generation H burning
• Li, Be and B are anomalously low in abundanceConsumed in He burning
• Overall ~ exponential drop in abundance with increasing ZDrop in bonding energy per nucleon w/ increasing Z
• Even Z > odd ZMemory of He burning
• Fe and neighbors are anomalously abundantMaximum in bonding energy per nucleon at Fe
These factors are directly responsible for the fact that terrestrial planets are made of silicates and oxides (‘rocks’) with magnetic Fe cores.
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N
Primitive meteorites look a lot like the sun (minus the gas and all the hotness)
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II. Accretion of the Earth
(and inheritance of interstellar dust)
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letters indicate compositional fields of various
types of primitive meteorites
Earth is somewhere near here
But primitive meteorites are diverse; how are we to know whichis most like the earth?
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Much of the diversity in meteorite composition reflects variations in oxidation state of solar nebula (H2O/CO ratio)
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Infer the earth based on ‘geochemical’ vs. ‘cosmochemical’diversity in composition
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Broad groupings of elements in geochemical processes
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The earth’s mantle is mostly chondritic, but depleted in moderately volatile elements (K, Na)
Silicate earthCI chondrites
Are they simply missing, or hiding somewhere in the earth? We’ll revisit this question in two lectures
1
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The earth’s mantle is also depleted in siderophile elements (Ni, Cu, Au)
Silicate earthCI chondrites
0.1
Are they simply missing, or hiding somewhere in the earth? We’ll revisit this question next lecture
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Entry speed estimated bythermally stepped He release method
>18 km/s probable comet origin
<14 km/s probable asteroid origin
Stratospheric IDPs
2µm- 25µm et particlesCollected by NASA
U2/ER2/WB-57F aircraft
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1 ng IDP >105 components Contents: anhydrous silicate minerals
amorphous silicate (glass)Fe, Ni sulfidesoxidesFe, Ni metal grainsorganic materials
1 µm
bulk composition ~ solarbulk composition ~ solar
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“Kuiper Belt” around HR 4796A
Samples from the Kuiper Belt(Neptune and beyond)
The ‘Stardust’ mission
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Wild 2 encounter1/2/2004
direction of interstellar flux
Launch2/7/99
Earth gravity
Assist1/15/2001
Earth return
1/15/2006
Wild 2 orbit
Loop #1
Loops #2 & 3
Interstellar dustCollection periods
Stardust’s Wild Ride - 3 loops around the Sun
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January 15, 2006
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A piece of ‘star dust’