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26 April 2024 |
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Nature's Starships II: Simulating the Synthesis of Amino Acids in Meteorite Parent Bodies | | Alyssa K. Cobb
; Ralph E. Pudritz
; Ben K. D. Pearce
; | | Date: |
22 Jun 2015 | | Abstract: | Carbonaceous chondrite meteorites are known for having high water and organic
material contents, including amino acids. Here we address the origin of amino
acids in the warm interiors of their parent bodies (planetesimals) within a few
million years of their formation, and connect this with the astrochemistry of
their natal protostellar disks. We compute both the total amino acid abundance
pattern as well as the relative frequencies of amino acids within the CM2 (e.g.
Murchison) and CR2 chondrite subclasses based on Strecker reactions within
these bodies. We match the relative frequencies to well within an order of
magnitude among both CM2 and CR2 meteorites for parent body temperatures $<$
200$^{circ}$C. These temperatures agree with 3D models of young planetesimal
interiors. We find theoretical abundances of approximately 7x10$^5$
parts-per-billion (ppb), which is in agreement with the average observed
abundance in CR2 meteorites of 4$pm$7x10$^5$, but an order of magnitude higher
than the average observed abundance in CM2 meteorites of 2$pm$2x10$^4$. We
find that the production of hydroxy acids could be favoured over the production
of amino acids within certain meteorite parent bodies (e.g. CI1, CM2) but not
others (e.g. CR2). This could be due to the relatively lower NH$_3$ abundances
within CI1 and CM2 meteorite parent bodies, which leads to less amino acid
synthesis. We also find that the water content in planetesimals is likely to be
the main cause of variance between carbonaceous chondrites of the same
subclass. We propose that amino acid abundances are primarily dependent on the
ammonia and water content of planetesimals that are formed in chemically
distinct regions within their natal protostellar disks. | | Source: | arXiv, 1506.6740 | | Services: | Forum | Review | PDF | Favorites | |
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