Abstract Details
(2020) Origin and Distribution of Volatile Elements in the Early Solar System
Füri E
https://doi.org/10.46427/gold2020.771
The author has not provided any additional details.
01c: Plenary Hall, Thursday 25th June 05:57 - 06:00
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Submitted by Xin Yang on Thursday 18th June 00:39
How do you quantify the amount of solar wind noble gas, given that the noble gas found in meteorites can be attributed to many processes like spallation reactions caused by cosmic rays? Best regards
Solar wind-derived noble gases are implanted at the surface of a meteorite; they likely represent a minor component in most samples. SW-derived noble gases can be extracted at low temperature (for example during step-wise heating analysis), whereas cosmogenic noble gases are only released at high temperatures. In addition, SW-derived and cosmogenic noble gases can easily be distinguished based on their diagnostic isotope ratios (e.g., 20Ne/22Ne - 21Ne/22Ne).
How do you quantify the amount of solar wind noble gas, given that the noble gas found in meteorites can be attributed to many processes like spallation reactions caused by cosmic rays? Best regards
Solar wind-derived noble gases are implanted at the surface of a meteorite; they likely represent a minor component in most samples. SW-derived noble gases can be extracted at low temperature (for example during step-wise heating analysis), whereas cosmogenic noble gases are only released at high temperatures. In addition, SW-derived and cosmogenic noble gases can easily be distinguished based on their diagnostic isotope ratios (e.g., 20Ne/22Ne - 21Ne/22Ne).
Submitted by My Riebe on Sunday 21st June 07:54
Could you expand a bit on what could have caused enstatite chondrites to be water poor but not volatile poor?
Carbonaceous chondrites have likely accreted water ice, whereas enstatite chondrites (inward of the snow line?) did not. Carbon and nitrogen predominantly occur in the form of organic matter dispersed in the matrix of carbonaceous chondrites, and in the form of reduced species (graphite, carbides, nitrides) in enstatite chondrites (e.g., Grady and Wright, Space Science Reviews, 2003). This suggests that the accretion and retention of nominally volatile elements (C, N) in the inner regions of the disk may have been facilitated by different oxidation states. The solubility of nitrogen, for example, in silicate melts is significantly enhanced at reducing conditions. Also note that carbonaceous chondrites themselves record a wide range of carbon (~0.2 to ~5 wt.%) and nitrogen (~0.01 to 0.5 wt.%) abundances. -> See also Braukmüller et al. for other 'volatile' elements
Could you expand a bit on what could have caused enstatite chondrites to be water poor but not volatile poor?
Carbonaceous chondrites have likely accreted water ice, whereas enstatite chondrites (inward of the snow line?) did not. Carbon and nitrogen predominantly occur in the form of organic matter dispersed in the matrix of carbonaceous chondrites, and in the form of reduced species (graphite, carbides, nitrides) in enstatite chondrites (e.g., Grady and Wright, Space Science Reviews, 2003). This suggests that the accretion and retention of nominally volatile elements (C, N) in the inner regions of the disk may have been facilitated by different oxidation states. The solubility of nitrogen, for example, in silicate melts is significantly enhanced at reducing conditions. Also note that carbonaceous chondrites themselves record a wide range of carbon (~0.2 to ~5 wt.%) and nitrogen (~0.01 to 0.5 wt.%) abundances. -> See also Braukmüller et al. for other 'volatile' elements
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