Table 1 Mean XCO values for different atmospheric levels and water enrichments in units of ppb with 1σ uncertainties

From: A supersolar oxygen abundance supported by hydrodynamic modelling of Jupiter’s atmosphere

\({E}_{{{\rm{H}}}_{2}{\rm{O}}}\)

×10

×7

×5

×2.5

×1.25

×0.6

Quench

1.663 ± 0.21

1.414 ± 0.14

1.195 ± 0.11

0.681 ± 0.04

0.359 ± 0.02

0.200 ± 0.006

Specific LCL

0.447 ± 0.19

0.318 ± 0.14

0.333 ± 0.11

0.176 ± 0.07

0.056 ± 0.02

0.013 ± 0.005

Near H2O cloud

0.769 ± 0.13

0.532 ± 0.12

0.561 ± 0.10

0.258 ± 0.05

0.096 ± 0.03

0.040 ± 0.009

\({E}_{{{\rm{H}}}_{2}{\rm{O}}}\)

0.3 × s.f. = 0.1

0.3 × s.f. = 1.0

0.3 × s.f. = 10

0.3 × s.f. = 500

2.5 × s.f. = 500

Quench

0.023 ± 0.001

0.098 ± 0.004

0.210 ± 0.04

0.386 ± 0.12

3.203 ± 1.44

Specific LCL

0.002 ± 0.0008

0.007 ± 0.002

0.015 ± 0.005

0.013 ± 0.004

0.5160 ± 0.16

Near H2O cloud

0.008 ± 0.001

0.024 ± 0.005

0.052 ± 0.012

0.041 ± 0.007

0.828 ± 0.17

  1. The quench-region values are typically representative of the 400–450 bar regime (corresponding to about 1,000 K) and were derived using Fig. 1a, whereas the specific LCL values were taken from Fig. 2 using the peaks of the static stability. We have also tabulated the values near the region associated with Jupiter’s water cloud deck. s.f. indicates the time scaling factor for the CO/CH4 interconversion (see text). The top three rows were calculated using the V12 network, whereas the bottom three were calculated for different scaling factors that approximate the effect of slow CH4 destruction.
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