http://arxiv.org/abs/2012.04971
Various trace species were detected for the first time in the atmosphere of Jupiter with the collision of comet Shoemaker-Levy 9 in July 1994 near 44$^\circ$ S. These trace species can be used to understand the dynamics and chemical mystery in the atmosphere of Jupiter. We present the spectroscopic detection of the emission lines of ethyl cyanide ($^{13}$CH$_3$CH$_2$CN) ($\sim$12$\sigma$) with transition J = 52(5,48)–51(6,45) at frequency $\nu$ = 195.430 GHz and acetone (CH$_3$COCH$_3$) ($\sim$3$\sigma$) with transition J = 50(38,12)–50(37,13)EE at frequency $\nu$=195.721 GHz in the atmosphere of Jupiter using Atacama Large Millimeter/Submillimeter Array (ALMA) with column density N($^{13}$CH$_3$CH$_2$CN) = 3.52$\times$10$^{14}$ cm$^{-2}$ and N(CH$_3$COCH$_3$) = 5.31$\times$10$^{10}$ cm$^{-2}$. We also confirm the presence of water vapour in the atmosphere of Jupiter with the detection of absorption line of water (H$_2$O) at frequency $\nu$ = 183.310 GHz with transition J = 3(1,3)–2(2,2) with column density N(H$_2$O)= 9.25$\times$10$^{14}$ cm$^{-2}$ ($\sim$4.3$\sigma$ statistical significance). We discussed possible photochemical pathways to produce detected organic molecules in the atmosphere of Jupiter.
A. Manna and S. Pal
Thu, 10 Dec 20
32/87
Comments: 11 pages, 2 figures and 1 table. Comments welcome
You must be logged in to post a comment.