| | |
| | |
Stat |
Members: 3643 Articles: 2'487'895 Articles rated: 2609
28 March 2024 |
|
| | | |
|
Article overview
| |
|
Mapping Vinyl Cyanide and Other Nitriles in Titan's Atmosphere Using ALMA | J. C.-Y. Lai
; M. A. Cordiner
; C. A. Nixon
; R. K. Achterberg
; E. M. Molter
; N. A. Teanby
; M. Y. Palmer
; S. B. Charnley
; J. E. Lindberg
; Z. Kisiel
; M. J. Mumma
; P. G. J. Irwin
; | Date: |
17 Oct 2017 | Abstract: | Vinyl cyanide (C$_2$H$_3$CN) is theorized to form in Titan’s atmosphere via
high-altitude photochemistry and is of interest regarding the astrobiology of
cold planetary surfaces due to its predicted ability to form cell membrane-like
structures (azotosomes) in liquid methane. In this work, we follow up on the
initial spectroscopic detection of C$_2$H$_3$CN on Titan by Palmer et al.
(2017) with the detection of three new C$_2$H$_3$CN rotational emission lines
at submillimeter frequencies. These new, high-resolution detections have
allowed for the first spatial distribution mapping of C$_2$H$_3$CN on Titan. We
present simultaneous observations of C$_2$H$_5$CN, HC$_3$N, and CH$_3$CN
emission, and obtain the first (tentative) detection of C$_3$H$_8$ (propane) at
radio wavelengths. We present disk-averaged vertical abundance profiles,
two-dimensional spatial maps, and latitudinal flux profiles for the observed
nitriles. Similarly to HC$_3$N and C$_2$H$_5$CN, which are theorized to be
short-lived in Titan’s atmosphere, C$_2$H$_3$CN is most abundant over the
southern (winter) pole, whereas the longer-lived CH$_3$CN is more concentrated
in the north. This abundance pattern is consistent with the combined effects of
high-altitude photochemical production, poleward advection, and the subsequent
reversal of Titan’s atmospheric circulation system following the recent
transition from northern to southern winter. We confirm that C$_2$H$_3$CN and
C$_2$H$_5$CN are most abundant at altitudes above 200 km. Using a 300 km step
model, the average abundance of C$_2$H$_3$CN is found to be $3.03pm0.29$ ppb,
with a C$_2$H$_5$CN/C$_2$H$_3$CN abundance ratio of $2.43pm0.26$. Our HC$_3$N
and CH$_3$CN spectra can be accurately modeled using abundance gradients above
the tropopause, with fractional scale-heights of $2.05pm0.16$ and
$1.63pm0.02$, respectively. | Source: | arXiv, 1710.6411 | Services: | Forum | Review | PDF | Favorites |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser claudebot
|
| |
|
|
|
| News, job offers and information for researchers and scientists:
| |