The quest for H$_3^+$ at Neptune: deep burn observations with NASA IRTF iSHELL

TL;DR

This study used the iSHELL instrument to search for H$_3^+$ emission at Neptune, setting new upper limits that challenge existing models and suggest the need for revised atmospheric dynamics understanding.

Contribution

First near-infrared spectral observations of Neptune with iSHELL that establish the most stringent upper limit on H$_3^+$ density to date.

Findings

No H$_3^+$ emission detected at Neptune.

Upper limit on H$_3^+$ density is 30% lower than previous constraints.

Models overestimate H$_3^+$ density by at least a factor of 5.

Abstract

Emission from the molecular ion H$_3^+$ is a powerful diagnostic of the upper atmosphere of Jupiter, Saturn, and Uranus, but it remains undetected at Neptune. In search of this emission, we present near-infrared spectral observations of Neptune between 3.93 and 4.00 $\mu$m taken with the newly commissioned iSHELL instrument on the NASA Infrared Telescope Facility in Hawaii, obtained 17-20 August 2017. We spent 15.4 h integrating across the disk of the planet, yet were unable to unambiguously identify any H$_3^+$ line emissions. Assuming a temperature of 550 K, we derive an upper limit on the column integrated density of $1.0^{+1.2}_{-0.8}\times10^{13}$ m$^{-2}$, which is an improvement of 30\% on the best previous observational constraint. This result means that models are over-estimating the density by at least a factor of 5, highlighting the need for renewed modelling efforts. A potential solution is strong vertical mixing of polyatomic neutral species from Neptune's upper stratosphere to the thermosphere, reacting with H$_3^+$, thus greatly reducing the column integrated H$_3^+$ densities. This upper limit also provide constraints on future attempts at detecting H$_3^+$ using the James Webb Space Telescope.