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\begin{document}

\title{The Meteoric Ni Layer in the Upper Atmosphere}



\author[1]{John Maurice Campbell Plane}%
\author[1]{Shane Daly}%
\author[1]{Wuhu Feng}%
\author[1]{Thomas Peter Mangan}%
\author[2]{Michael Gerding}%
\affil[1]{University of Leeds}%
\affil[2]{Leibniz-Institute of Atmospheric Physics}%


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  \date{May 24, 2024}


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\begin{abstract}
The first global atmospheric model of Ni (WACCM-Ni) has been developed
to understand recent observations of the mesospheric Ni layer by
ground-based resonance lidars. The three components of the model
comprise: the Whole Atmospheric Community Climate Model (WACCM6); a
meteoric input function derived by coupling an astronomical model of
dust sources in the solar system with a chemical meteoric ablation
model; and a comprehensive set of neutral, ion-molecule and
photochemical reactions pertinent to the chemistry of Ni in the upper
atmosphere. In order to achieve closure on the chemistry, the reaction
kinetics of three important reactions were first studied using a fast
flow tube with pulsed laser ablation of a Ni target, yielding k(NiO + O)
= (4.6 +/- 1.4)e-11; k(NiO + CO) = (3.0 +/- 0.5)e-11; and k(NiO2 + O) =
(2.5 +/- 1.2)e-11 cm3 molecule-1 s-1 at 294 K. The photodissociation
rate of NiOH was computed to be J(NiOH) = 0.02 s-1. WACCM-Ni simulates
satisfactorily the observed neutral Ni layer peak height and width, and
Ni measurements from rocket-borne mass spectrometry. The Ni layer is
predicted to have a similar seasonal and latitudinal variation as the Fe
layer, and its usually broad bottom-side compared with Fe is caused by
the relatively fast NiO + CO reaction. The quantum yield for photon
emission from the Ni + O, observed in the nightglow, is estimated to be
between 6 and 40\%.%
\end{abstract}%



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