Thermospheric neutral temperatures derived from charge-exchange produced N 2 + Meinel (1,0) rotational distributions

• Published in: Annales Geophysicae
• Main Authors: C. K. Mutiso, M. D. Zettergren, J. M. Hughes, G. G. Sivjee
• Format: Article in Journal/Newspaper
• Language: English
• Published: Copernicus Publications 2013
• Subjects: Science; Q; Physics; QC1-999; Geophysics. Cosmic physics; QC801-809; Norway; Svalbard
• Online Access: https://doi.org/10.5194/angeo-31-463-2013; https://doaj.org/article/aa514b3512254bbcb14d6431a4c5f65d

Thermalized rotational distributions of neutral and ionized N 2 and O 2 have long been used to determine neutral temperatures ( T n ) during auroral conditions. In both bright E-region (≲150 km) auroras, and in higher-altitude auroras, spectral distributions of molecular emissions employed to determine T n in the E-region cannot likewise be used to obtain T n in the F-region. Nevertheless, charge-exchange reactions between high-altitude (≳130 km) species provide an exception to this situation. In particular, the charge-exchange reaction O + ( 2 D) + N 2 (X) → N + 2 (A 2 Π u , ν' = 1 + O( 3 P) yields thermalized N 2 + Meinel (1,0) emissions, which, albeit weak, can be used to derive neutral temperatures at altitudes of ~130 km and higher. In this work, we present N 2 + Meinel (1,0) rotational temperatures and brightnesses obtained at Svalbard, Norway, during various auroral conditions. We calculate T n at thermospheric altitudes of 130–180 km from thermalized rotational populations of N 2 + Meinel (1,0); these emissions are excited by soft electron (≲1 keV) impact and charge-exchange reactions. We model the contributions of the respective excitation mechanisms, and compare derived brightnesses to observations. The agreement between the two is good. Emission heights obtained from optical data, modeling, and ISR data are consistent. Obtaining thermospheric T n from charge-exchange excited N 2 + Meinel (1,0) emissions provides an additional means of remotely sensing the neutral atmosphere, although certain limiting conditions are necessary. These include precipitation of low-energy electrons, and a non-sunlit emitting layer.