## 1 Introduction
During aurora and geomagnetic storm, significant amounts of energy and particles are deposited into the Earth's atmosphere, leading to alterations in its structure, composition, and dynamics. The storm energy dissipates quickly from the atmosphere, and heat balance is achieved through infrared emissions [14; 22; 23; 24]. The cooling process occurs due to the conversion of kinetic energy into radiative energy, which is then released into space and the lower atmosphere [14; 15]. Based on satellite observations and auroral infrared detection experiments [25; 26; 27; 28], it has been found that during the auroral disturbance, 5.3 \(\upmu\)m radiation mainly derives from the \(\mathrm{\Delta v=1}\) band of NO, as shown in reaction (4):  
\[\mathrm{NO(X^{2}\Pi,\
u=1)\to NO(X^{2}\Pi,\
u=0)+h\
u(5.3\ \upmu m)} \tag{4}\]  
The radiation emission of NO 5.3 \(\upmu\)m mainly results from the fundamental transition between adjacent vibrational levels. Under static atmospheric conditions, the inelastic collision between nitric oxide and atomic oxygen primarily generates this radiation [12; 29; 30], although N\({}_{2}\) and O\({}_{2}\) also contribute, but to a lesser extent [31]:  
\[\mathrm{NO(\
u=0)+O\to NO(\
u=1)+O} \tag{5}\]This reaction is a non-elastic collision process with a reaction rate of (4.2 \(\times\) 0.7) \(\times 10^{-11}\)\(\exp(-2700/\mathrm{T})\) cm\({}^{3}\)/s [32; 33], making it the primary source of NO(\(\
u=1\)) in the altitude regions of 110-300 km. Under auroral disturbance conditions, in addition to the reaction (5), another main source of excited-state NO arises from collisions between O\({}_{2}\) and N(\({}^{2}\)D,\({}^{4}\)S) [10; 34; 35]:  
\[\mathrm{N}(^{4}\mathrm{S}\ )+\mathrm{O}_{2}\rightarrow\mathrm{NO}(\
u)+\mathrm{O} \tag{6}\]  
\[\mathrm{N}(^{2}\mathrm{D}\ )+\mathrm{O}_{2}\rightarrow\mathrm{NO}(\
u)+0.9 \mathrm{O}(^{1}\mathrm{D}\ )+0.1\mathrm{O} \tag{7}\]  
The rate of reaction (6) is (1 \(\times\) 10\({}^{-12}\)) \(\exp(-3220/\mathrm{T})\) cm\({}^{3}\)/s, and the rate of reaction (7) is (7.4 \(\times\) 10\({}^{-12}\)) (T/300)\({}^{0.5}\) cm\({}^{3}\)/s; both are temperature-dependent. During auroral events, the temperature of the Earth's thermosphere can increase by several hundred Kelvin due to the energy deposition, and this significant temperature rise can be effectively controlled through radiative cooling processes, as described in the reactions (4) above. Therefore, further exploration of the spatiotemporal variability in NO infrared radiation at 5.3 \(\upmu\)m from the perspective of radiance can provide theoretical support for predicting changes in the auroral parameters caused by disturbances. On the other hand, the enhanced infrared band during an auroral disturbance serves as vital background radiation for various meteorological satellites and spacecrafts. Therefore, studying the important infrared radiation components during auroral disturbance is also crucial. In-depth analyses conducted by [PERSON] et al. [14; 15] on the enhanced NO 5.3 \(\upmu\)m infrared radiation detected by SABER in April 2002 provide a basis for studying the infrared response of thermosphere to strong disturbance events. More recently, [PERSON] et al. [36] and [PERSON] et al. [37] investigated the asymmetry of NO 5.3 \(\upmu\)m radiance between the Northern and Southern hemispheres and its correlation with various factors. [PERSON] et al. [38] analyzed SABER radiation data to investigate the latitudinal and longitudinal variations in cooling rates at the NO 5.3 \(\upmu\)m during the unusual disturbance period in 21-22 January 2005, and examined how radiation cooling rates responded to the anomalous event. This paper includes four sections. The motivation and main purpose of this paper are briefly introduced in Section 1. The datasets used in this study are described in Section 2. The spatiotemporal variations of NO 5.3 \(\upmu\)m radiance during auroral processes and their correlation with temperature, solar wind speed, AE index, and Dst index are mainly discussed in Section 3.