Spatio-temporal variation characteristics of the Mars surface brightness temperature

	Spatio-temporal variation characteristics of the Mars surface brightness temperature
	Jia, Mengna 1; Di, Kaichang 1; Yue, Zongyu 1; Sun, Shujuan 1
刊名	Yaogan Xuebao/Journal of Remote Sensing
	2016
卷号	20 期号:4 页码:632-642
通讯作者	Di, Kaichang (dikc@radi.ac.cn)
英文摘要	This paper presents a comprehensive analysis of the patterns of spatio-temporal variations in the Mars Surface Brightness Temperature (SBT) by using thermal infrared data acquired by three orbiters. Inter-annual changes in SBT are determined by comparing temperature data from different thermal infrared sensors, with spectral and local time corrections. Seasonal variations in the northern (NH) and southern (SH) hemisphere night SBT are presented with four Mars-year Thermal Emission Spectrometer (TES) data. The influences of the latitude and altitude on night SBT are analyzed based on TES measurements. The discrepancies between the adjusted Infrared Thermal Mapper (IRTM) band-B and the Mars Climate Sounder (MCS) band-A4 measurements are 1.3 K and 1.0 K for day and night SBT, respectively. The differences between the IRTM band-B and the average TES Mars Year (MY) 24-26 are 3.1 K and 2.1 K for day and night SBT, respectively. During the aphelion period, seasonal changes in SH night SBT conform well to the sine curve, and the inter-annual variation is lower than 3 K. However, the seasonal variation greatly diverges from the sine curve; the inter-annual difference is significant during the perihelion period. By contrast, NH night SBT exhibits no clear seasonal trend; the variation of this parameter is smaller than that of SH. No signs of the sine-curve pattern are displayed. Night SBT increased by approximately 17 K in NH and SH during the MY 25 global dust storm. When Ls is 115°-125°, NH SBT is obviously influenced by topography, whereas the SH SBT isotherms are nearly parallel to the latitude lines. Some plains, such as Acidalia Planitia, Chryse Planitia, Isidis Planitia, and Utopia Planitia, are warmer than their surrounding areas; moreover, high-altitude regions, including Arsia Mons, Alba Patera, Elysium Mons, Terra Sabaea, and Olympus Mons, have almost the lowest SBT, except for the Polar regions. When Ls is 295°-315°, the SH isotherms are fragmentized, which corresponds to the cratered surfaces. The NH isotherms in winter are only parallel to the latitude lines north of 50°N. The maximum SBT gradually decreased from the equator to the poles, except for 35°S. The minimum SBT between 15°S and 35°N are lower than that of the higher latitude regions because of the influence of to pography. The SBT standard deviations and differences between maxima and minima reveal the same law, that is, the closer to the equator, the higher are both values. Conclusions: The following conclusions are reached. (1) The 5 Mars-year inter-annual variation in SBT is within the precision range of measurement and processing; thus, the detection of Mars climate change is not feasible using current thermal infrared measurements. (2) The inter-annual difference in SBT during the perihelion period is higher than that during the aphelion period. The amplitude of seasonal variations in NH is smaller than that in SH. Increased SBT in NH caused by dust storm is higher than that caused by increased solar radiation in summer. Low-altitude topographies, such as basin sand canyons, exhibit higher temperatures than high-altitude topographies, such as mountains, terrains, and plateaus. Night SBT exhibits a strong negative correlation with altitude in Olympus Mons. The linear fitting result indicates that night SBT decreases by approximately 1.4 K as the altitude increases by 1 km. Night SBT at low latitudes is generally higher than that at high latitudes. Influenced by factors, such as topography, the SBT maximum exists at 35°S instead of the equator. The SBT minima at the latitudes close to the equator are smaller than those at high latitudes. The lowlatitude SBT varies more intensely than those near the polar latitudes. © 2016, Science Press. All right reserved.
收录类别	EI
语种	中文
WOS记录号	WOS:20163202695325
内容类型	期刊论文
源URL	[http://ir.radi.ac.cn/handle/183411/39580]
专题	遥感与数字地球研究所_SCI/EI期刊论文_期刊论文
作者单位	1. State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing Applications of Chinese Academy of Sciences, Beijing 2.100101, China 3. University of Chinese Academy of Sciences, Beijing 4.100049, China
推荐引用方式 GB/T 7714	Jia, Mengna,Di, Kaichang,Yue, Zongyu,et al. Spatio-temporal variation characteristics of the Mars surface brightness temperature[J]. Yaogan Xuebao/Journal of Remote Sensing,2016,20(4):632-642.
APA	Jia, Mengna,Di, Kaichang,Yue, Zongyu,&Sun, Shujuan.(2016).Spatio-temporal variation characteristics of the Mars surface brightness temperature.Yaogan Xuebao/Journal of Remote Sensing,20(4),632-642.
MLA	Jia, Mengna,et al."Spatio-temporal variation characteristics of the Mars surface brightness temperature".Yaogan Xuebao/Journal of Remote Sensing 20.4(2016):632-642.