An investigation of ionospheric upper transition height variations at low and equatorial latitudes deduced from combined COSMIC and C/NOFS measurements

doi:10.1016/j.asr.2016.11.024

CORC > 地质与地球物理研究所 > 中国科学院地质与地球物理研究所 > 中国科学院地球与行星物理重点实验室

	An investigation of ionospheric upper transition height variations at low and equatorial latitudes deduced from combined COSMIC and C/NOFS measurements
	Yang, Changjun 1,2,3; Zhao, Biqiang 1,2,3; Zhu, Jie 1,2,3; Yue, Xinan 1,2; Wan, Weixing 1,2
刊名	ADVANCES IN SPACE RESEARCH
	2017-10-15
卷号	60 期号:8 页码:1617-1628
关键词	Topside ionosphere Upper transition height Scale height C/NOFS COSMIC
ISSN号	0273-1177
DOI	10.1016/j.asr.2016.11.024
文献子类	Article
英文摘要	In this study we propose the combination of topside in-situ ion density data from the Communication/Navigation Outage Forecast System (C/NOFS) along with the electron density profile measurement from Constellation Observing System for Meteorology, Ionosphere & Climate (COSMIC) satellites Radio Occultation (RO) for studying the spatial and temporal variations of the ionospheric upper transition height (h(T)) and the oxygen ion (O+) density scale height. The latitudinal, local time and seasonal distributions of upper transition height show more consistency between hT re-calculated by the profile of the O+ using an alpha-Chapman function with linearly variable scale height and that determined from direct in-situ ion composition measurements, than with constant scale height and only the COSMIC data. The discrepancy in the values of hT between the C/NOFS measurement and that derived by the combination of COSMIC and C/NOFS satellites observations with variable scale height turns larger as the solar activity decreases, which suggests that the photochemistry and the electrodynamics of the equatorial ionosphere during the extreme solar minimum period produce abnormal structures in the vertical plasma distribution. The diurnal variation of scale heights (H-m) exhibits a minimum after sunrise and a maximum around noon near the geomagnetic equator. Further, the values of H-m exhibit a maximum in the summer hemisphere during daytime, whereas in the winter hemisphere the maximum is during night. Those features of H-m consistently indicate the prominent role of the vertical electromagnetic (E x B) drift in the equatorial ionosphere. (C) 2016 Published by Elsevier Ltd on behalf of COSPAR.
WOS关键词	RADIO OCCULTATION MEASUREMENTS ; ELECTRON-DENSITY PROFILES ; SOLAR MINIMUM ; SCALE HEIGHT ; TOPSIDE ; ARECIBO ; MODEL ; IRI
WOS研究方向	Astronomy & Astrophysics ; Geology ; Meteorology & Atmospheric Sciences
语种	英语
出版者	ELSEVIER SCI LTD
WOS记录号	WOS:000412620000005
资助机构	National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; 41321003 ; 41321003 ; 41321003 ; 41321003 ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 41131066) ; 41131066) ; 41131066) ; 41131066) ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; 41321003 ; 41321003 ; 41321003 ; 41321003 ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 41131066) ; 41131066) ; 41131066) ; 41131066) ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; 41321003 ; 41321003 ; 41321003 ; 41321003 ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 41131066) ; 41131066) ; 41131066) ; 41131066) ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National Natural Science Foundation of China(41674148 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; National High Technology Research and Development Program of China (863 Program)(2014AA123503 ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; NASA(NAS5-01068) ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; Chinese Academy of Science ; 41321003 ; 41321003 ; 41321003 ; 41321003 ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 2014IES0406) ; 41131066) ; 41131066) ; 41131066) ; 41131066)
内容类型	期刊论文
源URL	[http://ir.iggcas.ac.cn/handle/132A11/61982]
专题	地质与地球物理研究所_中国科学院地球与行星物理重点实验室
通讯作者	Zhao, Biqiang
作者单位	1.Chinese Acad Sci, Key Lab Earth & Planetary Phys, Inst Geol & Geophys, Beijing 100029, Peoples R China 2.Chinese Acad Sci, Beijing Natl Observ Space Environm, Inst Geol & Geophys, Beijing 100029, Peoples R China 3.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
推荐引用方式 GB/T 7714	Yang, Changjun,Zhao, Biqiang,Zhu, Jie,et al. An investigation of ionospheric upper transition height variations at low and equatorial latitudes deduced from combined COSMIC and C/NOFS measurements[J]. ADVANCES IN SPACE RESEARCH,2017,60(8):1617-1628.
APA	Yang, Changjun,Zhao, Biqiang,Zhu, Jie,Yue, Xinan,&Wan, Weixing.(2017).An investigation of ionospheric upper transition height variations at low and equatorial latitudes deduced from combined COSMIC and C/NOFS measurements.ADVANCES IN SPACE RESEARCH,60(8),1617-1628.
MLA	Yang, Changjun,et al."An investigation of ionospheric upper transition height variations at low and equatorial latitudes deduced from combined COSMIC and C/NOFS measurements".ADVANCES IN SPACE RESEARCH 60.8(2017):1617-1628.