KMS of Xinjiang Astronomical Observatory, CAS
| Martian electron density profiles retrieved from Mars Express dual-frequency radio occultation measurements | |
| Zhang, S. J.1,2,3,4; Cui, J.2; Guo, P.1; Li, J. L.1; Ping, J. S.2; Jian, N. C.1; Zhang, K. F.5; Zhang, SJ | |
| 2015-05-01 | |
| Source Publication | Advances in Space Research
 |
| ISSN | 0273-1177 |
| Volume | 55Issue:9Pages:2177-2189 |
| Abstract | The S- and X-band dual-frequency Doppler radio occultation observations obtained by the Mars Express Radio Science (MaRS) experiments are reduced in this study. A total of 414 Martian electron density profiles are retrieved covering the period from DOY 93 2004 to DOY 304 2012. These observations are well distributed over both longitude and latitude, with Sun-Mars distance varying from 1.38 AU to 1.67 AU, the solar zenith angle (SZA) ranging from 52 degrees to 122 degrees. Due to the improved vertical resolution for the MaRS experiments, the vertical structures of the retrieved profiles appear to be more complicated than those revealed by early radio occultation experiments. Dayside electron density profiles have primary peaks (M2) typically around 130 km and secondary peaks (M1) around 110 km. Nightside electron density profiles are highly variable, many of which do not have double layer structures. Both the dayside and nightside electron density profiles reveal some atypical features such as topside layering above M2 and bottom-side layering below M1. The former likely represent the plasma fluctuations in response to the solar wind (SW) interactions with the Martian ionosphere, whereas the latter is thought to be induced by the meteoric influx. We fit the peak electron density of profiles up to terminator with a simple power relation (N-m = N-0/ch(k)(x)) with the best-fit subsolar peak electron density being N-0 = (1.499 +/- 0.002) x 10(5) cm(-3), and the best-fit power index being k = 0.513 +/- 0.001. The measured total electron content (TEC) is obtained by integrating the observed electron density profile vertically from 50 km to 400 km, which is then compared with the ideal TEC computed from the one-layer Chapman model. We find that the one-layer Chapman model can generally underestimate the measured TEC up to similar to 0.1 TECU (1 TECU = 1.0 x 10(16) m(-2)) for 55 degrees < SZA < 90 degrees and up to similar to 0.05 TECU for 90 degrees < SZA < 120 degrees. The dayside TEC (SZA <= 75 degrees) varies from 0.1 to 0.6 TECU, whereas the nightside TEC (SZA >= 105 degrees) is usually below 0.2 TECU. Several large TEC values can be found in the terminator region. The corresponding slab thickness varies from 40 km-60 km for the dayside and 40 km-140 km for the nightside, with an average value of 61 km. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved. |
| Correspondent Email | sjzhang@shao.ac.cn |
| Keyword | Martian Ionosphere Radio Occultation Inversion Differential Doppler |
| Subtype | Article |
| DOI | 10.1016/j.asr.2015.01.030 |
| Indexed By | SCI |
| Language | 英语 |
| WOS Keyword | global surveyor ; radar soundings ; ionosphere ; atmosphere ; topography ; spacecraft ; tracking ; venus |
| WOS Research Area | Astronomy & Astrophysics ; Geology ; Meteorology & Atmospheric Sciences |
| WOS Subject | Astronomy & Astrophysics ; Geosciences, Multidisciplinary ; Meteorology & Atmospheric Sciences |
| WOS ID | WOS:000353078400003 |
| Project Number | 11103063 ; 11178008 ; PSL15\_04 ; XDB09040400 |
| Funding Organization | National Natural Science Foundation of China ; Key Laboratory of Planetary Sciences, Chinese Academy of Sciences ; Chinese Academy of Sciences |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/1612 |
| Collection | 110米口径全可动射电望远镜（QTT）_110米大口径全可动射电望远镜关键技术研究（973项目）_课题1：大样本射电天体的观测和前沿问题研究 |
| Corresponding Author | Zhang, SJ |
| Affiliation | 1.Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China 2.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 3.Key Laboratory of Planetary Sciences, Chinese Academy of Sciences, Shanghai 200030, China 4.University of Chinese Academy of Sciences, Beijing 100049, China 5.Royal Melbourne Institute of Technology, Melbourne, Victoria 3001, Australia |
| Recommended Citation GB/T 7714 | Zhang, S. J.,Cui, J.,Guo, P.,et al. Martian electron density profiles retrieved from Mars Express dual-frequency radio occultation measurements[J]. Advances in Space Research,2015,55(9):2177-2189. |
| APA | Zhang, S. J..,Cui, J..,Guo, P..,Li, J. L..,Ping, J. S..,...&Zhang, SJ.(2015).Martian electron density profiles retrieved from Mars Express dual-frequency radio occultation measurements.Advances in Space Research,55(9),2177-2189. |
| MLA | Zhang, S. J.,et al."Martian electron density profiles retrieved from Mars Express dual-frequency radio occultation measurements".Advances in Space Research 55.9(2015):2177-2189. |
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| File Name/Size | DocType | Version | Access | License | ||
| 1-s2.0-S027311771500（2870KB） | 期刊论文 | 作者接受稿 | 开放获取 | CC BY-NC-SA | View Application Full Text | |
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