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Sökning: onr:"swepub:oai:DiVA.org:uu-253088" > Total electron cont...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00003880naa a2200553 4500
001oai:DiVA.org:uu-253088
003SwePub
008150520s2015 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-2530882 URI
0247 a https://doi.org/10.1002/2014JA0206302 DOI
040 a (SwePub)uu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Sanchez-Cano, B.4 aut
2451 0a Total electron content in the Martian atmosphere :b A critical assessment of the Mars Express MARSIS data sets
264 1c 2015
338 a electronic2 rdacarrier
520 a The total electron content (TEC) is one of the most useful parameters to evaluate the behavior of the Martian ionosphere because it contains information on the total amount of free electrons, the main component of the Martian ionospheric plasma. The Mars Express Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) radar is able to derive TEC from both of its operation modes: (1) the active ionospheric sounding (AIS) mode and (2) the subsurface mode. TEC estimates from the subsurface sounding mode can be computed from the same raw data independently using different algorithms, which should yield similar results. Significant differences on the dayside, however, have been found from two of the algorithms. Moreover, both algorithms seem also to disagree with the TEC results from the AIS mode. This paper gives a critical, quantitative, and independent assessment of these discrepancies and indicates the possible uncertainty of these databases. In addition, a comparison between the results given by the empirical model of the Martian ionosphere developed by Sanchez-Cano et al. (2013) and the different data sets has been performed. The main result is that for solar zenith angles higher than 75 degrees, where the maximum plasma frequency is typically small compared with the radar frequencies, the two subsurface algorithms can be confidently used. For solar zenith angles less than 75 degrees, where the maximum plasma frequency is very close to the radar frequencies, both algorithms suffer limitations. Nevertheless, despite the solar zenith angle restrictions, the dayside TEC of one of the two algorithms is consistent with the modeled TEC.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a Mars Express
653 a total electron content
653 a Martian ionosphere
653 a MARSIS TEC assessment
653 a TEC data sets
7001 a Morgan, D. D.4 aut
7001 a Witasse, O.4 aut
7001 a Radicella, S. M.4 aut
7001 a Herraiz, M.4 aut
7001 a Orosei, R.4 aut
7001 a Cartacci, M.4 aut
7001 a Cicchetti, A.4 aut
7001 a Noschese, R.4 aut
7001 a Kofman, W.4 aut
7001 a Grima, C.4 aut
7001 a Mouginot, J.4 aut
7001 a Gurnett, D. A.4 aut
7001 a Lester, M.4 aut
7001 a Blelly, P. -L4 aut
7001 a Opgenoorth, Hermannu Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)heropgen
7001 a Quinsac, G.4 aut
7102 a Uppsala universitetb Institutet för rymdfysik, Uppsalaavdelningen4 org
7730 t Journal of Geophysical Research - Space Physicsg 120:3, s. 2166-2182q 120:3<2166-2182x 2169-9380x 2169-9402
8564 u https://doi.org/10.1002/2014JA020630y Fulltext
8564 u https://uu.diva-portal.org/smash/get/diva2:816019/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-253088
8564 8u https://doi.org/10.1002/2014JA020630

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