Evidence for topographic effects on the Martian ionosphere

Wang, J.-S.; Nielsen, E.

doi:10.1016/j.pss.2004.01.008

Cited by 23 publications

(18 citation statements)

References 18 publications

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“…13 and can be categorized into two types: first, upward propagating disturbances originating from near the planet, and second, downward propagating disturbances that originate from the solar wind. Sources in the first category consist of (1) propagating disturbances caused by atmospheric waves excited by topographical features on Mars (Hinson et al 2001;Wang and Nielsen 2004), and (2) propagating disturbances produced by the interaction of the ionosphere with crustal magnetic fields (Ness et al 2000;Krymskii et al 2003Krymskii et al , 2004Eastwood et al 2008). Sources in the second category consist of (1) solar wind plasma and magnetic field disturbances incident on the dayside ionosphere (Wang and Nielsen 2003), (2) waves generated by the mirror-mode instability in the magnetosheath (Volwerk et al, 2008), and (3) waves originating from the Kelvin-Helmholtz instability caused by the velocity shear between the rapidly flowing magnetosheath and the nearly stationary ionosphere (Penz et al 2004).…”

Section: Discussionmentioning

confidence: 99%

“…Radio occultation measurements have previously shown that large density fluctuations are present in the lower levels of the ionosphere. Some of these fluctuations are known to be related to surface topography (Wang and Nielsen 2004), and others are known to be associated with variations in the crustal magnetic field (Krymskii et al 2004;Withers and Mendillo, 2005). Although the bottom panels of Figs.…”

Section: Comparison To Remote Soundingsmentioning

confidence: 99%

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Large density fluctuations in the martian ionosphere as observed by the Mars Express radar sounder

Gurnett

Morgan

Duru

et al. 2010

Icarus

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Section: Discussionmentioning

confidence: 99%

Section: Comparison To Remote Soundingsmentioning

confidence: 99%

Large density fluctuations in the martian ionosphere as observed by the Mars Express radar sounder

Gurnett

Morgan

Duru

et al. 2010

Icarus

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“…Moreover, the planet is also a major source of variability in the ionosphere, as dust storms, thermal atmospheric tides, crustal magnetic fields, or the topography itself modulate the behaviour of the ionosphere (e.g. Shinagawa and Cravens, 1989;Witasse, 2000;Withers et al, 2003;Morel et al, 2004;Wang and Nielsen, 2004;Mendillo et al, 2006;Nĕmec et al, 2011;Zou et al, 2011;Withers et al, 2012a, b;González-Galindo et al, 2013;Withers and Pratt, 2013;Bougher et al, 2015;Matta et al, 2015;Sánchez-Cano et al, 2015b. However, the solar cycle is the factor that plays the most important long-term role in ionospheric variability, as each solar cycle phase produces changes in the neutral atmosphere, in the ionospheric temperatures and in the densities.…”

Section: Introductionmentioning

confidence: 99%

Variaciones de la ionosfera de Marte debidas al ciclo solar

et al. 2016

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Solar cycle variations in solar radiation create notable changes in the Martian ionosphere, which have been analysed with Mars Express plasma datasets in this paper. In general, lower densities and temperatures of the ionosphere are found during the low solar activity phase, while higher densities and temperatures are found during the high solar activity phase. In this paper, we assess the degree of influence of the long term solar flux variations in the ionosphere of Mars. Key words: solar cycle; ionosphere of Mars; TEC. Variaciones de la ionosfera de Marte debidas al ciclo solarResumen La radiación solar en cada fase del ciclo solar crea importantes variaciones en la ionosfera de Marte, las cuales son analizadas en este artículo con datos de la sonda Mars Express. En general, las densidades y temperaturas más bajas de la ionosfera se encuentran durante la fase de baja actividad solar, mientras que las densidades y temperaturas más elevadas se encuentran durante la fase de alta actividad solar. Este artículo evalúa el efecto que las variaciones del flujo solar tienen a largo plazo en la ionosfera. Palabras clave: ciclo solar; ionosfera de Marte; TEC.

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“…The primary peak of the Martian ionosphere is under photochemical equilibrium, and its behavior can be described by Chapman theory. There are many factors that control the behavior of the Martian ionosphere, including solar F10.7 cm radiation flux [4][5][6], solar zenith angle (SZA) [7], solar wind [8], neutral atmosphere [3], differences between southern and northern hemispheres [9], dust storm [10], topography [11], etc. Effects of the Martian crustal magnetic field on ionosphere are also one of the hot topics in the Martian ionosphere research [12][13][14].…”

Section: Introductionmentioning

confidence: 99%

Effects of Martian crustal magnetic field on its ionosphere

Zou

Chen

et al. 2010

Sci. China Technol. Sci.

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The effect of the Martian crustal magnetic field is one of the hot topics of the study of Martian ionosphere. The studies on this topic are summarized in this paper. Main data of the Martian ionosphere were resulted from radio occultation experiments. According to the observations, the electron density scale height and the peak electron density of the Martian ionosphere are influenced by its crustal magnetic field. The strong horizontal magnetic field prevents the vertical diffusion of the plasma and makes the electron density scale height in the topside ionosphere close to that in the photo equilibrium region. In the cusp-like regions with strong vertical magnetic field, the enhanced vertical diffusion leads to a larger electron density scale height in the diffusion equilibrium region. The observation of radio occultation experiment onboard Mars Global Surveyor (MGS) showed that the averaged peak electron density observed in the southern hemisphere with strong crustal magnetic field was slightly larger than that in the northern hemisphere with weak crustal magnetic field. The Mars advanced radar for subsurface and ionosphere sounding (MARSIS) onboard Mars Express (MEX) was the first topside sounder to be used to observe Martian ionosphere. The MARSIS results confirmed that the enhancement of the peak electron density occurred in cusp-like regions with open field lines, and the amount of the enhancement was much larger than that observed by the radio occultation experiment. There are two possible mechanisms for the peak electron density enhancement in the cusp-like crustal magnetic field regions: One is the precipitation of the energetic particles and the other is the heating by the waves excited by plasma instabilities. It's difficult to determine which one is the key mechanism for the peak electron density enhancement. Based on these studies, several interesting problems on the Martian ionosphere and plasma environment are presented. Mars exploration, Martian crustal megnetic field, Martian ionosphere, energetic particles detection, plasma wave detection Citation:Zou H, Chen H F, Yu N, et al. Effects of Martian crustal magnetic field on its ionosphere.

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Evidence for topographic effects on the Martian ionosphere

Cited by 23 publications

References 18 publications

Large density fluctuations in the martian ionosphere as observed by the Mars Express radar sounder

Large density fluctuations in the martian ionosphere as observed by the Mars Express radar sounder

Variaciones de la ionosfera de Marte debidas al ciclo solar

Effects of Martian crustal magnetic field on its ionosphere

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