Mars Initial Reference Ionosphere (MIRI) Model: Updates and Validations Using MAVEN, MEX, and MRO Data Sets

Mendillo, M.; Narvaez, C.; Trovato, Jeffrey; Withers, Paul; Mayyasi, Majd; Morgan, D. D.; Kopf, A. J.; Gurnett, D. A.; Němec, F.; Campbell, B. A.

doi:10.1029/2018ja025263

Cited by 16 publications

(4 citation statements)

References 38 publications

(77 reference statements)

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“…In this regard, it may often prove useful and sufficient to analyze total electron content of the ionosphere in place of electron density profiles (Dubinin et al, ; Mendillo et al, ), which may be at times easier to evaluate (Safaeinili et al, ). Empirical models of total electron content as a function of relevant controlling parameters were subsequently developed (Mendillo et al, ) and validated (Mendillo et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…This was used by Mendillo et al (), along with nearly 113,000 peak electron density values obtained by the MARSIS instrument between 2005 and 2012, to develop a model of peak electron densities characterized by the solar zenith angle (SZA), orbital distance, and F 10.7 index as a proxy for the solar ionizing flux. The analysis was later extended by Mendillo et al () to incorporate as many as 215,818 peak electron density values from the years 2005–2015. Sánchez‐Cano et al () used the same parametrization and a combined data set of 1,200 MARSIS radar sounding profiles and 500 Mars Global Surveyor occultation profiles to construct a model of electron densities describing not only the main M2 ionospheric layer but also the lower M1 layer (Fallows et al, , ; Fox & Weber, ; Fox & Yeager, ).…”

Section: Introductionmentioning

confidence: 99%

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Characterizing Average Electron Densities in the Martian Dayside Upper Ionosphere

et al. 2019

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We use more than 10 years of the Martian topside ionospheric data measured by the Mars Advanced Radar for Subsurface and Ionosphere Sounding radar sounder on board the Mars Express spacecraft to derive an empirical model of electron densities from the peak altitude up to 325 km. Altogether, 16,044 electron density profiles obtained at spacecraft altitudes lower than 425 km and at solar zenith angles lower than 80° are included in the analysis. Each of the measured electron density profiles is accurately characterized by the peak electron density, peak altitude, and three additional parameters describing the profile shape above the peak: (i) steepness at high altitudes, (ii) main layer thickness, and (iii) transition altitude. The dependence of these parameters on relevant controlling factors (solar zenith angle, solar irradiance, crustal magnetic field magnitude, and Sun‐Mars distance) is evaluated, allowing for a formulation of a simple empirical model. Mars Atmosphere and Volatile EvolutioN Extreme Ultraviolet monitor data are used to show that the solar ionizing flux can be accurately approximated by the F10.7 index when taking into account the solar rotation. Electron densities predicted by the resulting empirical model are compared with electron densities locally evaluated based on the Mars Advanced Radar for Subsurface and Ionosphere Sounding measurements, with the Langmuir Probe and Waves electron density measurements on board the Mars Atmosphere and Volatile EvolutioN spacecraft, and with electron densities obtained by radio occultation measurements. Although the electron densities measured by the Langmuir Probe and Waves instrument are systematically somewhat lower than the model electron densities, consistent with former findings, the model performs reasonably well.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Characterizing Average Electron Densities in the Martian Dayside Upper Ionosphere

et al. 2019

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“…Peter et al (2014) published a 1-dimensional model of the ionosphere, used to interpret the Mars Express radio-occultation data. Recently, the Mars International Reference Ionosphere (MIRI-2018, Mendillo et al, 2018) provides a new module for Total Electron Content (TEC) using more than 120,000 values from the Mars Reconnaissance Orbiter/SHAllow RADar (MRO/SHARAD). The TEC output available on the web (http://sirius.bu.edu/miri/miri.php) is driven by Solar Zenith Angle (SZA) and solar index only.…”

Section: Introductionmentioning

confidence: 99%

MoMo: a new empirical model of the Mars ionospheric total electron content based on Mars Express MARSIS data

Bergeot

Witasse

Maistre

et al. 2019

J. Space Weather Space Clim.

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Aims: Several scientific landers and rovers have reached the Martian surface since the 1970s. Communication between the asset (i.e., lander or rover) and Mars orbiters or Earth antennas uses radio signals in UHF to X-band frequencies passing through the Mars’ ionosphere. It is consequently necessary to take into account electron density variation in the Mars’ ionosphere to correct the refraction of the signal transmitted. Methods: We developed a new empirical model of the Mars’ ionosphere called MoMo. It is based on the large database of Total Electron Content (TEC) derived from the subsurface mode of the Mars Express MARSIS radar. The model provides vertical TEC as a function of solar zenith angle, solar activity, solar longitude and location. For validation, the model is compared with Mars Express radio occultation data as well as with the numerical model IPIM (IRAP Plasmasphere-Ionosphere Model). Results: We discussed the output of the model in terms of climatology behaviour of the Mars’ ionosphere. The output of MoMo is then uses to quantify the impact of the Martian ionosphere for radio-science experiments. From our results, the effect is of the order of 10−3 mm s−1 in Doppler observables especially around sunrise and sunset. Consequently, this new model could be used to support the data analysis of any radio-science experiment and especially for present InSight RISE and futur ExoMars LARA instruments aiming at better understand the deep-interior of Mars.

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“…The Radio Occultation Science Experiment (ROSE) on the MAVEN spacecraft has conducted a series of two-way, single-frequency radio occultation observations of Mars (Withers et al, 2018(Withers et al, , 2020. Vertical profiles of electron density in the ionosphere of Mars have been derived from time series of the frequency of the radio signal received on Earth during these observations (Crismani et al, 2019;Mendillo et al, 2018;Withers et al, 2018;Yao, 2019). Here we report the theoretical development of the processing methods used to generate these ionospheric electron density profiles.…”

Section: Introductionmentioning

confidence: 99%

How to Process Radio Occultation Data: 2. From Time Series of Two‐Way, Single‐Frequency Frequency Residuals to Vertical Profiles of Ionospheric Properties

Withers

Moore

2020

Radio Science

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The MAVEN Radio Occultation Science Experiment (ROSE) generates vertical profiles of electron density in the ionosphere of Mars from two‐way, single‐frequency radio occultation observations. Here we develop methods for generating vertical profiles of ionospheric electron density from frequency residuals obtained from such observations. We show that the relevant set of equations can be closed for ionospheric observations if the uplink bending angle is equal to the product of the downlink bending angle and the square of the turn‐around ratio. This is consistent with the dispersion relation for radio waves in plasma. Four angles, each being the angle between the asymptote of a portion of a refracted ray path and the corresponding idealized unrefracted ray path, provide a natural framework for development of these methods. We also present forms of these methods appropriate to one‐way radio occultation experiments. These methods have been validated using a simulated occultation representative for the ionosphere of Mars. Errors are found to be on the order of a few percent.

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Mars Initial Reference Ionosphere (MIRI) Model: Updates and Validations Using MAVEN, MEX, and MRO Data Sets

Cited by 16 publications

References 38 publications

Characterizing Average Electron Densities in the Martian Dayside Upper Ionosphere

Characterizing Average Electron Densities in the Martian Dayside Upper Ionosphere

MoMo: a new empirical model of the Mars ionospheric total electron content based on Mars Express MARSIS data

How to Process Radio Occultation Data: 2. From Time Series of Two‐Way, Single‐Frequency Frequency Residuals to Vertical Profiles of Ionospheric Properties

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