HF radio wave attenuation due to a meteoric layer in the atmosphere of Mars

Witasse, Olivier; Nouvel, Jean-Francois; Lebreton, Jean‐Pierre; Kofman, W.

doi:10.1029/2001gl013164

Cited by 24 publications

(33 citation statements)

References 12 publications

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“…However, Figure 13 of Hake and Phelps [1967] shows that the temperature dependence of ϕ is relatively small, so we assume a constant value for this exploratory survey. Note that a wide range of values of ϕ have been used in previous work [ Melnik and Parrot , 1999; Witasse et al , 2001; Safaeinili et al , 2003]. Some previous workers adopted the terrestrial (N 2 /O 2 ) value for ϕ, which is 2 orders of magnitude smaller than the value in the CO 2 atmosphere of Mars [ Nielsen et al , 2007].…”

Section: Application To Marsmentioning

confidence: 99%

“…They found that these low frequencies, which might be naturally produced in the lower atmosphere by electrical discharges associated with airborne dust, could only propagate upward to orbital detectors under nightside ionospheric conditions at low solar activity and in the presence of a strong magnetic field. Witasse et al [2001] investigated the effects of meteoric layers on MHz radio signals to support radar experiments on Mars Express and Nozomi. They found that the attenuation could exceed tens of dB.…”

Section: Introductionmentioning

confidence: 99%

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Attenuation of radio signals by the ionosphere of Mars: Theoretical development and application to MARSIS observations

Withers

2011

Radio Science

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[1] We investigate the ionospheric conditions required to explain Mars Express Mars Advanced Radar for Subsurface and Ionosphere Sounding topside radar sounder observations of ionospheric attenuation in excess of 13 dB at 5 MHz during solar energetic particle events. We develop theoretical expressions for the attenuation caused by a layer of ionospheric plasma in cases of high, intermediate, and low radio frequency relative to the electron-neutral collision frequency at the ionospheric layer. We apply these relationships to four layers: the M2 layer produced at 120 km by solar extreme ultraviolet photons, the M1 layer produced at 100 km by solar X-ray photons and associated electron impact ionization, the meteoric layer produced at 85 km by meteoroid ablation, and a putative plasma layer produced at 35 km by cosmic rays. Attenuation is weaker in the M2 layer than in the M1 layer. Attenuation in the M1 and meteoric layers are comparable, although their properties are quite variable. The greatest attenuation for radio frequencies above 50 MHz occurs in the predicted plasma layer at 35 km, but its effects are relatively small at lower frequencies. If optimally located with a peak altitude of 50 km, a layer with a peak plasma density of 10 9 m −3 is sufficient to explain the observed 13 dB attenuation. Although the electron densities produced by solar energetic particle events at Mars have not been directly simulated, the required electron densities are plausible. However, the altitude at which solar energetic particles produce plasma is uncertain.Citation: Withers, P. (2011), Attenuation of radio signals by the ionosphere of Mars: Theoretical development and application to MARSIS observations, Radio Sci., 46, RS2004,

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Section: Application To Marsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Attenuation of radio signals by the ionosphere of Mars: Theoretical development and application to MARSIS observations

Withers

2011

Radio Science

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“…These include the activity of comets, the dynamics of dust in space, delivery of cometary organic materials to planets, collision hazards for spacecraft, and ionospheric production, loss and transport processes. Meteoric layers may also affect remote sensing, navigation and communication techniques that use radio wavelengths [ Witasse et al , 2001; Nielsen et al , 2007].…”

Section: Introductionmentioning

confidence: 99%

Physical characteristics and occurrence rates of meteoric plasma layers detected in the Martian ionosphere by the Mars Global Surveyor Radio Science Experiment

et al. 2008

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[1] Low-altitude plasma layers are present in 71 of 5600 electron density profiles from the Martian ionosphere obtained by the Mars Global Surveyor Radio Science experiment. These layers are produced by the ablation of meteoroids and subsequent ionization of meteoric atoms. The mean altitude of the meteoric layer is 91.7 ± 4.8 km. The mean peak electron density in the meteoric layer is (1.33 ± 0.25) Â 10 10 m À3. The mean width of the meteoric layer is 10.3 ± 5.2 km. The occurrence rate of meteoric layers varies with season, solar zenith angle, and latitude. Seasonal variations in occurrence rate are particularly strong, often exceeding an order of magnitude. Meteoric layer altitude, peak electron density, and width are all positively correlated, with correlation coefficients of 0.3-0.4. Other correlation coefficients between the physical characteristics of meteoric layers and atmospheric or observational properties, such as scale height, solar zenith angle, and solar flux, have absolute values that are significantly smaller, indicating lack of correlation. The photochemical lifetime of plasma in meteoric layers is $12 days and depends on altitude.

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“…The model is not unique or complete: Other factors like surface scattering (not included) [ Picardi et al , 2004] will add further losses while lower‐than‐modeled dust concentrations may improve the detectability. A possible highly‐attenuating meteoric layer near 80 km altitude is not considered herein [ Pesnell and Grebowsky , 2000; Witasse et al , 2001]. Also, any unfrozen water mixed with the ice will increase conductivity/attenuation beyond model values.…”

Section: Discussionmentioning

confidence: 99%

Detecting sub‐glacial aquifers in the north polar layered deposits with Mars Express/MARSIS

Farrell

Plaut

Gurnett

et al. 2005

Geophysical Research Letters

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[1] The penetration of the MARSIS radar signal into the polar ice mass is modeled to determine the capability of the instrument to locate sub-glacial aquifers. As a ground penetrating radar, the orbiting MARSIS transmits a signal >1 W between 1 -5 MHz. In this work we will investigate the effect of ice reflective and conductive losses on the radar-detection of subsurface aquifers using an MGS MOC profile of the ice layering. We find that a basal lake located $2.5 km below the surface is at the limit of detectability.

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HF radio wave attenuation due to a meteoric layer in the atmosphere of Mars

Cited by 24 publications

References 12 publications

Attenuation of radio signals by the ionosphere of Mars: Theoretical development and application to MARSIS observations

Attenuation of radio signals by the ionosphere of Mars: Theoretical development and application to MARSIS observations

Physical characteristics and occurrence rates of meteoric plasma layers detected in the Martian ionosphere by the Mars Global Surveyor Radio Science Experiment

Detecting sub‐glacial aquifers in the north polar layered deposits with Mars Express/MARSIS

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