Meteor impact perturbation in the lower ionosphere of Mars: MGS observations

Pandya, B. M.; Haider, S. A.

doi:10.1016/j.pss.2011.09.013

Cited by 14 publications

(15 citation statements)

References 38 publications

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“…Some years later, these layers were confirmed by Mars Express observations of a layer between 65 and 110 km which appeared sporadically in about 10% of measured electron density profiles (Pätzold et al 2005). A more extensive set of electron density profiles obtained using Mars Global Surveyor exhibited secondary layers between 70 and 105 km, in ∼4% of cases (Withers et al 2008;Pandya and Haider 2012). Their sporadic occurrence, width of a few km, and appearance over the height range where ablation occurs ( Fig.…”

Section: Meteoric Metal Layers On Venus and Marsmentioning

confidence: 64%

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

et al. 2017

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Recent advances in interplanetary dust modelling provide much improved estimates of the fluxes of cosmic dust particles into planetary (and lunar) atmospheres throughout the solar system. Combining the dust particle size and velocity distributions with new chemical ablation models enables the injection rates of individual elements to be predicted as a function of location and time. This information is essential for understanding a variety of atmospheric impacts, including: the formation of layers of metal atoms and ions; meteoric smoke particles and ice cloud nucleation; perturbations to atmospheric gas-phase chemistry; and the effects of the surface deposition of micrometeorites and cosmic spherules. There is discussion of impacts on all the planets, as well as on Pluto, Triton and Titan.

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Section: Meteoric Metal Layers On Venus and Marsmentioning

confidence: 64%

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

et al. 2017

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“…Pandya and Haider, 2012;Gurnett et al, 2015). As such, 100 km is used as the starting altitude for methane generation for the IDPs.…”

Section: Production and Destruction Of Methane During Atmospheric Pasmentioning

confidence: 99%

UV production of methane from surface and sedimenting IDPs on Mars in light of REMS data and with insights for TGO

Moores

Smith

Schuerger

2017

Planetary and Space Science

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This paper refines model predictions for the production of methane from UV-irradiated interplanetary dust particles (IDPs) now that the Rover Environmental Monitoring Station (REMS) instrument onboard the Mars Science Laboratory (MSL) Rover has made the first measurements of the UV environment on the surface of Mars, at Gale Crater.Once these measurements are included in a UV radiative transfer model, we find that . An examination of IDP-derived methane production during atmospheric settling indicates that no more than 0.32% of organic carbon from meteor streams may be deposited in the atmosphere. Thus, such a process cannot explain either the spikes observed in methane nor the low equilibrium values observed by MSL. Instead, this discrepancy may be explained if < 80 tons per year of organic carbon survives to the surface, the atmospheric lifetime of methane is < 110 years or the efficiency of the UV-CH 4 process is < 7%. Under the assumption of reduced carbon input cycling in the Martian system from these processes, both soil concentrations of organic carbon and atmospheric measurements of methane observed by MSL are consistent with the UV-CH 4 process. This refinement of methane production from IDPs and its geographical and vertical distribution will be an important input for models attempting to understand the results to be derived 2 Moores et al., 2017, P&SS_2017_232 R1 Martian Methane in the light of REMSfrom the Trace Gas Orbiter (TGO) mission that will map methane concentrations in the martian atmosphere in 2018 at 0.01 ppbv.

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“…Their analysis suggests that the characteristics of these meteoric layers vary with season, SZA and latitude. Later Pandya and Haider [12] analyzed 1500 MGS electron density profiles to study the physical characteristics of meteoric plasma layers over Mars during the period January-June 2005. They found that 65 electron density profiles out of these 1500 profiles were strongly perturbed with peak densities~(0.…”

Section: Earlier Measurements Of Meteoric Layers On Marsmentioning

confidence: 99%

Probing of meteor showers at Mars during the encounter of comet C/2013 A1: predictions for the arrival of MAVEN/Mangalyaan

Haider

Pandya

2015

Geosci. Lett.

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We have estimated (1) production rates, (2) ion and electron densities of meteor ablation and (3) ionization for different masses and velocities of meteoroids when comet C/2013 A1 crossed the orbit of Mars on 19 October, 2014 at 18:27 UT. Meteor ablations of small masses < 10 −4 g have created a broad layer between altitude~90 km and 110 km. The meteoroids of large masses ≥ 10 −4 g are burnt at around 60-90 km well below the main ionization peak at altitude~160 km produced in the nighttime by solar wind particle impact. The production rates and densities of 15 metallic ions (Mg

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Meteor impact perturbation in the lower ionosphere of Mars: MGS observations

Cited by 14 publications

References 38 publications

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

Impacts of Cosmic Dust on Planetary Atmospheres and Surfaces

UV production of methane from surface and sedimenting IDPs on Mars in light of REMS data and with insights for TGO

Probing of meteor showers at Mars during the encounter of comet C/2013 A1: predictions for the arrival of MAVEN/Mangalyaan

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