Nighttime ionosphere caused by meteoroid ablation and solar wind electron‐proton‐hydrogen impact on Mars: MEX observation and modeling

Haider, S. A.; Pandya, B. M.; Molina‐Cuberos, G. J.

doi:10.1002/jgra.50590

Cited by 19 publications

(42 citation statements)

References 64 publications

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“…It has been suggested that there are two main sources of plasma in the upper nightside ionosphere. The first being impact ionization from precipitating particles, which are thought mostly to be electrons of solar wind origin [ Verigin et al , ; Fox et al , ; Haider , ] but may also include solar wind protons, energetic neutral atoms (ENAs), and dayside photoelectrons [ Kallio and Janhunen , ; Haider et al , ; DiéVal et al , ; Xu et al , ]. The second source of plasma is thought to be day‐to‐night ion transport driven by cross‐terminator winds [ Chaufray et al , ; Cui et al , ].…”

Section: Introductionmentioning

confidence: 99%

Nightside ionosphere of Mars: Composition, vertical structure, and variability

et al. 2017

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We provide an overview of the composition, vertical structure, and variability of the nightside ionosphere of Mars as observed by Mars Atmosphere and Volatile EvolutioN (MAVEN)'s Neutral Gas and Ion Mass Spectrometer (NGIMS) through 19 months of the MAVEN mission. We show that O 2+ is the most abundant ion down to ∼130 km at all nightside solar zenith angles (SZA). However, below 130 km NO+ is the most abundant ion, and NO+ densities increase with decreasing altitude down to at least 120 km. We also show how the densities of the major ions decrease with SZA across the terminator. At lower altitudes the O 2+ and CO 2+ densities decrease more rapidly with SZA than the NO+ and HCO+ densities, which changes the composition of the ionosphere from being primarily O 2+ on the dayside to being a mixture of O 2+, NO+, and HCO+ on the nightside. These variations are in accord with the expected ion‐neutral chemistry, because both NO+ and HCO+ have long chemical lifetimes. Additionally, we present median ion density profiles from three different nightside SZA ranges, including deep on the nightside at SZAs greater than 150° and discuss how they compare to particle precipitation models. Finally, we show that nightside ion densities can vary by nearly an order of magnitude over monthlong timescales. The largest nightside densities were observed at high northern latitudes during winter and coincided with a major solar energetic particle event.

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Section: Introductionmentioning

confidence: 99%

Nightside ionosphere of Mars: Composition, vertical structure, and variability

et al. 2017

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“…10 of 120 electron density profiles) of MEX measurements during the daytime ionosphere. Recently Haider et al [15] have identified meteoric layers in two electron density profiles of MEX observations carried out in the nighttime ionosphere also, one on 22 August and the other on 25 September, 2005.…”

Section: Earlier Measurements Of Meteoric Layers On Marsmentioning

confidence: 99%

“…[15]). We have used this model to calculate the production rates and electron densities at SZA 110°due to impact of micrometeoroids and meteoroids of different masses and velocities.…”

Section: Modeling and Input Parametersmentioning

confidence: 99%

“…The solar wind electron-protonhydrogen impact ionizations are not included in this model calculation because they are important above 120 km (cf. [15]). …”

Section: Modeling and Input Parametersmentioning

confidence: 99%

“…The radio occultation experiment onboard MGS and MEX have observed meteoric plasma layers in most of the electron density profiles during daytime and nighttime ionosphere of Mars [cf. [2,11,15]]. MGS has now stopped working since 2 November, 2006, but MEX is orbiting around Mars.…”

Section: Constraints On the Meteor Measurements From Maven And Mangalmentioning

confidence: 99%

See 2 more Smart Citations

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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