A coupled model of the D and E regions of Mars' ionosphere for flare and non-flare electron density profiles

Shah, Siddhi Y.; Haider, S. A.; Molina‐Cuberos, G. J.; Abdu, M. A.; Batista, I. S.

doi:10.1016/j.icarus.2021.114403

Cited by 9 publications

(5 citation statements)

References 28 publications

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“…X‐rays are more energetic radiation, which actually produce photoelectrons and are attenuated greatly in the D region ionosphere. Therefore, the photoelectron impact ionization rates are higher than the photoionization rates by ∼1 order of magnitude (Shah et al., 2021). The production rates of H 2 O + , HDO + , and D 2 O + depend on the modeling parameters: the mixing ratios of H 2 O, HDO, and D 2 O, air density, photo ionization/photo electron impact cross sections, photon flux, GCR flux, and yield spectrum method (Haider et al., 2016, 2022; Shah et al., 2021; Vandaele et al., 2019).…”

Section: Resultsmentioning

confidence: 99%

“…X-rays are more energetic radiation, which actually produce photoelectrons and are attenuated greatly in the D region ionosphere. Therefore, the photoelectron impact ionization rates are higher than the photoionization rates by ∼1 order of magnitude (Shah et al, 2021). The production rates of H 2 O + , HDO + , and D 2 O + depend on the modeling parameters: the mixing ratios of H 2 O, Altitude profiles of production rates of (a) H 2 O + , (b) HDO + , and (c) D 2 O + due to impact of GCR and hard X-ray in model 1 (presence of dust storm) and model 2 (absence of dust storm) The red triangle represents the photoionization rates resulting from model 1 due to the impact of hard X-rays and GCR, while the black circle shows the photoionization rate resulting from model 2 due to the impact of hard X-rays and GCR.…”

Section: Response Of H 2 O + Hdo + and D 2 O + Photoionization Rate...mentioning

confidence: 99%

“…The red star represents the production rate caused by photoelectrons resulting from model 1 due to the impact of hard X-rays, while the black star shows the production rate caused by photoelectrons resulting from model 2 due to the impact of hard X-rays. HDO, and D 2 O, air density, photo ionization/photo electron impact cross sections, photon flux, GCR flux, and yield spectrum method (Haider et al, 2016(Haider et al, , 2022Shah et al, 2021;Vandaele et al, 2019).…”

Section: Response Of H 2 O + Hdo + and D 2 O + Photoionization Rate...mentioning

confidence: 99%

“…Therefore, the sum of the positive ion densities is equal to the electron density and the sum of the negative ion densities (Σn i + = Σn i − + n e ). The chemical equilibrium conditions are valid in the lower ionosphere of Mars because their chemical life time is much lower than the transport time (Haider et al, 2007(Haider et al, , 2009Shah et al, 2021;Sheel & Haider, 2012). We have used GCR and hard X-ray radiation for the ionization of the neutral gases in the lower atmosphere.…”

Section: Theorymentioning

confidence: 99%

“…The function was fitted analytically later (cf. Haider et al, 2009Haider et al, , 2010Haider et al, , 2016Haider et al, , 2022Shah et al, 2021). These ion production rates have been used in the calculation of the densities of cluster ions.…”

Section: Modeling In the D Region Of Mars' Ionospherementioning

confidence: 99%

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Impact of Mars GDS 2018 on the Chemistry of Water, Nitrogenated and Deuterated Cluster Ions: NOMAD Observations

Shah,

Haider,

Korablev

2023

JGR Planets

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The ExoMars Trace Gas Orbiter instruments, Nadir and Occultation for Mars Discovery and Atmospheric Chemistry Suite have provided vertical profiles of H2O and HDO mixing ratios in the presence and absence of Global Dust Storm 2018. These observations are carried out in the lower atmosphere at SZA ∼ 71° of northern mid latitude (∼55°N, 130°E). Using NOMAD observations, we developed chemical models 1 and 2 for dust and non‐dust storm conditions, respectively. The production/loss rates of H2O, HDO and D2O and the densities of water, nitrogenated and deuterated cluster ions (H2O+, D2O+, HDO+, H+(H2O)n, D+(D2O)n, H+(HDO)n, CO4−, CO3−, CO3−(H2O)n, CO3−(D2O)n, CO3−(HDO)n, NO2−(H2O), NO2−(HDO), and NO2−(D2O) (for n = 1 to 5)) are estimated from these models between 10 and 70 km. We have used two ionization sources: (a) Galactic Cosmic Rays (GCR) and (b) hard X‐ray in both models. The D peak density produced by GCR is lower by a factor of ∼5 than that produced by the hard X‐rays. In model 1, the electron densities were increased by a factor of ∼2–3 than that produced by model 2. The estimated production/loss rates of H2O, HDO, and D2O are also larger by an order of magnitude in model 1 than that estimated by model 2.

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