2018
DOI: 10.1002/2017je005510
|View full text |Cite
|
Sign up to set email alerts
|

Meteoric Metal Chemistry in the Martian Atmosphere

Abstract: Recent measurements by the Imaging Ultraviolet Spectrograph (IUVS) instrument on NASA's Mars Atmosphere and Volatile EvolutioN mission show that a persistent layer of Mg + ions occurs around 90 km in the Martian atmosphere but that neutral Mg atoms are not detectable. These observations can be satisfactorily modeled with a global meteoric ablation rate of 0.06 t sol −1 , out of a cosmic dust input of 2.7 ± 1.6 t sol −1 . The absence of detect… Show more

Help me understand this report

Search citation statements

Order By: Relevance

Paper Sections

Select...
3
1
1

Citation Types

3
66
0

Year Published

2018
2018
2024
2024

Publication Types

Select...
5
1
1

Relationship

2
5

Authors

Journals

citations
Cited by 37 publications
(69 citation statements)
references
References 59 publications
(100 reference statements)
3
66
0
Order By: Relevance
“…Persistent layer observations of Mg + (Crismani et al, ) offer the only constraints on the meteoric chemistry of atomic Mg, which can be, but has not been, observed by IUVS. Figure demonstrates that the chemical model from Plane, Carrillo‐Sanchez, et al () does predict the abundance of Mg to a reasonable accuracy. However, as these are the only observations of Fe + and Fe in the atmosphere of Mars, it is not surprising that, though the shape of Fe + and Fe are roughly consistent, the model overestimates their abundances.…”
Section: Analysis and Interpretationmentioning
confidence: 67%
See 3 more Smart Citations
“…Persistent layer observations of Mg + (Crismani et al, ) offer the only constraints on the meteoric chemistry of atomic Mg, which can be, but has not been, observed by IUVS. Figure demonstrates that the chemical model from Plane, Carrillo‐Sanchez, et al () does predict the abundance of Mg to a reasonable accuracy. However, as these are the only observations of Fe + and Fe in the atmosphere of Mars, it is not surprising that, though the shape of Fe + and Fe are roughly consistent, the model overestimates their abundances.…”
Section: Analysis and Interpretationmentioning
confidence: 67%
“…The model is then run for more than 60 hr with relevant vertical transport and chemistry (Figure ). Because the Siding Spring dust entered the atmosphere at a velocity of 56 km/s, the peak ablation altitudes are ~30 km higher than predicted for the persistent layer (Crismani et al, ; Plane, Carrillo‐Sanchez, et al, ). The correlation of dust velocity with ablation altitude is counterintuitive when compared to auroral or energetic particle processes.…”
Section: Observations Data Processing and Model Detailsmentioning
confidence: 86%
See 2 more Smart Citations
“…The first region is the lower ionosphere. It lies below ~150 km, is photochemically driven, includes a main plasma layer and often one or more lower altitude plasma layers, and is produced by absorption of extreme ultraviolet, X‐ray photons, and meteor ablation (Fallows et al, ; Molina‐Cuberos et al, ; Plane et al, ; Rishbeth & Mendillo, ). Observations of the lower ionosphere of Mars have been adequately interpreted using photochemical equilibrium theory and subsequently well reproduced by numerical simulations (e.g., Fallows et al, ; Fox & Dalgarno, ; Fox et al, ; Fox & Weber, ; Fox & Yeager, , ; Krasnopolsky, ; Lollo et al, ; Martinis et al, ).…”
Section: Introductionmentioning
confidence: 99%