Martian Ionosphere Electron Density Prediction Using Bagged Trees [PDF]
, 2022 The availability of Martian atmospheric data provided by several Martian missions broadened the opportunity to investigate and study the conditions of the Martian ionosphere. As such, ionospheric models play a crucial part in improving our understanding of ionospheric behavior in response to different spatial, temporal, and space weather conditions ...
arxiv +1 more source
Mars' atmospheric neon suggests volatile-rich primitive mantle [PDF]
, 2021 Martian atmospheric neon (Ne) has been detected by Viking and also found as trapped gas in Martian meteorites, though its abundance and isotopic composition have not been well determined. Because the timescale of Ne loss via atmospheric escape estimated from recent measurements with MAVEN is short (0.6--1 $\times$ 10$^8$ years), the abundance and ...
arxiv +1 more source
Model for Nitric oxide and its dayglow emission in the Martian upper atmosphere using NGIMS/MAVEN measured neutral and ion densities [PDF]
, 2022 A comprehensive study of Nitric oxide (NO) chemistry in the Martian upper atmosphere is restricted due to the lack of requisite measurements. NO is an abundant form of odd nitrogen species in the Martian lower atmosphere and its density depends on several photochemical processes.
arxiv +1 more source
Did high-energy astrophysical sources contribute to Martian atmospheric loss? [PDF]
MNRAS (November 21, 2016) Vol. 463 L64-L68, 2016 Mars is believed to have had a substantial atmosphere in the past. Atmospheric loss led to depressurization and cooling, and is thought to be the primary driving force responsible for the loss of liquid water from its surface. Recently, MAVEN observations have provided new insight into the physics of atmospheric loss induced by ICMEs and solar wind ...
arxiv +1 more source
Dust storm-enhanced gravity wave activity in the Martian thermosphere observed by MAVEN and implication for atmospheric escape [PDF]
, 2021 Lower atmospheric global dust storms affect the small- and large-scale weather and variability of the whole Martian atmosphere. Analysis of the CO$_2$ density data from the Neutral Gas and Ion Mass Spectrometer instrument (NGIMS) on board NASA's Mars Atmosphere Volatile EvolutioN (MAVEN) spacecraft show a remarkable increase of GW-induced density ...
arxiv +1 more source
A Thermal Plume Model for the Martian Convective Boundary Layer [PDF]
Journal of Geophysical Research: Planets. Volume 118, Issue 7,
pages 1468-1487, July 2013, 2013 The Martian Planetary Boundary Layer [PBL] is a crucial component of the Martian climate system. Global Climate Models [GCMs] and Mesoscale Models [MMs] lack the resolution to predict PBL mixing which is therefore parameterized. Here we propose to adapt the "thermal plume" model, recently developed for Earth climate modeling, to Martian GCMs, MMs, and ...
arxiv +1 more source
Martian Dust Storms and Gravity Waves: Disentangling Water Transport to the Upper Atmosphere [PDF]
, 2022 Simulations with the Max Planck Institute Martian general circulation model for Martian years 28 and 34 reveal details of the water "pump" mechanism and the role of gravity wave (GW) forcing. Water is advected to the upper atmosphere mainly by upward branches of the meridional circulation: in low latitudes during equinoxes and over the south pole ...
arxiv +1 more source
Evolution of Water Reservoirs on Mars: Constraints from Hydrogen Isotopes in Martian Meteorites [PDF]
, 2014 Martian surface morphology implies that Mars was once warm enough to maintain persistent liquid water on its surface. While the high D/H ratios (~6 times the Earth's ocean water) of the current martian atmosphere suggest that significant water has been lost from the surface during martian history, the timing, processes, and the amount of the water loss
arxiv +1 more source
Strong depletion of $^{13}$C in CO induced by photolysis of CO$_{2}$ in the Martian atmosphere calculated by a photochemical model [PDF]
arXiv, 2023 The isotopic signature of atmospheric carbon offers a unique tracer for the history of the Martian atmosphere and the origin of organic matter on Mars. Photolysis of CO$_{2}$ is known to induce strong isotopic fractionation of carbon between CO$_{2}$ and CO.
arxiv
CO+ first-negative band emission: A tracer for CO in the Martian upper atmosphere [PDF]
A&A 639, A60 (2020), 2020 Recently, Imaging Ultraviolet Spectrograph (IUVS) on-board Mars Atmosphere and Volatile EvolutioN (MAVEN) satellite observed CO$^+$ first-negative band limb emission in the Martian upper atmosphere. We aim to explore the photochemical processes in the Martian upper atmosphere, which drives this band emission. A photochemical model is developed to study
arxiv +1 more source