TY - JOUR
T1 - An Investigation of the Encirclement of Mars by Dust in the 2018 Global Dust Storm Using EMARS
AU - Gillespie, H. E.
AU - Greybush, S. J.
AU - Wilson, R. J.
N1 - Funding Information:
We thank Luca Montabone for facilitating access to the dust opacity maps used as inputs to EMARS, and to the MCS team, especially David Kass and Armin Kleinboehl, for consultation on the best use of MCS data. This research was supported by the NASA Mars Data Analysis Program Grant 80NSSC17K0690. EMARS data shown in this paper from before MY 34 are available from the Penn State Data Commons at https://doi.org/10.18113/d3w375 (Greybush et al., 2019 ). Data from the MY 34 dust storm are available publicly in the Penn State Data Commons at https://doi.org/10.26208/e67e‐w443 .
Funding Information:
We thank Luca Montabone for facilitating access to the dust opacity maps used as inputs to EMARS, and to the MCS team, especially David Kass and Armin Kleinboehl, for consultation on the best use of MCS data. This research was supported by the NASA Mars Data Analysis Program Grant 80NSSC17K0690. EMARS data shown in this paper from before MY 34 are available from the Penn State Data Commons at https://doi.org/10.18113/d3w375 (Greybush et al., 2019). Data from the MY 34 dust storm are available publicly in the Penn State Data Commons at https://doi.org/10.26208/e67e-w443.
Publisher Copyright:
©2020. American Geophysical Union. All Rights Reserved.
PY - 2020/7/1
Y1 - 2020/7/1
N2 - Determining how global dust storms originate and develop is one of the major challenges of Martian meteorology. We model the 2018 global dust storm using the Ensemble Mars Atmosphere Reanalysis System (EMARS), combining satellite observations with a Mars global climate model via data assimilation. A reanalysis is a valuable data set for this investigation because it is anchored to the real Martian atmosphere by temperature and dust observations, and the model provides full 4D coverage of wind fields, which are not directly observed and are key to assessing advection. Dust was observed to encircle the northern hemisphere early on in the storm's development. This encirclement could be caused by either the formation of new lifting centers along the path of observed encirclement or the advection of dust from active lifting center(s) elsewhere. Results from EMARS, including particle advection from inferred EMARS winds, provide evidence that the aforementioned dust encircling Mars's northern hemisphere may come from the initial lifting center of the storm, near Chryse Planitia. We propose that dust from the initial lifting center of the storm was entrained into the Martian Hadley circulation, with the assistance of the thermal tides, and then entrained into the northern hemisphere westerly jet.
AB - Determining how global dust storms originate and develop is one of the major challenges of Martian meteorology. We model the 2018 global dust storm using the Ensemble Mars Atmosphere Reanalysis System (EMARS), combining satellite observations with a Mars global climate model via data assimilation. A reanalysis is a valuable data set for this investigation because it is anchored to the real Martian atmosphere by temperature and dust observations, and the model provides full 4D coverage of wind fields, which are not directly observed and are key to assessing advection. Dust was observed to encircle the northern hemisphere early on in the storm's development. This encirclement could be caused by either the formation of new lifting centers along the path of observed encirclement or the advection of dust from active lifting center(s) elsewhere. Results from EMARS, including particle advection from inferred EMARS winds, provide evidence that the aforementioned dust encircling Mars's northern hemisphere may come from the initial lifting center of the storm, near Chryse Planitia. We propose that dust from the initial lifting center of the storm was entrained into the Martian Hadley circulation, with the assistance of the thermal tides, and then entrained into the northern hemisphere westerly jet.
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U2 - 10.1029/2019JE006106
DO - 10.1029/2019JE006106
M3 - Article
AN - SCOPUS:85088571476
SN - 2169-9097
VL - 125
JO - Journal of Geophysical Research: Planets
JF - Journal of Geophysical Research: Planets
IS - 7
M1 - e2019JE006106
ER -