Recurrence rate and magma effusion rate for the latest volcanism on Arsia Mons, Mars

Richardson, J. A.; Wilson, James A.; Connor, Charles B.; Bleacher, J. E.; Kiyosugi, Koji

doi:10.1016/j.epsl.2016.10.040

Cited by 33 publications

(24 citation statements)

References 37 publications

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“…Both crater counting and planetary heat-flow models support this conclusion, as they demonstrate that the rate of volcanism during the Noachian and Hesperian (4500–3000 Ma) was at least 2–10 times greater than in the Amazonian (<3000 Ma) 3 , 4 , 7 . Our data compare favourably with remote-sensing crater-counting studies of Martian volcanoes 45 – 47 , which indicate that volcanism occurred at much lower rates in the recent past, compared to early in the planet’s history. For example, over the last 300 Ma the maximum effusion rate at the Arisa Mons volcano 47 was between 1 and 8 km 3 Ma −1 —well below the eruption rate of 270 km 3 Ma −1 averaged over the 3400 Ma duration of the volcano (Supplementary Table 1 ).…”

Section: Discussionsupporting

confidence: 66%

Taking the pulse of Mars via dating of a plume-fed volcano

et al. 2017

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Mars hosts the solar system’s largest volcanoes. Although their size and impact crater density indicate continued activity over billions of years, their formation rates are poorly understood. Here we quantify the growth rate of a Martian volcano by 40Ar/39Ar and cosmogenic exposure dating of six nakhlites, meteorites that were ejected from Mars by a single impact event at 10.7 ± 0.8 Ma (2σ). We find that the nakhlites sample a layered volcanic sequence with at least four discrete eruptive events spanning 93 ± 12 Ma (1416 ± 7 Ma to 1322 ± 10 Ma (2σ)). A non-radiogenic trapped 40Ar/36Ar value of 1511 ± 74 (2σ) provides a precise and robust constraint for the mid-Amazonian Martian atmosphere. Our data show that the nakhlite-source volcano grew at a rate of ca. 0.4–0.7 m Ma−1—three orders of magnitude slower than comparable volcanoes on Earth, and necessitating that Mars was far more volcanically active earlier in its history.

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Section: Discussionsupporting

confidence: 66%

Taking the pulse of Mars via dating of a plume-fed volcano

et al. 2017

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“…Although much of the topography is interpreted to have formed early in Martian history, modest volcanism persisted into the Amazonian. For example, Arsia Mons may have been active as recently as 10-90 Ma (Richardson et al 2017).…”

Section: Geologic Historymentioning

confidence: 99%

Pre-mission InSights on the Interior of Mars

et al. 2018

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The Interior exploration using Seismic Investigations, Geodesy, and Heat Transport (InSight) Mission will focus on Mars' interior structure and evolution. The basic structure of crust, mantle, and core form soon after accretion. Understanding the early differentiation process on Mars and how it relates to bulk composition is key to improving our understanding of this process on rocky bodies in our solar system, as well as in other solar B S.E. Smrekar

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“…A relatively young cluster of 29 low shield volcanoes comprises one such volcanic terrain on Mars, in the 110 km diameter caldera at the summit of Arsia Mons (Bleacher et al, 2010). Volcanism at this site has likely been extinct for tens of millions of years (Richardson et al, 2017), so the purpose of estimating the spatial density of vents is not to estimate locations of future vents. Instead, modes of vent spatial density indicate increased ability for the region to accumulate and/or erupt magma from given locations, which can provide insight into magma-tectonic interactions during epochs of volcanic activity.…”

Section: Example: Arsia Mons Marsmentioning

confidence: 99%

How to use kernel density estimation as a diagnostic and forecasting tool for distributed volcanic vents

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Germa

et al. 2019

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2019) How to use kernel density estimation as a diagnostic and forecasting tool for distributed volcanic vents, Statistics in Volcanology 4.3 : 1 − 25. AbstractVolcanic activity often results in the formation of new volcanic vents. These new vents can create hazards in unexpected areas. Therefore, the probability of new vent formation should be assessed as part of volcanic hazard assessments. This paper describes our use of kernel density estimation (KDE) as a way to estimate the spatial density of future volcanic vents. The bivariate Gaussian kernel function is described step-by-step using pseudocode. Our computer code, written in PERL, is used to calculate the spatial density of existing vents and then create a contour map using GMT (Generic Mapping Tools). Application of this method and code relies on several assumptions about the definition of volcanic events, independence of events, the type of kernel function used, and the selection of kernel bandwidth. Three examples using the code are provided: (1) for volcanic vents located west of the city of Managua (Nicaragua), (2) for volcanic vents distributed within the Arsia Mons caldera (Mars), weighted by volume, and (3) for vents of the Lassen volcanic system (northern California), sub-divided by geochemistry.

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Recurrence rate and magma effusion rate for the latest volcanism on Arsia Mons, Mars

Abstract: Magmatism and volcanism have evolved the Martian lithosphere, surface, and climate throughout the history of Mars. Constraining the rates of magma generation and timing of volcanism on the surface clarifies the ways in which magma

Cited by 33 publications

References 37 publications

Taking the pulse of Mars via dating of a plume-fed volcano

Taking the pulse of Mars via dating of a plume-fed volcano

Pre-mission InSights on the Interior of Mars

How to use kernel density estimation as a diagnostic and forecasting tool for distributed volcanic vents

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