Flood Volcanism in the Northern High Latitudes of Mercury Revealed by MESSENGER

Head, J. W.; Chapman, C. R.; Strom, R. G.; Fassett, C. I.; Denevi, Brett W.; Blewett, D. T.; Ernst, C. M.; Watters, T. R.; Solomon, Sean C.; Murchie, S. L.; Prockter, L. M.; Chabot, N. L.; Gillis-Davis, J. J.; Whitten, J. L.; Goudge, T. A.; Baker, D. M. H.; Hurwitz, D. M.; Ostrach, L. R.; Xiao, Zhiyong; Merline, W. J.; Kerber, L.; Dickson, J. L.; Oberst, J.; Byrne, P. K.; Klimczak, C.; Nittler, L. R.

doi:10.1126/science.1211997

Cited by 223 publications

(274 citation statements)

References 29 publications

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“…In the north polar region of Mercury, SP are known as the 'Northern smooth plains' (SPn, Denevi et al, 2013;Ostrach et al, 2015); inside the H02 quadrangle most of the mapped SP pertain to this unit ( Figure 6). Several authors believe SP belong to the Calorian period estimating an age of 3.7-3.9 Ga based on crater density distribution (Denevi et al, 2013;Fassett et al, 2009;Head et al, 2011;Ostrach, Robinson, Denevi, & Thomas, 2011;Strom, Chapman, Merline, Solomon, & Head, 2008, 2011.…”

Section: Smooth Plainsmentioning

confidence: 99%

Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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Mercury's quadrangle H02 'Victoria' is located in the planet's northern hemisphere and lies between latitudes 22.5°N and 65°N, and between longitudes 270°E and 360°E. This quadrangle covers 6.5% of the planet's surface with a total area of almost 5 million km 2 . Our 1:3,000,000-scale geologic map of the quadrangle was produced by photo-interpretation of remotely sensed orbital images captured by the MESSENGER spacecraft. Geologic contacts were drawn between 1:300,000 and 1:600,000 mapping scale and constitute the boundaries of intercrater, intermediate and smooth plains units; in addition, three morpho-stratigraphic classes of craters larger than 20 km were mapped. The geologic map reveals that this area is dominated by Intercrater Plains encompassing some almost-coeval, probably younger, Intermediate Plains patches and interrupted to the north-west, north-east and east by the Calorian Northern Smooth Plains. This map represents the first complete geologic survey of the Victoria quadrangle at this scale, and an improvement of the existing 1:5,000,000 Mariner 10-based map, which covers only 36% of the quadrangle. ARTICLE HISTORY

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Section: Smooth Plainsmentioning

confidence: 99%

Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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“…Similar high-reflectance material is recognized elsewhere on the planet within craters and basins, particularly associated with the Caloris basin (Denevi et al, 2009). These areas have ages near the end of the Late Heavy Bombardment (3.7-3.8 Ga; Head et al, 2011) and may have a volcanic origin, while some might represent impact melts and/or basin ejecta (Denevi et al, 2009). Recent volcanism, possibly as young as 1 Ga, has been identified near the Rachmaninoff basin, suggesting prolonged duration of volcanic activity on Mercury (Prockter et al, 2010).…”

Section: Compositional Variation and Terrains On Mercurymentioning

confidence: 99%

“…Data treated in this study do not include the northern volcanic plains described by Head et al (2011). The ten XRS measurements discussed here have been acquired at high altitudes and thus cover large areas averaging the composition of various units (Fig.…”

Section: Introductionmentioning

confidence: 99%

Phase equilibria of ultramafic compositions on Mercury and the origin of the compositional dichotomy

Charlier

Grove

Zuber

2013

Earth and Planetary Science Letters

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a b s t r a c tMeasurements of major element ratios obtained by the MESSENGER spacecraft using x-ray fluorescence spectra are used to calculate absolute element abundances of lavas at the surface of Mercury. We discuss calculation methods and assumptions that take into account the distribution of major elements between silicate, metal, and sulfide components and the potential occurrence of sulfide minerals under reduced conditions. These first compositional data, which represent large areas of mixed highreflectance volcanic plains and low-reflectance materials and do not include the northern volcanic plains, share common silica-and magnesium-rich characteristics. They are most similar to terrestrial volcanic rocks known as basaltic komatiites. Two compositional groups are distinguished by the presence or absence of a clinopyroxene component. Melting experiments at one atmosphere on the average compositions of each of the two groups constrain the potential mineralogy at Mercury's surface, which should be dominated by orthopyroxene (protoenstatite and orthoenstatite), plagioclase, minor olivine if any, clinopyroxene (augite), and tridymite. The two compositional groups cannot be related to each other by any fractional crystallization process, suggesting differentiated source compositions for the two components and implying multi-stage differentiation and remelting processes for Mercury. Comparison with high-pressure phase equilibria supports partial melting at pressure o10 kbar, in agreement with last equilibration of the melts close to the crust-mantle boundary with two different mantle lithologies (harzburgite and lherzolite). Magma ocean crystallization followed by adiabatic decompression of mantle layers during cumulate overturn and/or convection would have produced adequate conditions to explain surface compositions. The surface of Mercury is not an unmodified quenched crust of primordial bulk planetary composition. Ultramafic lavas from Mercury have high liquidus temperatures (1450-1350 1C) and very low viscosities, in accordance with the eruption style characterized by flooding of pre-existing impact craters by lava and absence of central volcanoes.

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“…Although no diagnostic volcanic features or constructs were conclusively identified in the Mariner 10 images, possibly due to resolution and illumination limitations (Schultz, 1977;Malin, 1978;Milkovich et al, 2002), a volcanic origin for much of the smooth plains was favored on the basis of their widespread distribution, embayment relations with surrounding topography, visible color properties, relatively young age, and superposed tectonic features (e.g., Murray et al, 1974b;Strom et al, 1975b;Trask and Strom, 1976;Kiefer and Murray, 1987;Spudis and Guest, 1988;Robinson and Lucey, 1997;Robinson and Taylor, 2001). Although a volcanic origin for smooth plains on Mercury was called into question (Wilhelms, 1976;Oberbeck et al, 1977), and although it is certainly possible that some smooth plains deposits are impact-generated products (i.e., fluidized ejecta, impact melt), most regions of smooth plains are now interpreted as products of effusive volcanism, much like the lunar maria (Murray et al, 1974b;Murray, 1975;Trask and Guest, 1975;Strom et al, 1975b;Trask and Strom, 1976;Kiefer and Murray, 1987;Robinson and Lucey, 1997;Head et al, 2008Head et al, , 2009aHead et al, , 2011Murchie et al, 2008;Robinson et al, 2008;Solomon et al, 2008;Denevi et al, 2009Denevi et al, , 2013aErnst et al, 2010;Fassett et al, 2009;Kerber et al, 2009Kerber et al, , 2011Watters et al, 2009Watters et al, , 2012Prockter et al, 2010;Freed et al, 20...…”

Section: Introductionmentioning

confidence: 99%

“…The northern smooth plains are relatively flat, have fewer superposed impact craters than the surrounding heavily cratered terrain (Murray et al, 1974b;Strom et al, 1975b;Guest and Gault, 1976), and are morphologically similar to the lunar maria (e.g., Murray et al, 1974aMurray et al, , 1974bMurray, 1975;Strom et al, 1975b;Head et al, 2008Head et al, , 2011. Smooth plains units identified from Mariner 10 images (e.g., Murray et al, 1974b;Murray, 1975) have a lower crater density than the heavily cratered terrain, indicating that the smooth plains are resolvably younger.…”

Section: Introductionmentioning

confidence: 99%