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Widespread effusive volcanism on Mercury likely ended by about 3.5 Ga
Author(s) -
Byrne Paul K.,
Ostrach Lillian R.,
Fassett Caleb I.,
Chapman Clark R.,
Denevi Brett W.,
Evans Alexander J.,
Klimczak Christian,
Banks Maria E.,
Head James W.,
Solomon Sean C.
Publication year - 2016
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1002/2016gl069412
Subject(s) - impact crater , volcanism , volcano , geology , mercury (programming language) , planet , earth science , lava , astrobiology , geochemistry , seismology , tectonics , astronomy , physics , computer science , programming language
Crater size–frequency analyses have shown that the largest volcanic plains deposits on Mercury were emplaced around 3.7 Ga, as determined with recent model production function chronologies for impact crater formation on that planet. To test the hypothesis that all major smooth plains on Mercury were emplaced by about that time, we determined crater size–frequency distributions for the nine next‐largest deposits, which we interpret also as volcanic. Our crater density measurements are consistent with those of the largest areas of smooth plains on the planet. Model ages based on recent crater production rate estimates for Mercury imply that the main phase of plains volcanism on Mercury had ended by ~3.5 Ga, with only small‐scale volcanism enduring beyond that time. Cessation of widespread effusive volcanism is attributable to interior cooling and contraction of the innermost planet.