50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1364.pdf LARGEST THARSIS VOLCANOES KEEP GROWING AND MARK >4-GA-LASTING MARTIAN HOT SPOTS. J. Ciazela1, D. Mège1, B. Pieterek2, M. Ciazela1, J. Gurgurewicz1, A. Lagain3, and P.-A. Tesson1, 1Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw, Poland (
[email protected]), 2Institute of Geology, Adam Mickiewicz University, ul. Bogumila Krygowskiego 12, 60-680 Poznan, Poland, 3Space Science and Technology Centre, Curtin University, Kent Street, Bentley, Perth, Western Australia 6102, Australia. Introduction: Due to the lack of plate tectonics The volumes were calculated with ArcMap using and magnetic field, the Martian core was long inter- the digital elevation model (DEM) from MOLA/MGS preted to be entirely solid and volcanism on Mars ex- (128 pixels/degree). In order to estimate a realistic tinct. This has been recently questioned by several error on the method, we have also computed simplified works suggesting existence of a liquid outermost layer volumes from the right conical frustums approximating at the Martian core [1–3]. The liquid core would ex- volcano shapes. The error bars in Fig. 1 represent the plain the growing body of evidence for recent (2-250 average relative volume difference between the DEM- Ma) Martian volcanism [4–10], and volcanic gases derived and simplified volumes. (i.e., CH4, H2S, SO2, and HCl) are currently tracked Results and Discussion: Our results indicate a sig- down by the ExoMars Trace Gas Orbiter (TGO) [11, nificant inverse correlation (R2 = 0.83) between volca- 12]. Two million years make up <0.1% of the Mars no volume and youngest summit caldera age, con- age (4567 myr) indicating timespan of volcano erup- sistent with earlier studies [4, 6] (Fig.