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Parasitic Cones in Tharsis Volcanic Province on Mars: Implications for Its Recent Magmatic Plumbing System B

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Parasitic cones in Tharsis volcanic province on Mars: Implications for its recent magmatic plumbing system B. Pieterek [1] , J. Ciążela [2] , D. Mège[2], P.-A. Tesson[2], M. Ciazela[2], J. Gurgurewicz[2], A. Lagain[3], A. Muszyń ski[1] [1]Institute of Geology, Adam Mickiewicz University, ul. Bogumila Krygowskiego 12, 60-680 Poznan, Poland ([email protected]), [2]Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw, Poland, [3]School of Earth and Planetary Science, Curtin University, GPO Box U1987, Perth, WA, 6845, Australia Introduction: Methods: Although Tharsis is the largest volcanic province on Mars, the origin of numerous small 1) The parasitic cones were mapped and dated using ArcMap software combining imagery from: volcanic cones in this area is not yet fully explained. Their genesis may be related to: the Thermal Emission Imaging System (THEMIS) of Mars Odyssey (MO) (spatial resolution 1) the evolution of larger volcanic ediices (Hughes et al., 2005), such as Olympus Mons or the of ~100 m/pixel); Tharsis Montes the Context Camera (CTX) of Mars Reconnaissance Orbiter (MRO) (6 m/pixel). 2) local tectonic trends (Hauber et al., 2009), independent younger magma production events 2) The orientations were plotted on the rose diagrams using Stereonet 10.2. (Bleacher et al., 2007, 2009), or locally-restricted stress ields that differed from the giant 3) Selected parasitic cones were dated using crater counting (>100 m in diameter) with the volcano caldera-wide stress regime (Mouginis-Mark and Christensen, 2005). ArcGIS extension CraterTools2.1 (Kneissl et al., 2011). Ages were obtained by CraterStats II Characterizing the system of small volcanic cones in terms of space and time is essential to (Michael and Neukum, 2010) by applying the Hartmann's [2005] chronology system (Hartmann, understand the Tharsis magmatic plumbing complex. 2005; Michael, 2013). Results: 135°W 120°W 105°W 90°W 130°W 125°W 120°W Alba Mons A 20°N In this study, we analyze (1) the spatial distribution, (2) 133±42 Ma ± Major volcanoes Olympus surface age as well as (3) orientation of volcano summit Mons Parasitic cones 64±26 Ma craters or central issure vents to determine whether or not N = 21 ± they are geologically associated with the major Tharsis Ages obtained by Ciazela et al., this meeting 30°N volcanoes. C 15°N 1) We mapped 309 parasitic cones of diameter >1 km, unevenly 200 km distributed across the Tharsis province. 2) We distinguish three major subprovinces related to A) 110°W 100°W Olympus Mons with orientations of (~N100E) B) Tharsis Olympus B ± Montes (~N055E), and C) Alba Mons (~N005E). Mons Pavonis 3) We dated 50 parasitic cones (A-C) in the identiied 64±26 Ma Mons A 138±13 Ma 0° subprovinces, as well as the most recent caldera activity of the 15°N giant volcanoes. Ascraeus Mons 193±17 Ma Arsia Age comparison between the three sets of parasitic cones (A-C) Mons 500 km 126±6 Ma and the related major volcanoes. 120°W 110°W 100°W Age (Ma) Subprovince C ± Major volcano Parasitic cones¹ N Pavonis B 0° Mons N = 88 138±13 Ma A Olympus Mons 64±26 70±25 17 126±6 20°N B Tharsis Montes 138±13 82±19 14 193±17 Arsia Mons Ascraeus 500 km Mons 126±6 Ma 193±17 Ma C Alba Mons 133±42 91±14 19 <40 Ma 75-100 Ma 50-75 Ma 100-120 Ma ¹arithmetic mean of all ages with standard deviation for parasitic cones within each subprovince; N - number of parasitic cones dated in each subprovince. Olympus Mons Tharsis Montes Alba Mons Discussion and conclusions: The spatial distribution, surface age, as well as orientation of volcano summit craters and central issure vents allow us to determine the geological link between the parasitic cones and the giant Tharsis volcanoes. Our results are supported by: Mouginis-Mark and Wilson (2019) who demostrate steady magma inlux from depth source near Olympus Mons consistent with the youngest activity of the parasitic cones (~40Ma); Richardson et al. (2017) who reveal that Arsia Mons might have had a magmatic pulse at ~100Ma summit craters suggesting link between parasitic cones (~82 Ma) and giant ediice. CTX P05_002829_2046_XN_24N110W Examples of volcanic CTX D05_029004_1954_XN_15N127W CTX B01_009870_1778_XI_02S_108W We conclude that recent or currently active major magma reservoirs may be present below Olympus Mons, Tharsis Montes, and perhaps Alba Mons, with auxiliary magmatic activity concentrating along the interconnecting system of N-S (N005E), W-E (N100E) and SW-NE (N055E) trending issures. OLYMPUS MONS SUMMIT CALDERA PARASITIC CONES W E fissure vent Three-dimensional (3D) block 5 [km] diagram of the Olympus Mons 10 subprovince based on the digital elevation model (DEM) from Examples of central CTX P19_008473_1952_XI_15N127W CTX P06_003330_2082_XN_28N108W CTX D12_031825_1789_XI_01S_106W 15 MAGMA MOLA/MGS (128 pixels/degree). 20 101 101 CHAMBER 3 2 No.3 Olympus Mons, area=2.34x102 km2 No. 29 Alba Mons, area=1.06x10 km No. 50 Tharsis Montes, area=5.80x102 km2 -5 -2 87 craters, N(1)=3.87x10-5 km-2 399 craters, N(1)=4.89x10 km 165 craters, N(1)=5.11x10-5 km-2 5 2 2 0 0 M M 10 a a 100 100 66±7 Ma 15 In addition, our results indicate that the small 20 84±5 Ma 88±7 Ma M volcanoes were forming (T₂) both during and P1 ag -1 -1 m 10 10 at after the end of the last eruptive activity at the ic a cti vity summit calderas of the nearby giant volcano P2 10-2 10-2 (T₁), this might be related to the smaller pressure (P₂) needed to feed these parasitic 10-3 10-3 cones compared to the pressure needed to feed Magma chamber pressure 5 km 10 km 105 km km PF: Mars, Hartmann (2005) PF: Mars, Hartmann (2005) PF: Mars, Hartmann (2005) T1 T2 Time summit calderas (P₁). CF: Mars, Hartmann (2005) [Michael (2013)] CF: Mars, Hartmann (2005) [Michael (2013)] CF: Mars, Hartmann (2005) [Michael (2013)] Major volcano Parasitic cone -4 Examples of dating 10-4 10 2m 4 8 16 31 63 125 250 500 1km 2 4 8 2m 4 8 16 31 63 125 250 500 1km 2 4 8 activity activity Diameter Diameter References Acknowledgements Bleacher, J.E., Glaze, L.S., Greeley, R., Hauber, E., Baloga, S.M., Sakimoto, S.E.H., Williams, D.A., Glotch, T.D., Kneissl, T., Van Gasselt, S., Neukum, G., 2011. Planet. Space Sci. 59, 1243–1254; This research is funded by European Funds Smart Growth (PO WER) project no. POWR.03.02.00-00-I027/17 and Foundation for Polish Science, program TEAM/2016- 2009. J. Volcanol. Geotherm. Res. 185, 96–102; Michael, G.G., 2013. Icarus 226, 885-890; 3/20. J. Ciazela is additionally supported within the START program of the Foundation for Polish Science (FNP) Bleacher, J.E., Greeley, R., Williams, D.A., Cave, S.R., Neukum, G., 2007. J. Geophys. Res. Planets 112, 1–15; Michael, G.G., Neukum, G., 2010. Earth Planet. Sci. Lett. 294, 223–229; Ciazela, J., Mege, D., Pieterek, B., Ciazela, M., Gurgurewicz, J., Lagain, A., Tesson, P.-A., 2019. LPSC 50, 1364; Mouginis-Mark, P.J., Christensen, P.R., 2005. J. Geophys. Res. 110, 1–17; Hartmann, W.K., 2005. Icarus 174, 294–320; Mouginis-Mark, P.J., Wilson, L., 2019. Icarus 319, 459–469; Hauber, E., Bleacher, J., Gwinner, K., Williams, D., Greeley, R., 2009. J. Volcanol. Geotherm. Res. 185, 69–95; Richardson, J.A., Wilson, J.A., Connor, C.B., Bleacher, J.E., 2017. Earth Planet. Sci. Lett. Hughes, S.S., Sakimoto, S.E.H., Gregg, T.K.P., Brady, S.M., 2005. LPSC 36, 2396; 458, 170-178..
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    p. 1 The Mars Global Surveyor Mars Orbiter Camera: Interplanetary Cruise through Primary Mission Michael C. Malin and Kenneth S. Edgett Malin Space Science Systems P.O. Box 910148 San Diego CA 92130-0148 (note to JGR: please do not publish e-mail addresses) ABSTRACT More than three years of high resolution (1.5 to 20 m/pixel) photographic observations of the surface of Mars have dramatically changed our view of that planet. Among the most important observations and interpretations derived therefrom are that much of Mars, at least to depths of several kilometers, is layered; that substantial portions of the planet have experienced burial and subsequent exhumation; that layered and massive units, many kilometers thick, appear to reflect an ancient period of large- scale erosion and deposition within what are now the ancient heavily cratered regions of Mars; and that processes previously unsuspected, including gully-forming fluid action and burial and exhumation of large tracts of land, have operated within near- contemporary times. These and many other attributes of the planet argue for a complex geology and complicated history. INTRODUCTION Successive improvements in image quality or resolution are often accompanied by new and important insights into planetary geology that would not otherwise be attained. From the variety of landforms and processes observed from previous missions to the planet Mars, it has long been anticipated that understanding of Mars would greatly benefit from increases in image spatial resolution. p. 2 The Mars Observer Camera (MOC) was initially selected for flight aboard the Mars Observer (MO) spacecraft [Malin et al., 1991, 1992].