A circular feature was observed on Mars by the HiRISE camera. From DTM analysis its circular positive relief shape has been interpreted as diapiric phenomenon

CREMONESE, Gabriele

Massironi, M.

Pozzobon, R.

RE, Cristina

OA@INAF - Istituto Nazionale di Astrofisica

2015Publication Year2020-03-14T14:15:58ZAcceptance in OA@INAFA Possible Diapir in Athabasca Region on MarsTitlePozzobon, R.; CREMONESE, Gabriele; Massironi, M.; RE, CristinaAuthorshttp://hdl.handle.net/20.500.12386/23239HandleA POSSIBLE DIAPIR IN ATHABASCA REGION ON MARS    R. Pozzobon1, G. Cremonese1, M. Massironi2 , C. Re1; 1INAF - Osservatorio Astronomico di Padova (ppoz-zopp@gmail.com),  2Dipartimento di Geoscienze, Università degli Studi di Padova    Introduction:  An interesting circular feature has been observed on Mars by the HiRISE (High Resolution Imaging Science Experiment) camera on board the NASA’s Mars Reconnaissance Orbiter (MRO). Located  at  0°17'N- 159°13'E, its diameter is ~2 km and it lies in the Athabasca region near the equator, in the South-Eastern sector of Elysi-um volcanic province. In this work, after having reconstruct-ed its topography through photogrammetry, we propose its possible genesis as an uprising diapir.  Figure 1: Dome-like feature in Athabasca region Wrinkles all around the circular feature are visible, whereas a crater-rim all around the dome is possible, although not certain. (HiRISE image ESP_013249_1805).  DTM generation:  The DTM generation has been per-formed following a photogrammetric workflow. The files have been fed into ISIS3 (Eliason, 1997), radiometrically calibrated and finally the images are ortho-rectified with cam2map program (i.e. projected onto the reference surface of the Mars spheroid). The correlation phase have been per-formed with the Area Based image matching software named “Dense Matcher” (Re, 2012). The software, developed at the University of Parma, have been used in order to compute the image correspondences implementing a disparity map initial-ization with NCC algorithm (Lewis, 1995) and a sub-pixel refinement by an advance Least Squares Matching algorithm (Gruen, 1985) that exploits a polynomial transformation as geometrical resampling model. As far as the triangulation stage is concerned, the Ames Stereo Pipeline (ASP) routine have been used by suitably modifying the Dense Matcher disparity map to produce an input data in the format accepted by ASP. Any Bundle Block Adjustment has been performed. In fig. 2 are displayed 3 DTM profiles, obtained at different angles. It does not appear a well-defined rim suggesting that the positive circular morphology might not be formed after an impact, or the rim has been obscured by embayment and burial.  Figure 2: DTM profiles generated from HiRISE im-agesESP_013249_1805 and ESP_038646_1805 with Dense Matcher.   Geologic interpretation:  The annular wrinkles surround-ing the body are not coherent with a lava flow moving around the rim. In fact in this area most of the lava flows tend to flow with NW to SE direction and we would have expected that wrinkled contacts with the rim would concen-trate on the direction of the lava flow (as in fact happens with other impact craters in the same area) or being absent. In-stead we can recognize a wrinkled margin all around the borders of the circular body, that instead seems to be more coherent with a diapiric ascent deformation. Indeed Sub-volcanic intrusions might actually evolve in extruding domes which can find their way to the surface by breaking apart the overburden, eventually creating slightly uplifted rims.  We think that being in a volcanic field (near to Elysium plan-itia, one of the main volcanic centres on Mars) whose main geological features are volcanic vents and widespread basal-tic lava flows, this feature would likely be originated as an 2142.pdf46th Lunar and Planetary Science Conference (2015)uprising ascent of a subvulcanic body or a salt diapir. Alt-hough at the time being there is no spectral evidence of salt presence in this area, also due to the lack of available CRISM data, salts mobilization in the dynamic context of such a volcanic field could still be possible (see Schofield et al., 2014). Either being a plutonic body or a salt mobilization, the dome-like feature is apparent both from the HiRISE images and from the Stereo DTM. A similar object has been found in the north-eastern Orcus Patera region (fig.3), a volcanic field covered by extensive lava flows as well.  Figure 3:A dome-like feature similar to Figure 1. in Orcus Patera region. (P07_003623_1903_XN_10N185W CTX image).  This second feature, located at 10° 8'N- 174°31'E (fig. 3), it is similar in size to the former one and ,at the CTX (Context camera) image resolution (6m/pixel), completely lacks of any rim-like feature. Its elliptical shape might be related to the fact that we are not in presence of a possible  pre-existing impact crater that might have focused diapiric ascent as could potentially be the case in the Athabasca region.    Discussion and conclusions: In a volcanic field context the presence and uprising of plutonic bodies is likely and widely seen on Earth. The mechanism of ascent to explain dome-like features such the ones of figure 1 and 3 would most likely be the buoyancy forces and the lower density of a magmatic body. The ∆ρ between the magmatic body and the bed-rocks is normally enhanced by presence of volatile phases or/and water/fluids. In addition, we cannot exclude a different and more evolved composition of  a sub-volcanic uprising body (eg. andesite vs. basalt).   Hence, according to our opinion the features of figures 1 and 3 may have a diapiric origin, either being an intrusive dome within a volcanic context whose shape and morphology is coherent with Namibian plutonic domes (e.g. 21°6’S – 14°33’E), or an uprising salt diapir (see Zagros diapir field 26°33’N  - 54°40’E) whose topography have a good match with our HiRISE stereo DTM.  References: [1] De Pablo, M.A., Komatsu, G., 2008. Icarus 2; [2] Koyi, H. J. Struct. Geol. 20, 321–338 (1998). [3] Schofield, N. et al. Geology (2014). doi:10.1130/G35406.1;  [4] Sherkati, S. & Letouzey, J. Mar. Pet. Geol. 21, 535–554 (2004). [5] Re C., Roncella R., Forlani G., Cremonese G., Naletto G. 2012, Int. Arch. of Photogrammetry, Remote Sensing and Spatial Information Sciences, Vol XXXIX, Part IV/7; [6] Vackiner, A. A. et al. 2013, Int. J. Earth Sci. 102, 1701–1716.  2142.pdf46th Lunar and Planetary Science Conference (2015)

A Possible Diapir in Athabasca Region on Mars

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A Possible Diapir in Athabasca Region on Mars

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