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GROOVES OF PHOBOS AS SEEN ON THE MEX HRSC RECTIFIED IMAGES AND

GROOVES OF PHOBOS AS SEEN ON THE MEX HRSC RECTIFIED IMAGES AND COMPARISONS WITH PLANETERY ANALOGS A.T. Basilevsky 1 , J. Oberst 2,3 , K. Willner 3 , M. Waehlisch 3 , G. Neukum 4 1 Vernadsky Institute, Moscow, Russia, 2 DLR Berlin, Germany,

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GROOVES OF PHOBOS AS SEEN ON THE MEX HRSC RECTIFIED IMAGES AND

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  1. GROOVES OF PHOBOS AS SEEN ON THE MEX HRSC RECTIFIED IMAGES AND COMPARISONS WITH PLANETERY ANALOGS A.T. Basilevsky1, J. Oberst2,3, K. Willner3, M. Waehlisch3, G. Neukum4 1Vernadsky Institute, Moscow, Russia, 2DLR Berlin, Germany, 3TU Berlin Germany, 4Free University Berlin, Germany Contact: atbas@geokhi.ru or alexander_basilevsky@brown.edu The Second Moscow Solar System Symposium Space Research InstituteMoscow, Russia10-14 October 2011

  2. Grooves on Phobos, What is their origin? There are considered several hypotheses:

  3. Fractures from crater-forming impacts e.g., Thomas et al., …1978

  4. The younger fractures typically abut against the older ones. Elysium, Mars, HIRISE image PSP_010348_1870.

  5. SW of crater Drunlo, observed in HRSC images of the orbits: 6906 (a, b), 4847 (c, d), and 2813 (e, f), reprojected for central longitude 102oW. No abuttings, No lateral offsets at intersections of grooves of different trends (different ages) are seen. Phobos groove intersections

  6. Martian potential analogs - pits and graben Collapsed pits in Cyane Fossae. Pits have no raised rims as some Phobos grooves have. HIRISE image PSP_010345_2150.

  7. Martian potential analogs - graben Graben near Alba Patera.They have no raised rims. THEMIS image V20111005.

  8. Martian potential analogs - graben Young faults Older faults Intersecting graben near Alba Patera. No abuttings, no lateral offsets of the younger faults at intersections are seen. THEMIS image V20111005.

  9. Scars formed by ejecta from Stickney and other craters e.g., Head and Wilson, …2010, Duxbury, 2010

  10. The HRSC images of craters Drunlo (lower left, D = 4.2 km) and Clustril (upper right, D = 3.4 km). All images are reprojected for central longitude 31oW. Plates a to f are from images obtained at the orbits 0756 (image a), 2780 (b, f), 2813 (c), 3310 (d) and 5851 (e). Grooves crossing the craters show no gaps at the crater rims in contrast to trails of bouncing boulders seen on slopes of lunar relief (see the next slides).

  11. Lunar analogs Downrange bright marks (white arrows) formed by a bouncing boulder (black arrow). LROC image M110383422R. Boulder trails on the wall of 15 km crater. LROC image M107985155LE

  12. Lunar analogs Long jump after crater rim Boulder trail crossing the 100 m crater on the wall of 15 km unnamed crater. LROC image M107985155LE. Details of boulder trail crossing the crater. LROC image M107985155LE

  13. Lunar analogs Boulders reaching the floor traveled only 50-100 m. LROC image M107985155LE. Boulders reached the crater floor. LROC image M107985155LE. Inertia is not a powerful mover

  14. Secondary impact craters chains. produced by ejecta from Mars craters e.g., Murrey, …2010

  15. Grooves morphology along 90o angular distance (left-right). Fragment of image taken during orbit 0756 (central longitude 31oW). Craters Drunlo and Clustril are in the image right. If grooves were formed by secondary impacts from Mars craters, one would expect a change in groove-forming crater morphology due to change in impact angle.

  16. Lutetian potential analogs - grooves 100 km asteroid Lutetia: No regular source of external secondaries Image taken by the OSIRIS camera. Rosetta, ESA.

  17. Grooves on Lutetia Grooves and crater chains similar to those observed on Phobos (upper red box on synoptic image)

  18. Grooves on Lutetia Grooves and crater chains similar to those observed on Phobos (lower red box on the synoptic image).

  19. Vestian potential analogs - grooves 500 km asteroid Vesta: No regular external source of secondaries (Dawn image 571329main_pia14313-full_full.jpg) Its surface shows many grooves, some very similar to grooves of Phobos.

  20. Phobos grooves 20 km stone is needed to produce this groove Grooves of Vesta looking similar to those observed on Phobos.

  21. Conclusions: • All suggested hypotheses of formation of grooves • on Phobos have their strong and weak sides. • Further analysis is needed to resolve the problem • of the groove formation. • Currently it looks that hypotheses of scars from • rolling stones and chains of secondary craters • produced by ejecta from Mars contradict • observations on lunar & asteroidal analogs. • Further analysis is needed to resolve theproblem • of absence of abutting and lateral offset in the • fracturing mechanism of the groove formation.

  22. Thank you for your attention

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