1 / 33

Mid-IR observations of Mercury’s Surface as related to MERTIS and PEL and BED (and SERENA, of course)

Mid-IR observations of Mercury’s Surface as related to MERTIS and PEL and BED (and SERENA, of course). Ann L. Sprague Lunar and Planetary Laboratory, Tucson, AZ, USA With many collaborators over 2 decades: Surface studies:

ipo
Download Presentation

Mid-IR observations of Mercury’s Surface as related to MERTIS and PEL and BED (and SERENA, of course)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Mid-IR observations of Mercury’s Surface as related to MERTIS and PEL and BED (and SERENA, of course) SERENA, Santa Fe, NM

  2. Ann L. Sprague Lunar and Planetary Laboratory, Tucson, AZ, USA With many collaborators over 2 decades: Surface studies: GROUND-BASED--Kozlowski,Donaldson Hanna, Warell, Helbert, Maturilli, Russel, Lynch, Witteborn, Lebofsky, Wooden, Hora, Kasis, Cruikshank, Graps, Deutch MESSENGER--MASCS, GRNS, XRS: Domingue, Vilas, McClintock, Izenberg, Holsclaw, Blewett, Head, Helbert, McCoy, Murchie, Goldsten, Lawrence, Boynton, Feldman, Evans, Nittler, Schlemm, Rhodes, Starr, Robinson, Solomon and the MESSENGER TEAM SERENA, Santa Fe, NM

  3. Ground-based and MESSENGER VIS NIR spectroscopy demonstrated no or very little FeO in Mercury’s regolith Ground-based summary: Vilas et al. (1994) A couple of detections of shallow Fe-bearing clinopyroxene at both N and S at high latitudes, 170º to 230º E Warell et al. (2006) MESSENGER MASCS McClintock et al. Submitted to Science, 2008 SERENA, Santa Fe, NM

  4. What might we see with the neutral and ionised particle analyser SERENA (IFSI Italy) coming directly from Mercury’s surface? SERENA, Santa Fe, NM

  5. 55N, 27S; • 6E, 354W • radar spots • B and A • b. Same • c. Same, also Kuiper-Murasaki craters • d. Spots B and A • e. Same • f. Same • g. Caloris Basin • h. 65N, 155W • 0, 125W • 9S, 105W • i. 35S, 43-73W SERENA, Santa Fe, NM Sprague et al. 1998

  6. atmospheric K emission surface reflection in band continuum Adapted from Potter and Morgan PSS (1997) SERENA, Santa Fe, NM

  7. The Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) H. Hiesinger, J. Helbert and the MERTIS Co-I Team SERENA, Santa Fe, NM

  8. Plagioclase in some detail Data from PEL, Berlin Emissivity Database, (Helbert et al. 2006) SERENA, Santa Fe, NM

  9. Credit: NASA/Johns Hopkins University Applied Physics Laboratory /Carnegie Institution of Washington New: There are composition differences between Caloris Basin, dark plains material, and radar bright region “C” SERENA, Santa Fe, NM

  10. MDIS image of region measured in mid-infrared spectral imaging discussed in this paper. This region, also known as radar bright region "C" also has a prominent impact crater centered at 114°E, 11° N and its system of ejecta rays appearing brighter against the darker heavily cratered surface beneath. SERENA, Santa Fe, NM

  11. 210º to 270º W Longitude (left) Goldstone-VLA X-band imaging showing radar-bright region "C" as the dark irregular patch--adapted from Butler et al. (1993). (right) Aricebo S-band dual polarization, delay-Doppler imaging showing same region as heavily cratered. Only the regions north of the "ambiguity line" approximately at the equator are relevant-- reproduced from Harmon et al. (2007). SERENA, Santa Fe, NM

  12. Key to Mineral types on following slides • Pyroxenes • (e) enstatite: Mg-rich (h) hypersthene: Mg,Fe • (diop) diopside: Ca,Mg (hed) hedenbergite Fe,Ca • Plagioclase Na-rich ~90 down to 30 wgt% Na • (and) andesine Na (olig) oligiclase Na • (lab) labradorite Na,Ca (byt) bytownite Ca,Na • Olivine • Mg-rich variety ~70 to 97 wgt% >>>FO(70), FO(97) • Garnet • (p) pyrope Mg - variety • (g) grossular Ca-variety SERENA, Santa Fe, NM

  13. bright region "C" data--black • models --grey • wide range of grain sizes • 5 options for comparison • 4 different opaque phases • a)90 spectral end members • 180 spectral end members • b) rutile (TiO2) permitted, • rutile chosen • c) ilmenite permitted (FeTiO3), but ilmenite not chosen • d) perovskite (CaTiO3) • permitted, perovskite chosen • e) troilite (FeS) permitted, troilite chosen SERENA, Santa Fe, NM

  14. orthopyroxene SERENA, Santa Fe, NM

  15. plagioclase feldspar SERENA, Santa Fe, NM

  16. SERENA, Santa Fe, NM

  17. Low albedo Smooth plains Caloris Basin smooth plains • Color and albedo controlled by maturity and composition • Map units statistically, next step is determine origin • PC 2 interpreted to represent compositional variation Low albedo material “streak” MNF (minimum noise fraction, similar to PC) 2-1-3 as R-G-B Low albedo material From Robinson et al. LPSC 2008 SERENA, Santa Fe, NM PC 2

  18. Next sequences from Donaldson Hanna et al 2008 EGU, Vienna, Austria SERENA, Santa Fe, NM

  19. Caloris Basin Observations 8 April 2006 - 0080 9 April 2006 - 0070 SERENA, Santa Fe, NM

  20. Best Fit Models – Caloris Basin EM TM 8 April 2006 TM EM 9 April 2006 SERENA, Santa Fe, NM

  21. Potassium feldspars: K-spars SERENA, Santa Fe, NM

  22. Caloris Basin Results SERENA, Santa Fe, NM

  23. Dark Plains Observations 8 April 2006 - 0098 9 April 2006 - 0063 SERENA, Santa Fe, NM

  24. Best Fit Models – Dark Plains TM EM 8 April 2006 TM EM 9 April 2006 SERENA, Santa Fe, NM

  25. Dark Plains Results SERENA, Santa Fe, NM

  26. Rutile TiO2 SERENA, Santa Fe, NM

  27. Perovskite CaTiO3 SERENA, Santa Fe, NM

  28. Ilmenite FeTiO3 SERENA, Santa Fe, NM

  29. Meteoritic troilite FeS SERENA, Santa Fe, NM

  30. SERENA, Santa Fe, NM

  31. SERENA, Santa Fe, NM

  32. Challenges for SERENA ●Quantify neutral and ions sputtered Mg, Al, Ca, O, etc. from pyroxenes and feldspars ●Quantify Na, K, and if possible locate it ● Distinguish between solar Fe and Fe from surface materials—is it possible? ● Perhaps use knowledge of H, H2 and He as a “boot strap” to distinguishing between solar wind and surface mineral partitioning?? SERENA, Santa Fe, NM

  33. This slide left intentionally empty end of presentation SERENA, Santa Fe, NM

More Related