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Distribution and Compositional Constraints on Subsurface Ice in Arcadia Planitia, Mars Ali M. Bramson1 S. Byrne1, N.E. Putzig2, S. Mattson1, J.J. Plaut3,

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Presentation on theme: "Distribution and Compositional Constraints on Subsurface Ice in Arcadia Planitia, Mars Ali M. Bramson1 S. Byrne1, N.E. Putzig2, S. Mattson1, J.J. Plaut3,"— Presentation transcript:

1 Distribution and Compositional Constraints on Subsurface Ice in Arcadia Planitia, Mars
Ali M. Bramson1 S. Byrne1, N.E. Putzig2, S. Mattson1, J.J. Plaut3, J.W. Holt4 Lunar and Planetary Laboratory, University of Arizona 2. Southwest Research Institute 3. Jet Propulsion Laboratory 4. Institute for Geophysics, University of Texas at Austin Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

2 Arcadia Planitia Northern mid-latitudes (~ 40°- 55°)
Amazonian-age volcanic terrain Numerous ice related features- many suggestive of excess ice (vs. pore-filling ice) Previously detected to have a widespread SHARAD subsurface reflector (Plaut et al. 2009, LPSC) Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

3 This Study Driving questions: How much excess ice is there?
How pure is it? 44°N vs Important to understanding amazonian climates in which this ice could have formed As well as be important for future human travel to Mars and astrobiology studies Have two ways to try to answer these questions by probing the subsurface...use of terraced craters…and SHARAD ground-penetrating radar Pore-filling ice in Antarctica Mellon et al. 2004 Excess ice exposed by recent impacts Dundas et al. 2014 Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

4 Cartoon of standard double-terraced crater profile
Terraced Craters 175 350 Meters 46.6°N, 194.8°E HiRISE Image: PSP_018522_2270 Form in layered targets- terraces at interfaces between different material strengths Constrain extent of ice by: mapping where terracing occurs Constrain thickness of ice by: making Digital Terrain Models (DTMs) from HiRISE stereo imagery measuring terrace depths Cartoon of standard double-terraced crater profile Floor terrace Wall terrace Pit Rock-ice interface ~40 m ~14 m Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

5 SHARAD Radar Radar reflectors appear when there is a contrast in dielectric properties Example Radargram delay time distance along track Radar Track Constrain extent of ice by: mapping where subsurface reflector occurs Constrain how pure ice is by: Calculating dielectric constant of layer Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

6 Map of Terraced Craters and Radar
Widespread Heterogenous Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

7 Cartoon of standard double-terraced crater profile
Dielectric Constants A measure of how effectively an EM wave moves through a material Air εr: ~1 Water Ice εr : ~3.15 Basalt εr: ~8 Cartoon of standard double-terraced crater profile Floor terrace Wall terrace Pit Rock-ice interface Layering within ice? Δx delay time Δt Constrain composition using the dielectric constant of the layer Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

8 Results 2 1 3 1 2 3 HiRISE stereo pairs:018522_2270 & 019010_2270
033963_2230 & _2230 HiRISE stereo pairs: 033805_2285 & _2285 1 2 3 3 craters have double crater morphology and nearby (within 15 km) SHARAD subsurface reflectors. Floor Terrace Depth (m) 42.8 56.3 41.8 Dielectric Constant Using Weighted Mean Within 15 km of Crater 2.63 2.70 2.73 Dielectric Constant Using Closest Radar Measurement 3.35 3.49 3.57 Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

9 Graduate Research Fellowship Program under Grant No. DGE-1143953.
Conclusions Terraced craters and radar data are consistent with a decameters thick layer of pure, excess water ice Mixtures of porous ice covered with regolith are also consistent Other work (Viola et al. 2014, In Press) show this ice has likely been around for 10s Myr Future work: conditions to keep ice stable Acknowledgements - SeisWare International Inc. for free license of SeisWare software used in analyzing SHARAD data - CO-SHARPS for SHARAD radar data products - Charles Brothers & Jack Holt for SHARAD clutter simulations This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

10 Backup Slides Ali M. Bramson (bramson@lpl.arizona.edu)
…Constraints on Subsurface Ice in Arcadia Planitia, Mars

11 3-Component Dielectric Mixing Models
εmix1/γ = νrockεrock1/γ + νiceεice1/γ + νairεair1/γ Best-fit power-law exponent for sand-ice mixtures: γ = 2.7 (Stillman et al., 2010) Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

12 3-Component Dielectric Mixing Models
Preliminary range (including errors) is ~2.2 to 4 Consistent with bulk composition of relatively pure water ice Consistent with geomorphic evidence Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

13 Radargram Clutter Simulation SHARAD Radar delay time
Radar Track distance along track Clutter Simulation Ali M. Bramson …Constraints on Subsurface Ice in Arcadia Planitia, Mars

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