Janus Kozdon, C.S. Edwards Physics and Astronomy Department,

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Presentation transcript:

Determination of Potential Localized Dust Sources and Sinks in Elysium Planitia, Mars Janus Kozdon, C.S. Edwards Physics and Astronomy Department, Northern Arizona University

Thermal Emission Spectrometer (TES) Introduction; Thermal Emission Spectrometer (TES) Surface differences are observed Due to the dust cycle Increase = more dust Decrease = less dust

Mars Climate Sounder (MCS) Introduction Mars Climate Sounder (MCS) Temperature Changes Higher = less dust Lower = more dust Fig 2. Global maps of Mars nighttime temperature from MCS data between MY 30 and 31. Temperature differences from the median 3AM temperatures are shown.

Does dust have an Effect? 0.01cm thick of dust can cause ~1-2K difference It does have a considerable effect Temperature differences can be correlated to differential dust thicknesses Fig 3. (top) Plot illustrating the effects of homogeneous dust (50TI) layers over a uniform Mars surface (200TI) over the course of a Mars year. Fig 4. (bottom) Plot illustrating the effect of homogeneous dust (50TI) layers over a uniform Mars surface (200TI) over the course of a Mars day

Mars Orbiter Laser Altimeter (MOLA) Geologic context Mars Orbiter Laser Altimeter (MOLA) https://marsoweb.nas.nasa.gov/globalData/images/thumbnails/MOLA_cylin.jpg

THEMIS Standard Processing Methods THEMIS Standard Processing Undrift Dewobble Rtilt Deplaid Destreak Temperature Conversion

Methods Co-Registering Images are given the same background reference frame for comparison accuracy

Methods Normalization Same average Same standard deviation Image 1 MY= 30 Ls= 85.7 Local time= 16.6 hr min: 192.0 max: 251.0 avg: 222.9 stddev: 5.17 sum: 197537508.1 Image 2 MY= 26 Ls= 95.9 Local time= 16.1 hr min: 194.1 max: 247.3 avg: 222.9 stddev: 5.17 sum: 197537508.1

Results Image1 - Image2 = Difference Image This is strictly what changed in the timeframe between images Difference Image min: -14.2 max: 12.4 avg: 2.21e-09 stddev: 1.14 sum: 0.001907348633

Results Image1 - Image2 = Difference Image This is strictly what changed in the timeframe between images -3.511123657 K Difference Image min: -14.2 max: 12.4 avg: 2.21e-09 stddev: 1.14 sum: 0.001907348633

Going Forward Temperature differences to dust thicknesses conversions Continual analysis over the same area of interest will help determine the location’s contribution to the dust cycle Temperature vs. Time plots Pair analysis for global coverage

Image Pairs Overlapping sections of THEMIS daytime (top) and nighttime (bottom) image pairs acquired within 1 hour local time and 20˚Ls of one another. Furthermore they have have a minimum of 100km2 overlap. Images acquired the same MY were eliminated.

acknowledgements The Northern Arizona University Hooper Undergraduate Research Award The Northern Arizona University NASA Space Grant program The NASA Mars Data Analysis Program Szwast, M. A., M. I. Richardson, and A. R. Vasavada (2006), Journal of Geophysical Research, 111(E11).