Icarus
ISSN: 0019--1035
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This file contains retrievals of column-integrated dust and water ice aerosol optical depth on Mars using infrared images from the THEMIS instrument on-board the Mars Odyssey spacecraft.
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  • Dataset
  • Document
The three figures were uploaded with the submission. All are derived from publicly available full resolution versions of the two HiRISE images described in the text: PSP_002721_2210 and ESP_016801_1300. Figures 1 and 3 have been subsampled from the original resolution in order to show a broader section of the Martian surface than could be done a full resolution. Figure 2 is a full resolution, to show the detail available in the original data.
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Labeled figures derived from original HiRISE images, as described in the text
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See "Fig&Table_collection.docx" for descriptions of each figure and table data. "I_F" means radiance factor. "DOP" means Degree of Polarization. "Spectrum" means reflectance spectrum.
Data Types:
  • Tabular Data
  • Dataset
  • Document
M122353240LC-crop-flip-contrast.png is part of LROC NAC image M122353240LC which has been cropped, flipped in the vertical direction to place north near the top, and contrast-stretched. It has been extended on the western (left) side to create space for part of the mapped data which falls just outside the image. M122353240LC-map-overlay.png is the same image as M122353240LC-crop-flip-contrast.png with an overlay showing dark streaks apparently associated with the Apollo 12 Lunar Module Ascent Stage impact. The streaks were visually identified on a contrast-enhanced version of the image and on versions processed by merging with an image having opposite illumination as described in the text. A small extension of the streak map outside the area of image M122353240LC was added by registering adjacent images to the geometry of M122353240LC, not shown here.
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This image was produced by merging parts of two LROC NAC images, M129431676LC and M122353240RC, which show the linear field of streaks we describe in the paper. The images have approximately opposite illumination (morning and afternoon) so shadows and highlights caused by topography roughly cancel each other and albedo variations are enhanced. The contrast was then greatly enhanced to emphasize the pattern of streaks. The putative impact site is visible at the right edge. North is approximately at the top in this image, which may be compared with Figure 1 for location and orientation. Figure 1C is a crop of a small atrea of this image. The topographic shading does not cancel exactly so craters are still visible, allowing this image to be georeferenced if desired. As presented the image is not georeferenced.
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Climatological fields for the Held-Suarez experiment with a) normal meridioinal temperautre gradient. All_HS.nc b) normal meridional temperature gradient and global uniform stratification. All_HS_S5.nc c) normal meridional temperature gradient under eddy-free setup. All_HS_trm1.nc d) normal meridional temperature gradient with seasonal cycle. annual mean: All_HS_season.nc. DJF: All_DJF_HS_season.nc h) normal meridional temperature gradient with the seasonal cycle under eddy-free setup. DJF: All_DJF_HS_season_trm1.nc e) reversed meridional temperature gradient. All_HotPole_ColdEQ.nc f) reversed meridional temperature gradient and global uniform stratification. All_HotPole_ColdEQ_S5.nc g) reversed meridional temperature gradient under eddy-free setup. All_HotPole_ColdEQ_trm1.nc h) reversed meridional temperature gradient with the seasonal cycle. annual mean: All_HotPole_ColdEQ_season.nc. DJF: All_DJF_HotPole_ColdEQ_season.nc h) reversed meridional temperature gradient with the seasonal cycle under eddy-free setup. DJF: All_DJF_HotPole_ColdEQ_season_trm1.nc Matlab code used to do all the calculations: a) Uprof.m: plotting the U, N2, S vertical profiles in Held Suarez models and the analytical form used in Eady model (Fig. S1) b) drive_hadley.m, drive_hadley_momentumonly.m, drive_hadley_temperatureonly.m: budget analysis to identify the driver of Hadley cells. (Fig. 2, Fig. 8) c) wave_structure_k.m: diagnose baroclinic eddy structure in Held Suarez model (Fig. 5) d) PV_y.m: check baroclinic unstable necessary condition (not shown) Generalized Eady model outputs: a) Normal case fields: eady9d_k7_normTy_output.dat. Normal case growth rate: eady9d_k7_normTy_growthrate.dat b) Reversed case fields: eady9d_k7_revTy_output.dat. Reversed case growth rate: eady9d_k7_revTy_growthrate.dat
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  • Document
Files containing: raw data of near-infrared samples from four areas (El Villar, Calañas, Quebrantahuesos, and Tharsis) in the Iberian Pyrite Belt raw data of thermal analysis of the above samples raw data of a survey of near-infrared spectra from Mars (Leighton Crater, Mawrth Vallis and Nili Fossae)
Data Types:
  • Tabular Data
  • Dataset
Protosolar elemental abundances: A machine-readable spreadsheet corresponding to Table 1 (Wang, Lineweaver, & Ireland, submitted to Icarus on 29 August 2018)
Data Types:
  • Tabular Data
  • Dataset
Kinetic rate constants for amino acids decomposition in water
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  • Dataset
  • Text
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