We report data on the martian meteorite Northwest Africa (NWA) 7034, which shares some petrologic and geochemical characteristics with known martian meteorites of the SNC (i.e., shergottite, nakhlite, and chassignite) group, but also has some unique characteristics that would exclude it from that group. NWA 7034 is a geochemically enriched crustal rock compositionally similar to basalts and average martian crust measured by recent Rover and Orbiter missions. It formed 2.089 ± 0.081 billion years ago, during the early Amazonian epoch in Mars' geologic history. NWA 7034 has an order of magnitude more indigenous water than most SNC meteorites, with up to 6000 parts per million extraterrestrial H(2)O released during stepped heating. It also has bulk oxygen isotope values of Δ(17)O = 0.58 ± 0.05 per mil and a heat-released water oxygen isotope average value of Δ(17)O = 0.330 ± 0.011 per mil, suggesting the existence of multiple oxygen reservoirs on Mars.

The source and nature of carbon on Mars have been a subject of intense speculation. We report the results of confocal Raman imaging spectroscopy on 11 martian meteorites, spanning about 4.2 billion years of martian history. Ten of the meteorites contain abiotic macromolecular carbon (MMC) phases detected in association with small oxide grains included within high-temperature minerals. Polycyclic aromatic hydrocarbons were detected along with MMC phases in Dar al Gani 476. The association of organic carbon within magmatic minerals indicates that martian magmas favored precipitation of reduced carbon species during crystallization. The ubiquitous distribution of abiotic organic carbon in martian igneous rocks is important for understanding the martian carbon cycle and has implications for future missions to detect possible past martian life.

We investigated the equatorial layered deposits (ELDs) of Arabia Terra, Mars, inFirsoff crater and on the adjacent plateau. We produced a detailed geological map that included a survey of the relative stratigraphic relations and crater count dating. We reconstructed the geometry of the layered deposits and inferred some compositional constraints. ELDs drape and onlap the plateau materials of late Noachian age, while they are unconformably covered by early and middle Amazonian units. ELDs show the presence of polyhydrated sulfates. The bulge morphology of the Firsoff crater ELDs appears to be largely depositional. The ELDs on the plateau display a sheet-drape geometry. ELDs show different characteristics between the crater and the plateau occurrences. In the crater they consist of mounds made of breccia sometimes displaying an apical pit laterally grading into a light-toned layered unit disrupted in a meter-scale polygonal pattern. These units are commonly associated with fi ssure ridges suggestive of subsurface sources. We interpret the ELDs inside the craters as spring deposits, originated by fl uid upwelling through the pathways likely provided by the fractures related to the crater formations, and debouching at the surface through the fi ssure ridges and the mounds, leading to evaporite precipitation. On the plateau, ELDs consist of rare mounds, fl atlying deposits, and cross-bedded dune fi elds. We interpret these mounds as possible smaller spring deposits, the fl at-lying deposits as playa deposits, and the cross-bedded dune fi elds as aeolian deposits. Groundwater fl uctuations appear to be the major factor controlling ELD deposition. Wind-related erosionYardangs 100 m B HiRISE PSP_004355_1830_RED Res. 0.25 m/pixel Main wind direction 100 m HiRISE ESP_016776_1810_RED Res. 0.5 m/pixel C 500 m CTX P06_003221_1815_XN_01N009W Res: 5.38 m/pixel Main wind direction Elevated lineament D Rim A B C D Figure 8. Erosional versus depositional morphologies. (A) Example of aeolian erosion with yardangs on equatorial layered deposits (ELDs). (B) ELD irregularly shaped layers. ELDs show rounded edges and lengthen in a direction and with geometries not consistent with formation by aeolian erosion. Main wind direction as inferred by yardang alignment is indicated at the top left. (C) ELD irregularly shaped layers. Some of the layers are characterized by the presence of rims. (D) Northwest-southeast-trending depression. Its regularity and trend do not seem consistent with an erosional formation by wind action. Main wind direction as inferred by yardang alignment is shown at the bottom left. Inside the depression, elevated lineaments (fi ssure ridges?), emphasized by mounds, are present. The location of the images is indicated in the HRSC mosaic at the top right of the fi gure.as

No abstract

No abstract

No abstract

We report on the detection of discrete grains of crystalline graphite and graphite whiskers (GWs) in an Apollo 17 impact melt breccia. Multiple instances of graphite and GWs within a discrete area of the sample imply that these grains are not terrestrial contamination. Both graphite and GWs are indicative of high-temperature conditions and are probably the result of the impact processes responsible for breccia formation. This suggests that impact processes may be an additional formation mechanism for GWs in the solar system and indicates that the Moon contains a record of ancient carbonaceous material delivered at the time of the Late Heavy Bombardment.

The Dallol volcano and its associated hydrothermal field are located in a remote area of the northern Danakil Depression in Ethiopia, a region only recently appraised after decades of inaccessibility due to severe political instability and the absence of infrastructure. The region is notable for hosting environments at the very edge of natural physical-chemical extremities. It is surrounded by a wide, hyperarid salt plain and is one of the hottest (average annual temperature Dallol : 36–38°C) and most acidic natural systems (pH Dallol ≈0) on Earth. Spectacular geomorphologies and mineral deposits produced by supersaturated hydrothermal waters and brines are the result of complex interactions between active and inactive hydrothermal alteration of the bedrock, sulfuric hot springs and pools, fumaroles and geysers, and recrystallization processes driven by hydrothermal waters, degassing, and rapid evaporation. The study of planetary field analog environments plays a crucial role in characterizing the physical and chemical boundaries within which life can exist on Earth and other planets. It is essential for the definition and assessment of the conditions of habitability on other planets, including the possibility for biosignature preservation and in situ testing of technologies for life detection. The Dallol area represents an excellent Mars analog environment given that the active volcanic environment, the associated diffuse hydrothermalism and hydrothermal alteration, and the vast acidic sulfate deposits are reminiscent of past hydrothermal activity on Mars. The work presented in this paper is an overview of the Dallol volcanic area and its hydrothermal field that integrates previous literature with observations and results obtained from field surveys and monitoring coupled with sample characterization. In so doing, we highlight its exceptional potential as a planetary field analog as well as a site for future astrobiological and exploration programs.