Entity

Time filter

Source Type

Budapest, Hungary

Kereszturi A.,Konkoly Astronomical Institute | Ormandi Sz.,Eotvos Lorand University | Jozsa S.,Eotvos Lorand University
Planetary and Space Science | Year: 2015

CV and CK chondrites might came from the same parent body from different depth values. To better constrain the conditions there, the composition, structure and chronology of mineral changes were analyzed in NWA 1465 CV3 chondrite meteorite. This sample represents an interesting part of the proposed ancient parent body where opposite to the generally poor altered state of CV3 chondrites, strong mechanical deformation produced elongated chondrules. All of the ingredients in the sample were flattened and fractured. After the chondrules settled down glass formation, opaque crystallization, fracturing and a second opaque generation followed by carbonate crystallization happened. The lack of fragments along the veins suggests no shearing movement happened, and the small number of weak shock signatures points to S2 level, and the oriented pressure in the parent body might come from burial induced pressure. The meteorite might came from a location in the CV-CK parent body where melting, and weak impact related fracturing and vein filling happened. In this an environment alteration of the primitive material started, possibly from a zone transitional between the shallow, less processed CV, and the deeper, more processed CK chondrites. © 2015 Elsevier Ltd. All rights reserved. Source


Orgel C.,Eotvos Lorand University | Kereszturi A.,Konkoly Astronomical Institute | Vaczi T.,Eotvos Lorand University | Groemer G.,Austrian Space Forum | And 2 more authors.
Acta Astronautica | Year: 2014

Between 15 and 25 April 2011 in the framework of the PolAres programme of the Austrian Space Forum, a five-day field test of the Aouda.X spacesuit simulator was conducted at the Rio Tinto Mars-analogue site in southern Spain. The field crew was supported by a full-scale Mission Control Center (MCC) in Innsbruck, Austria. The field telemetry data were relayed to the MCC, enabling a Remote Science Support (RSS) team to study field data in near-real-time and adjust the flight planning in a flexible manner. We report on the experiences in the field of robotics, geophysics (Ground Penetrating Radar) and geology as well as life sciences in a simulated spaceflight operational environment. Extravehicular Activity (EVA) maps had been prepared using Google Earth and aerial images. The Rio Tinto mining area offers an excellent location for Mars analogue simulations. It is recognised as a terrestrial Mars analogue site because of the presence of jarosite and related sulphates, which have been identified by the NASA Mars Exploration Rover "Opportunity" in the El Capitan region of Meridiani Planum on Mars. The acidic, high ferric-sulphate content water of Rio Tinto is also considered as a possible analogue in astrobiology regarding the analysis of ferric sulphate related biochemical pathways and produced biomarkers. During our Mars simulation, 18 different types of soil and rock samples were collected by the spacesuit tester. The Raman results confirm the presence of minerals expected, such as jarosite, different Fe oxides and oxi-hydroxides, pyrite and complex Mg and Ca sulphates. Eight science experiments were conducted in the field. In this contribution first we list the important findings during the management and realisation of tests, and also a first summary of the scientific results. Based on these experiences suggestions for future analogue work are also summarised. We finish with recommendations for future field missions, including the preparation of the experiments, communication and data transfer - as an aid to the planning of future simulations. © 2013 IAA. Source


Orgel C.,Eotvos Lorand University | Kereszturi A.,Konkoly Astronomical Institute | Vaczi T.,Eotvos Lorand University | Sattler B.,University of Innsbruck
Proceedings of the International Astronautical Congress, IAC | Year: 2012

Between 15 - 25 April 2011 the framework of the PolAres program of the Austrian Space Forum, a five-day field test of the Aouda.X spacesuit simulator was conducted at the Rio Tinto Mars-analogue site in southern Spain. The field crew was supported by a full-scale Mission Control Center (MCC) in Innsbruck, Austria. The field telemetry data were channelled to the MCC to enable a Remote Science Support (RSS) team to study field data in near-real-time and adjust the flight planning in a flexible manner. We report on experiments in the field of robotics, geophysics (Ground Penetrating Radar) and geology (Raman spectroscopy on the field and in the laboratory, Scaled Observations, rock - And water sampling) as well as life sciences (Yeti: Youth Explores Terra Incognita, Microbial Assessment, Drill for Contamination Vector Experiment) in an operational environment. Extravehicular Activity (EVA) maps had been prepared using Google Earth and aerial images. The Rio Tinto mining area offers an excellent location for Mars analogue simulations. It is recognized as a terrestrial Mars analogue site because of the presence of jarosite and related sulphates, which have been identified by the NASA Mars Exploration Rover "Opportunity" in the El Capitan region of Meridiani Planum on Mars. The acidic, high ferric-sulphate content water of Rio Tinto in the region is also possible analogue in astrobiology regarding the analysis of ferric sulphate related biochemical pathways and produced biomarkers. During our Mars simulation, 18 different types of soil and rock samples were collected inside Rock Garden" and Mineral Flowers" area by the spacesuit tester. The collected samples were transferred to laboratories where Raman spectroscopic investigation and the YETI experiment were done. The Raman results confirm the presence of minerals expected, such as jarosite, different Fe oxides and oxi(hydroxides), pyrite and complex Mg and Ca sulphates. Eight successfully finished activities were conducted in the field. In the contribution first we list the important findings during the management and realization of tests. Secondly, the geology-related results regarding the EVA tracks, Raman spectroscopic studies and the Scaled Observation projects are listed. Thirdly, the main suggestions for future analogue work are summarized. We had to deal with some challenges on the field, which could be improved during a follow-up mission, including the preparation of the experiments, communication and data transfer - Their description would provide useful experiences during the planning of future simulations. Copyright © (2012) by the International Astronautical Federation. Source


Akos K.,Konkoly Astronomical Institute | Akos K.,Eotvos Lorand University | Szivia O.,Eotvos Lorand University | Sandor J.,Eotvos Lorand University | And 2 more authors.
Planetary and Space Science | Year: 2014

Analysing NWA 3118 CV3 chondrite with optical microscopy and electron microprobe methods, mostly intact chondrules were present, and fragmentation happened before the chondrules settled down at their current location. During or after the consolidation metasomatism changed Mg to Fe in olivines around the scale of 100 μm toward the chondrules' interior. Specific elongated dark, often rim-like features with length above 0.3 mm were identified in the matrix. While in most cases these features looked like as a rim around chondrules, at several cases they appeared without chondrules. Their mineral size was very small, and elemental composition did not show obvious difference from that of the matrix, although they have moderately elevated S at some locations. They were mostly composed of olivine, although it is very difficult to determine the exact mineral phase because of the small grain size. They contained elongated, chain-like larger crystals, occasionally arranged along curved arches, suggesting some specific oriented crystal growth and also some small-scale mechanical movement might contribute in their formation. Our observations suggest that some features earlier termed as chondrule rims in CV meteorites might also form without chondrules or not directly around them. Their origin irrespective of chondrules and may represent a knowledge gap in the understanding of processes inside CV parent bodies. © 2014 Elsevier Ltd. All rights reserved. Source


Kereszturi A.,Konkoly Astronomical Institute | Ormandi S.,Eotvos Lorand University | Jozsa S.,Eotvos Lorand University
Meteoritics and Planetary Science | Year: 2015

In analyzing a thin section of the NWA 6604 CK4 meteorite, only altered chondrules and various components that are probably left behind the destruction of former chondrules can be observed. We suggest that melting, grain size decrease, resorption of the original chondrules, and crystallization of opaque minerals were the main processes that destroyed the chondrules. Four different events could be identified as having occurred during this alteration. First, opaques crystallized along former fractures producing chains of separated grains. Later, opaques and Ca-rich minerals crystallized together in veins and large melt pockets; this was the strongest recrystallization phase involving the largest volume of melt. This occurred along different fractures than the first phase above. During the third phase, only Ca-rich plagioclase crystallized along thin veins, and in a fourth phase, fractures formed again, partly along those formed during the second phases but without substantial mineral infill. Two simple possible case models should be considered for this meteorite: alteration by purely impact-driven processes or mainly by melt-driven processes. Although for CK4 chondrites, the shock-produced alteration driven by impact is the more accepted and widespread approach, melting is also compatible with the observed textural characteristics of chondrule destruction. During melting, recrystallization took place producing iron-rich minerals earlier and Ca-Si-rich ones later. The penetration of melts into veins contributed in the chondrule destruction. The stress directions also changed during these alterations, and minerals that formed later filled differently oriented fractures than the earlier ones. From our observations, we favor a view where heat-driven melting and recrystallization produced the destruction and uniform mineralogy in the sample. © The Meteoritical Society, 2015. Source

Discover hidden collaborations