
Steinmann VilmosEötvös Loránd University · Department of Physical Geography
Steinmann Vilmos
Master of Science
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22
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Publications
Publications (22)
Identifying surface sites with significant astrobiological potential on Mars requires a comprehensive understanding of past geological processes and conditions there, including the shallow subsurface region. Numerical modelling could distinguish between regions dominated by erosion and those characterized by sediment accumulation in ancient wet env...
A model-based surface fluvial erosion and deposition approach was adapted to Martian conditions to forecast the potential locations for shallow subsurface sampling by the Rosalind Franklin ExoMars rover at Oxia Planum. While remote and on-site images show only the surface visible features, former fluvial-related accumulation sites might be hidden....
There are many hydrological models for normal terrestrial environments based on precipitation related erosion, but few of them work well in arid and hyper-arid conditions. These extreme arid regions can be good Mars analogue sites to test and model the conditions and laws of precipitation fed runoff and produced erosion on the Red Planet and infer...
This work aims to introduce and test various semiquantitative field methods and environmental magnetic measurements to help prepare future planetary missions on Mars. For analog observations, paleosols of loess successions in various stages of soil development were investigated and were used as models to infer environmental change during environmen...
The 31 km diameter and 7.5 km deep de Gerlache crater, located 30 km from the southern pole of the Moon was surveyed. At its bottom a 15 km diameter younger crater can be also found beside many smaller overprinting craters. At moderately sloping terrains a few m high, 100–200 m wide, curving quasi-parallel, km long set of ridges could be identified...
This work presents and tests the classical crater size frequency distribution statistical analysis based age estimation for lunar terrains where optical images are not available, e.g. in permanently shadowed polar craters. A comparison of the optical and topographic data based analysis with the joint evaluation of slope maps of about 1° slope resol...
This work analysis an 81 km long 1.85 km wide fluvial valley on Mars (at 2°55’ South and 111°53’ East) for the first time, located near to the so-called Palos carter and Tinto Vallis, called Tinto-B hereafter. The length of the valley is approximately 81 km, and the average width is ~1.85 km, depth ~250 m. The hypsometric curves were created in 5 d...
This study summarises the potential of rock and enviromagnetic methods, which can help to identify weathered horizons and pedogenic processes in future planetary missions, focusing on methods used on-board future rovers.
Certain terrestrial soils have been already used as potential analogues to Mars on soil-like weathering produced surface layer. P...
Surface erosion happened intensively of Mars in the Noachian, partly from precipitation and/or ice melting. However the exact method of erosion is poorly understood, despite various models are used for the Earth successfully. In this work we present the first test results of an erosion simulation GIS based system for Mars. The testing area is (2°55...
This work analyses a 81 km long 1.85 km wide
fluvial valley on Mars (at 2°55’ South and 111°53’
East) that has not been analysed yet, located near to
the so-called Tinto Vallis [1], called Tinto-B
hereafter. The studied area is near to the Palos Carter
and Tinto Vallis. The crater statistical analysis based
age of the analysed valley (2.9 Ga) corre...
The analysed area is ~81 km long and ~1.85 km wide fluvial valley on Mars, next to the equator (2°55' S and 111°53' E) and next to the main fluvial valley Tinto Vallis. The average depth of the valley is ~250 m. The highest pont is +402 m and the deepest point is-752 m. The flow direction of the analysed valley is from south to north. The Martian f...
Introduction: Analysis of the size frequency distribution of impact craters on atmosphereless bodies support the age estimation of the given surfaces covered by these craters (1]). While previously mainly larger craters above km size were analyzed ([2]; [3]), based on the new images from Lunar Reconnaissance Orbiter ([4]) craters down to 2-4 m size...
Analysing the size-frequency distribution of very small lunar craters (sized below 100 m including ones below 10 m) using LROC images, spatial density and related age estimations were calculated for mare and terra terrains. Altogether 1.55 km² area was surveyed composed of 0.1–0.2 km² units, counting 2784 craters. The maximal areal density was pres...