Jarmo Korteniemi

Arctic Planetary Science Institute

We show the Dao Vallis floor to consist of many units with distinct ages, e.g., patches of original canyon floor, and viscous flows resurfaced in the last few Ma.

Floor-fractured craters appear to occur on all the cratered terrestrial planets. Their floors are typically raised as a whole, or they are cut into large elevated blocks. The floors exhibit radial, concentric and/or polygonal fractures, occasionally mixed with volcanic features. The craters occur almost always next to large regional volcanic provin...

The eastern Hellas basin rim has been highly modified by a multitude of both volcanic and fluvial processes. It is covered by a large part of the Circum-Hellas Volcanic Province, consisting of the volcanic plains of Hesperia Planum and western Promethei Terra, as well as the two central volcanoes Hadriaca and Tyrrhena Patera and their associated la...

Journal: Geologi. Note: This article is in Finnish, but it contains an English summary. The work’s title is ’On the verge of a new kind of geophysics: Part 4 – Geoscientific and archaeological applications of muon imaging.' Tämä artikkeli on myonigrafaa eli myonikuvausta käsittelevän kirjoitussarjamme neljäs osa. Sarjan tarkoitus on tehdä tätä uutt...

A transition towards sustainable energy sources requires the exploration and development of minerals critical to electronics and energy storage and delivery systems. Funded under Horizon Europe (Grant Agreement N°101058178), the AGEMERA project is a three-year initiative addressing critical raw materials (CRMs), including their exploration and extr...

Robotic and manned exploration of the Moon is the next target in Solar System exploration. The availability of in situ resources such as water ice, iron oxides, helium-3, and rare earth elements, combined with permanently sunlit areas, provides the opportunity for the first settlement, either human or robotic, on the Moon. We used several selection...

Tunnelling and underground mining face many risks threatening underground operations. Such hazards include sudden incidents of dangerous and violent rock bursts and cave-ins. We propose that stationary muography arrays in underground settings could map potentially risky areas.

Note: This article is in Finnish, but it contains an English summary. The work’s title is ’On the verge of a new kind of geophysics: Part 2 — Muon detection and the basic principles of muography.’ Tämä artikkeli on toinen osa myonikuvausta esittelevien kirjoitustemme sarjassa, jonka tarkoitus on tehdä menetelmä tutuksi geotieteelliselle yhteisölle...

Note: This article is in Finnish, but it contains an English summary. The work’s title is ’On the verge of a new kind of geophysics: Part 1 — Muons and the most common applications of muography.’ Myonigrafia on aineen tiheyden uusi kuvantamismenetelmä. Se perustuu ilmakehässä syntyvien myonien havaitsemiseen, sen jälkeen kun ne ovat kulkeneet kuva...

The supply of European critical raw materials (CRMs) does not currently meet the European demand. This gap is predicted to increase, making Europe even more dependent on outside suppliers. AGEMERA is a project to help tackle this strategic problem by studying CRM sites in Finland, Poland, Spain, the Balkans, and Zambia. We conduct geological studie...

Outflow channel formation on the eastern Hellas rim region is traditionally thought to have been triggered by activity phases of the nearby volcanoes Hadriacus and Tyrrhenus Montes: As a result of volcanic heating subsurface volatiles were mobilized. It is however under debate, whether eastern Hellas volcanism was in fact more extensive, and if the...

DefinitionStraight-to-sinuous ridge composed of sand/gravel, deposited in a confined glacial meltwater drainage channel.CategoryA type of straight-to-sinuous ridge (Linear ridge types (various origins)).Proposed origin of some of the inverted channels and sinuous ridges on Mars.DescriptionWinding, steep sided, narrow, sharp- to broad-crested ridges...

DefinitionSteep-walled depressions on the floors of craters.SynonymsIrregular depression craterDescriptionMars: depressions on the floor units of impact craters (Fig. 1). Depression walls often have straight segments and exhibit layering. The parent craters tend to be shallower than the surrounding (i.e., nondepressed) craters (Korteniemi et al. 20...

DefinitionA magmatic vertical sheet intrusion that has penetrated into a preexisting body of rock.SynonymsMagmatic dike. Alternative spelling: dyke; Vertical intrusionDescriptionA solidified near-vertical subsurface magma body that penetrates through one or more layers of preexisting rock bodies or layers (regardless of rock type). The thickness of...

DefinitionAny surface along which material cohesion is lost. The term is commonly used for discontinuities of any kind, both tectonic and non-tectonic. The term fracture is also selectively applied to the smallest of tectonic displacement types, e.g., smaller than a fissure or a graben on Venus, or smaller than a ridge or a band on Europa, or as a...

DefinitionIntracrater occurrence of chaotic terrain; a crater interior morphology.SynonymsChaotic floor crater (CF); Collapsed crater (CC, Rodriguez et al. 2005).A type of modified craterA type of chaotic terrain (Mars)DescriptionKnobs and irregular mesas that occur in groups or as isolated features (van Kan Parker et al. 2010) inside martian crate...

DefinitionStreamlined hill, typically ovoid to elongate, in previously ice sheet/glacier affected terrains.A type of subglacial streamlined hill.DescriptionA streamlined hill that occurs mostly in glacial sediments (Menzies 1979; Clark et al. 2009; Shaw 2002; Stokes et al. 2011). They are ubiquitous on the now-exposed beds of former ice sheets, whe...

We describe several constructs in the Dao-Niger Valles system in the Hellas region of Mars. Based on morphology we interpret them as probable volcanic edifices.

This paper presents morphometric parameters of Martian layered sequences of different origin that outcrop in the scarps and crater walls, which form natural geologic profiles. The objective of this study was to develop quantitative criteria that would allow distinguishing layers of volcanic and, presumably, sedimentary origin. As a result of measur...

DefinitionA crater exhibiting a system of floor fractures (rilles/crevasses/troughs/moats) and in some cases uplifted crater floor.CategoryA type of impact crater floor modification.May be Chaotic crater floor (Mars).SynonymsCracked floor crater; Cracks or fissures on crater floor; Crevassed crater (Sato et al. 2007); Crevassed floor crater; Floor-...

We performed a systematic survey of typical surface patterns and small (5–50 m) impact craters in a zone between 50° and 70° latitude in the Northern Lowlands of Mars. We found that small-scale (<10 m) polygonal pattern formed by narrow fractures is typical in the northern half of the studied zone. We interpret this pattern to be formed by active t...

Regional tectonic time span extends from 4-Ga-old highland to <3-Ga-old hanging wall faults and to Claritas Rupes activity 2.5 Ga ago.

Due to the availability of the new high resolution images obtained by the CTX and HiRISE cameras onboard MRO, the crater size-frequency distributions have been extended to smaller craters, providing new insights into the erosional and depositional histories of the surfaces. In this work, we compare our preliminary results of age determinations base...

Preliminary results of CTX/HiRISE scale geologic mapping and age estimates on the various floor units of Dao Vallis head, Mars. We have identified a complex and distinct feature set from an area previously considered as a single unit.

Layers exposed in volcanic and sedimentary key sites were used as a foundation for morphologic and morphometric identification criteria. Criteria were used for several test sites and results compared to determine the origin of the observed layering.

Boulders on patterned ground terrain on Mars tend to cluster in cracks (Fig. 1). The precise mechanism for boulder clustering remains unknown but various hypotheses have been proposed. These processes are based on our understanding of patterned ground on Earth but Mars presents a unique situation. We propose the following model (pictured in Figure...

We examine a narrow latitudinal band (60°N–70°N) on Mars to place constraints on the seasonally averaged velocity Q of boulder movements over patterned ground. These latitudes comprise a region of the northern lowlands where patterned ground covers nearly every surface. Here boulders meters in diameter are consistently found to be concentrated at o...

Existence of glacial-like formations on the southern mid-latitude highland of Claritas Fossae is postulated and will be presented with details.

The study is a detailed look on one of the several fluvial systems located on the eastern rim region of the Hellas basin on Mars. We analyzed the morphologic and morphometric characteristics of an extensive channel system, which extends for over 650km from 35.8°S, 106.4°E in Hesperia Planum to Reull Vallis at 39.5°S, 98.1°E, and has a drainage area...

We conduct a detailed survey of the northern polygonal terrain margin (latitude band 50°-70°N), identify terrain types, describe their association with distinct crater populations, and show geological evidence of orbital element driven climate changes.

Impact crater formation is sometimes affected by preexisting target inhomogeneities like faults or joint sets in ways that cause the plan view of the crater to deviate from the idealized circular shape. The resulting polygonal impact craters have been known to exist on the Moon for over a century, and they have been subsequently identified on all t...

Four prominent fluvial systems, Dao, Niger, and Harmakhis Valles, and a system of smaller channels between Niger and Harmakhis Valles characterize a wide topographic trough that connects Hesperia Planum and Hellas Planitia (Hesperia–Hellas trough, HHT). The source depressions of the canyons of Dao and Harmakhis Valles are at the lowermost level (ab...

Geologic evolution of the western portion of Promethei Terra (40–50°S, 90–105°E) consists of two major episodes. The first was the formation of a late Noachian–early Hesperian volcanic province. During this episode a kilometer-thick suite (≈0.3 × 106 km3) of lavas accumulated to the south of Reull and Harmakhis Valles within a regional depression t...

We outline criteria to determine mission options and identify four example lunar landing sites that explore the flux and evolution of lunar volcanism with the goal of understanding the thermal and chemical development of the Moon.

The deposition of ice-bearing materials at different levels during the growth of the lava plateau in Hesperia-Hellas Trough offers a better explanation to the key features of the Valles structures.

Basalts spanning the duration of lunar mare volcanism are incompletely sampled. Presented here is a brief summary of the current knowledge of mare basalt ages and a set of exploration targets where the youngest and oldest mare basalts may be found.

In a crater on Noachis Terra there are domes within a narrow crater floor unit. The unit is connected to a channel that breaches the crater rim. In this study we discuss of a possible pingo-like characteristics of the domes.

The first results of a systematic photogeological study to look at the characteristic morphology of the layers formed by volcanic processes (especially emplacement of lava flows) and due to deposition and sedimentation on Mars.

We use ArcGIS to provide detailed global maps of compositional information combined with stratigraphic and volcanic features that will assist mission planners in locating sites with unsampled volcanic products.

We map out potential landing sites on the Harbinger region (25.71°N, 44.47°W) for future missions. Most open lunar science questions can be addressed there, particularly ones concerning volcanism, internal activity, dating and impact processes.

A survey of floor-fractured craters on the Moon from global data. They are locations where a multitude of volcanic deposits can be sampled, and they should thus be taken into account when considering landing sites for future missions.

This work studies small Martian high latitude impact craters. We focus on the northern polygonal terrain margin, identify and describe crater populations there, associate them with surface texture differences, and show geological evidence of climate changes driven by orbital elements.

In our study we have analyzed 1) the head regions of the Hellas region outflow channels and related structures, and 2) the morphologic and morphometric characteristics of one of the channel systems within the Hellas rim region. We have found that ice-deposits are important as primary sources (both sub-and on-surface) for the different scale systems...

Examples of structures which may be (mis)interpreted as magmatic dikes or their surface manifestations.

The eastern Hellas Basin rim region displays evidence for continued fluvial and glacial activity from Noachian-early Hesperian to Amazonian. The observations and analysis of the region suggest a complex and multitemporal fluvial activity.

We present evidence for extensive dike systems on the Hadriaca Patera volcano on the east Hellas rim and in the volcanic plains south of it, near the outflow channels, and hypothesise on what controls their distribution and orientation.

This study focuses on one of the several fluvial systems located on the eastern rim region of the Hellas basin, Mars. We have analyzed the morphologic and morphometric characteristics of this extensive, over 650km long channel system. Beginning from Hesperia Planum, it intersects several basins and exhibits a multitude of flow morphologies. Eventua...

Impact craters are not always circular; sometimes their rims are composed of several straight segments. Such polygonal impact craters (PICs) are controlled by pre‐existing target structures, mainly faults or other similar planes of weakness. In the Argyre region, Mars, PICs comprise ˜ 17% of the total impact crater population (>7 km in diameter), a...

Polygonal impact craters (PICs) can be used to decipher tectonics of a cratered surface (1-4). Studies of PICs on Mars and Venus (5-7) have provided information of their importance in revealing ancient structures. Some observations are not fully explained with the current ideas. Thus, new ideas for the PIC formation type and preferred PIC size are...

Abstract The Hadriaca Patera (HP) volcano [e.g. 1-9] on Mars is situated on the north-easten rim of the giant Hellas impact basin, and on the western edge of the vast volcanic plains of Hesperia Planum [10, 11]. The eastern Hellas rim region harbours also other, possibly separate centers of volcanism that have only recently been proposed [12, 13]....

Polygonal impact craters may form by thrusting along pre-existing fault planes. They are preferentially formed in the size range of small to mid-sized complex craters, and may perhaps indicate the presence of basin-induced conjugate shear fractures.

The analysis of topographic and morphologic characteristics of the head areas of Hellas valles formations gives implications for relative timing of the formation of the sources of the channels, and also for the volcanic episodes within the region.

We search for dike-indicative formations in the region around Hadriaca Patera. So far, we have identified and documented a large number of straight/curvilinear ridges, fractures and grabens on the volcano as well as in its vicinity.

Valley, channel, sapping, alcove, spring, fault and fold structures allow us to find traces of hydrologic history in relation to episodic tectonics and water re-distribution on Mars. Five different water-related phases were identified.

The western Promethei Terra region (36-50°S, 90-106°E) studied is roughly ~700 km across. It occupies a unique area on the smoothened eastern Hellas basin rim, and consists of two parts: a gentler (~0.07°, eastward of ~97°E) and a steeper (~0.88°, W of ~97°E) regional slope. The Noachian cratered terrain surrounds the region in the NE, E, and S. Th...

These mesas show evidence of intense degradation/erosion. They are the source of several fluvial channels, which have been active during a long period of time. We interpret the mesas as possible remnants of an ancient larger glacier-like structure.

Analysis of three martian paleolakes and connecting channels in Promethei Terra.

We present a preliminary view of the possible evolution of the smooth plains region near Promethei Terra, and characterize the features found within the region.

The last major geological episode of the study region (35°-45°S, 90°-110°E) was a period of late resurfacing. Localised channels (with no apparent sources), possible lag deposits, and esker-like features imply that one possibility for this was a glacier.

The focus of the study is a highly modified crater in Arabia Terra, Mars. It has undergone complex post-formation evolution and there is multitude of evidence of water-related processes.

The slope between Reull-Teviot Vallis and Hellas basin has a set of unique flat-topped E-W elongated mesas with scalloped flanks. They show evidence of long-lasting intense erosion, indicating that they are remnants of a large regional massif.

Impact craters with fractured floors are a feature found on many terrestrial planets. On the Moon they typically occur in near-mare craters, and are thought to be caused by laccolith etc. intrusions ascending and progressing through the under-crater fracture systems [e.g. Schultz, 1976]. The floor-fractured craters on Mars exhibit a wide range of t...

The channel out of the Claritas paleolake led out water and deposited particles. Dust was washed away, particles were sorted and re-oriented. The alluvial fan can be identified by four-channel HRSC classification.

According to the preliminary study, Noachis Terra has been modified by several processes, which have characterized the unforeseeably varied geological history of the region.

On Mars craters with floor fractured and/or irregular depressions are linked to specific locations near the dichotomy boundary and giant impact basins. They provide information on the subsurface processes.

This HRSC study discusses the characteristics of an enigmatic ~25 km crater, located at 36.0N°, 351.8E°, in Arabia Terra. It is either of volcanic or impact origin.

This study discusses the characteristics of an enigmatic ˜25 km crater. It is located at 36,0No /351,8Eo , in Arabia Terra on the highland side of the dichotomy boundary. It has a slightly elliptical shape and it exhibits almost no raised rim and no traceable ejecta field. Earlier mappings show that the region is of Noachian age. We use a multitude...

1] Tyrrhena Terra, located just north of the roughly 2000 km Hellas impact basin, is a typical region of the ancient cratered southern highlands on Mars. Its base material is a mixture of Hellas ejecta, prebasin remnants, and highland terrain, all later saturated with smaller (<200 km) impact craters. Fluvial and lacustrine deposits, erosion, tecto...

1] The High Resolution Stereo Color camera (HRSC) data over Hesperia Planum and its surroundings reveal important details of geologic episodes and water-related processes in this region. (1) The Noachian fluvial events of Hesperia Planum depression included accumulation of water and formation of a water/ice reservoir there. Later, the reservoir was...

The studied area is located in the central part of the Noachis Terra (36-46S and 20-30E), which is located on the southern highlands of Mars, to the west of Hellas basin. We have studied the area using the freshest data sets - Themis and MOC - to clear out what input they can give to the geological analysis of this highland region. The first observ...

Two craters in Terra Tyrrhena north of Hellas basin exhibit anomalous floors. Here we present the geological history of the area.

This study concentrates on mapping and describing the paleolakes on Hellas Basin region using the Mars Express HRSC- images. The camera has imaged the area with enough good coverage to to give preliminary view of paleolake distribution there.

The Mars Express HRSC data were used to study fluvial history of southern Claritas on Mars. Volatiles, transported downslope to the basin, breached through a saddle valley and formed a channel towards Icaria Planum in the west. Along the channel, sapping provided additional water. The channel broke into a 30-km impact crater and formed a temporary...

Water was transported from the southern Claritas Fossae upland peaks into the Claritas basin. The channel from the paleolake into Icaria Planum displays also sapping, crater lake with delta, and alluvial fan.