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This analysis provides a detailed snapshot of the radio news landscape in Hungary, a European-Union-member ‘illiberal state’ in mid-April 2018, a few weeks after the general election. In this study, we wished to quantitatively characterize radio news broadcasts. This is the first study that provides a detailed analysis of contemporary radio news output across all formats, target audiences, owners and regions in Hungary. The study uses several quantitative and geographic indicators that include objective elements such as news ecosystem diversity, local news production, news about local issues, sound bites, credited political press, news sections and more subjective news framing and a framing-based bias indicator. Our results show that the ideological diversity of radio news was far the highest in the Budapest region. MTVA, the state media provider had significantly more politically biased news than other stations. Local radios never criticized local public affairs. A few stations in Budapest did broadcast balanced, pro-opposition and critical news, but they were in minority over pro-government news items that dominated the rural media landscape with significantly less choice.

The Navua Valles are comprised of a system of channels and valleys on the inner Northeastern rim of Hellas Basin, which is a 1500-km-long sloping terrain. Drainage systems and regional geology in this unique setting were not previously mapped in detail. We mapped this region using CTX (6 m/px) as the base map and assessed surface unit ages resulting from our crater counting. We found that the timing of the deposit-forming episodes in this region during the Hesperian and Early to Middle Amazonian largely correlated to active phases of the Hadriacus Mons volcanic center. We found evidence for several episodes of fluvial activity Hesperian to the Amazonian with declining intensity, and transitioning to ice-dominated processes. The channels in the Navua Valles region erode into deposits dating from the Noachian to Early Amazonian, including the Noachian highlands, Noachian to early Amazonian crater ejecta, and likely volcanic plains formed from the Hesperian to the Hesperian–Amazonian transition. Channels directly originating from Hadriacus Mons are younger, while precipitation-fed channels at larger distance from the volcanic center are older, indicating different triggers for fluvial activity. Crater counting results indicate that almost all channel floors were at least partially resurfaced during the Amazonian and that several channel deposits formed during the last 0.5 Gyr. Water pathways likely included surface channels, lakes, and subsurface flow. The Navua Valles channel system is discontinuous, and the number of terminal deposits (sink locations) is almost as high as the number of channel sources, which is unusual for valley networks elsewhere on Mars. Interior channels formed only in the major Navua channels, they are even more fragmented than their parent channels, but occur along their entire length. Channels and valley systems within the Navua Valles are potential targets for in situ astrobiological studies, as they could have provided potential habitats at least periodically, from the Late Hesperian to the Late Amazonian.

Introduction: In the field of planetary remote sensing, terabytes of data from extraterrestrial planetary bodies are made available to the scientific community today. With the development of new missions, the volume and variety of these data continue to grow. This development has been largely facilitated through developments leading to higher integrated technology allowing to build compact and efficiently performing platforms and instrumentation. A likely other reason might be an increasing international competitive pressure which motivated new developments in sensor technology and mission designs. Along with the increase of raw data volume, the volume of derived research data continues to grow in parallel, albeit at a slower rate. While mission data, i.e. primary research data (PRD), as derived from instruments, are commonly well maintained within archives such as the Planetary Data System (PDS) and Planetary Science Archive (PSA), derived research data, i.e., secondary research data (SRD) might not always share the same fate. For an more user and object-oriented usage of mission data first efforts came up in the last years [1-3]. Scientific studies, resulting in further derived data do not often receive the same attention. In order to accomplish efficient research data management (RDM) for both kind of RD and to provide tools across research domains it is important to develop appropriate and effective structures. In that context, research data infrastructures (RDI) have the primary goal of collecting existing data under uniform guidelines and to make data accessible in defined ways. RDI initiatives supports the establishment of research management practices, including adopted metadata standards, research lifecycle and associated infrastructures. E.g. The European Open Science Cloud (EOSC) as RDI undertaking, "aims to federate existing and future RDI - across disciplines - under a single umbrella, and provides (open) services for the European researcher community." [4] They are targeted to provide faster and more efficient data access in order to pool resources and avoid duplication where redundancy is technically not needed. A large volume of RD that are derived in the field of planetary research carry an explicit spatial component through an absolute reference, or through relative location information, as inherent characteristics, which can thus be described as spatial data and spatial RD. These spatial (research) data serve as fundamental basis for further cartographic products and maps. Maps, as one example of SRD, have been an essential part of planetary research since the beginning of observation and they have been constantly refined and improved since then. Planetary maps range from image maps to topographic reference maps, to geologic and to landing-site maps. Their variety, however, is naturally limited due to the lack of anthropogenic overprint and lithologic diversity. In order to re-integrate these maps into the research-data life cycle [5] and to make them not only available for a sustainable reuse, but also to improve the associated information, further efforts are necessary which are outlined in the following sections. Aims: The overarching goal here is to develop a practical concept, and to address requirements to enable open, transparent and sustainable access to planetary maps as part of the open planetary spatial research data family. Therefore, approved and established environments serve as blueprint for our concept for an Open Planetary Map repository. We here refer to maps as conventional cartographic visualization products which contain a classical map layout composed of the main map contents (the topics), map frame, map grid information related to at least one cartographic reference system, map scale information, map title and map legend, as well as other map-related metadata information [6, 7]. These maps can be provided in different formats on various media. Method and Results: In order to assess the current situation and to find a strategy to close the planetary research-data cycle, we first need to analyze the main elements along its current research path. We here 1. identify how the current situation, including users (actors) and data flows, is constituted and how main processes are characterized. In step 2., additional as well as potentially alternative roles and data paths, respectively, are identified and further developed through user and system requirements. Finally, based on the assessment of the current situation and a requirement analysis, potential solutions are highlighted in step 3. that build upon existing Earth-based Infrastructure developments, especially the INSPIRE framework [8] or demonstrate which additional developments are required. Especially the adaption of spatial research infrastructure developments shows how the planetary community could benefit from an adaption of existing infrastructure environments in order to Summary: The aim of this study is to characterize the relationships between different interest groups (stakeholders) and products as well as processes, and to discuss how processes could potentially be optimized and streamlined in order to re-insert planetary maps (and research information) into a healthy and sustainable research cycle. Developments like this could build a thematic bridge to Earth-based RD repositories [9-11] in order to push the reuse of planetary maps forward. One way of realizing an approach targeted at improving the re-use of research data in the planetary sciences is by merging the existing alternatives and to integrate the structural benefits from the INSPIRE (or any other SDI) domain. The creation of an Open Map Repository as part of a Planetary Research Data Infrastructure is described in detail in [12], in particular with respect to the communication and participation, coordination and the technical implementation. References: [1] Laura, J.R., et al 2017. ISPRS Journal of Geo-Information 6, 181; [2] Laura, J.R. et al 2018. Earth and Space Science 5, doi:10.1029/10702018EA000411; [3] Laura, J.R. and Beyer, R.A., 2021. The Planetary Science Journal 2. doi:10.10663847/PSJ/abcb94; [4] Latif, A. et al, 2019. Data Science Journal 18. doi:10.5334/dsj-2019-017 [5] Corti, L., et al. 2019. Managing and Sharing Research Data: A Guide to Good Practice. SAGE Publishing [6] Robinson, A.H., et al. 1995. Elements of Cartography. 6 ed., Wiley, New York; [7] Hake, G., et al. 2001. Kartographie, de Gruyter; [8] https://inspire.ec.europa.eu/tags/sdi# [9] www.eosc.eu, [10] https://www.earthcube.org/, [11] https://pangaea.de/, [12] Nass, A. et al. 2021, in print) Facilitating Reuse of Planetary Spatial Research Data. PSS

Volcanic channels are common features on the terrestrial planets. They have diverse morphologies including sinuous rilles, channelized flows, and potentially collapsed lava tubes. Many of these channels are a part of a typical igneous assemblage of landforms. In addition, some channels have an ambiguous origin, where a volcanic interpretation explains many of the observed features in some settings. This chapter describes volcanically formed sinuous channels, pitted channels, channelized flows, streamlined forms, platy terrain, and discusses a potential volcanic context for outflow channels and some valley networks on Mars.

Channel morphologies are sinuous, negative-relief linear forms that form by a current of water or lava. They may be fluvial or volcanic in origin. Channels are exclusively volcanic on Venus, volcanic or fluvial on Mars and fluvial on Titan. On Venus and Mars, channels are all paleoforms while on Titan (and Earth) they are actively forming. Channels may be hosted by valleys, that represent the cumulative erosional history of the embedded channel. They may be singular or may form braided pattern separated by streamlined island forms (e.g., Kasei Valles); a channel floor may host interior channels (e.g., Navua Valles), and channels may disappear gradually into flat plains (e.g., Simud Vallis). These are just a few of their characteristics that make their cartographic representation a complex issue.In this work we analyzed and compared the symbology of channel forms in planetary geologic maps. An ongoing work on planetary geologic symbology identified 95 maps containing channel symbols in a total of 154 map (Nass et al. 2017b). Symbology is important for several reasons (Nass et al. 2011, Nass et al. 2017a). Although each map is complete on its own, standardized symbology enables direct comparison between maps. Maps are used for measurements: channel morphometry measurements across different quadrangles become problematic if symbols are used and defined differently.Planetary geologic maps use three classes of symbols for representing channel forms: polygons as geologic units, polygons as surficial units laid over a geologic unit and line symbols for smaller channels. Line symbols often transform to geologic units when they reach a cutoff size for the used map scale. Line symbols do not continue over the unit symbols. This way drainage networks are split into two, incompatible symbol types. The cutoff size is often not reported in the legend that use the vague "narrow channels" designation for the line symbols. Sometimes line symbols are used only for "small distributary channels" or "small valleys".Named channel units may be grouped geographically (e.g., Ares Vallis), by age (e.g., Hesperian channels), by morphology (steep walled channels), process (outflow channels) or as true geologic units (vallis floor sediments). These categories may be even mixed within one map.The line symbols are typically solid blue (cyan) lines. This is in accordance with FGDC standards (FGDC 2006).Different problems arise with drainage databases (Hynek et al. 2010, Alemanno et al. 2018). They typically uniformly trace dendritic valley networks, but they also contain singular and other channel forms, whereas "outflow channels" and lava channels are missing from these databases. The global map of Tanaka et al. (2014) uses two different blue line symbols for "channel axis" (i.e., valley network and some outflow-like channels) and "outflow channels".It is needed to redefine channel form classification in the planetary domain and symbology (from Venus to Mars to Titan) and make it clear for mappers if different symbols should be used for different sizes, origins, and morphologies and how different symbols may be combined in one map.

The Navua Valles are a system of channels and valleys on the inner rim of Hellas Basin. The aim of this mapping study was to determine the geologic history of the Navua Valles region; and the relationships between the basement, flow, and channel units along the northeastern slope of Hellas Basin. We have produced a 1:1 million scale geologic map of the Navua Valles region, utilizing standard USGS geologic mapping procedures, but not within a regular USGS mapping project. We selected the mapping area boundaries specifically to cover the Navua Valles drainage systems. The primary base of this mapping effort was a mosaic of 161 Mars Reconnaissance Orbiter Context Camera images, at approximately 6 m/pixel. This paper is part of a double publication, one paper describing the geology of this area, and this paper presenting the geologic map produced during the investigation.

The Navua Valles are systems of paleodrainages located north of Dao Vallis, which empty into Hellas Planitia, the largest impact basin on Mars. In this study, we mapped and characterized the Navua Valles Region's individual drainage systems, including drainages along the southwestern flank of Hadriacus Mons, and one valley network from the same source as Navua Valles but flowing in the opposite direction. The major drainage systems share morphological characteristics common to both outflow channels and valley networks. The slopes in this region are dissected by two major Navua drainage systems (here Navua A* and B*) and several shorter, sub-parallel valleys formed on the highest gradient (approximately 20 m/km [1.15°]) slopes, at the lowest part of Hellas Basin's rim. The two major drainage systems originate in the highlands, and empty into the basin. Our mapping suggests that water in Navua Valles reached the basin floor in a complicated descent and included several episodes of surface ponding, surface runoff, infiltration, subsurface flow and subsequent outflow. The most prominent channel system, Navua A, forms a repetitive sequence of deep incision into bedrock, followed by a transition into broad channels in erodible materials, and then into unconfined deposits. This successive erosion–transport–deposition sequence continues to repeat along the valley's entire length forming a discontinuous pattern that is consistent with classical fluvial process models. The channels cut into volcanic plains likely emplaced from the formation of Tyrrhenus and Hadriacus Montes. The dendritic source valleys of Navua A originate from the rim of a highland crater while the rest of this subsystem consists of a single, discontinuous channel which is consistent with a single water source zone that likely supplied water for all channels downslope. These drainages may have formed as discontinuous channels, revealing the potential existence of subsurface drainage pathways located within an approximately 1.5 × 10 5 km 2 area. Water transported underground emerged in segments that are either isolated or aligned downslope from each other. We have identified several causes of discontinuities, located the zones of potential ground-water discharge and recharge, and a site of localized precipitation at the headwaters of Navua A.

Results in astrogeologic investigations are rarely communicated towards the general public by maps despite the new advances in planetary spatial informatics and new spatial datasets in high resolution and more complete coverage. Planetary maps are typically produced by astrogeologists for other professionals, and not by cartographers for the general public. We report on an application designed for students, which uses cartography as framework to aid the virtual exploration of other planets and moons, using the concepts of size comparison and travel time calculation. We also describe educational activities that build on geographic knowledge and expand it to planetary surfaces.

The Gazetteer of Planetary Nomenclature (GPN) is maintained by the International Astronomical Union Working Group for Planetary System Nomenclature. It contains the internationally approved forms of place names of planetary and lunar surface features. In the last decades, spacefaring and other nations have started to develop local standardized equivalents of the GPN. This initiated the development of transformation methods and created a need for auxiliary information on the names in the GPN that is not available from the database of the GPN. The creation of ‘localized’ (local language) variants of the GPN in non-Roman scripts is an unavoidable necessity, but is also a cultural need. This paper investigates the localization methods into Chinese, Russian two nations with different scripts, and two that are spacefaring ones. The need for the creation of a localized GPN is related to the local importance of scientific papers published in the local language and the existence of locally developed and operated s...

Cartography is the science, technique, and art of filtering and compiling spatial data into map information and to communicate complex spatial relationships and interdependences by advanced visualization techniques. In this context, Cartography provides the whole environment and necessary analysis toolsets to derive mapping results and produce maps. This chapter gives a description about what planetary cartography is about and how planetary cartographic products are produced, the process from data, via information, to knowledge and understanding, and also discussing the recent technical and conceptual transition from hardcopy end products to interactive, dynamic digital databases.

In this chapter, we review basic concepts, measurements, and methods in mapping topographic and reflectance (image) data of planetary surfaces. This includes the definition of coordinate systems for each body, the identification of the shape of a planetary body, and the establishment of reference systems and reference bodies that are required to produce horizontally and vertically accurate representations of a planetary surface.

Elevation data can characterize geology, from global to local scales. For centuries, however, the only planetary topographic data were those of lunar peaks and craters. In the last few decades, several independent techniques have been developed to extract topographic information from diverse types of planetary datasets, which provide key information for the distinction and geologic interpretation of surface features. In this chapter, we discuss techniques to obtain, reconstruct, and visualize elevation data.

The slopes of northeastern Hellas Basin, Mars exhibit a wide variety of fluvial landforms. In addition to the Dao-Niger-Harmakhis-Reull Valles outflow channels, many smaller channels and valleys cut into this terrain, several of which include discontinuous sections. We have mapped these channels and channel-associated depressions to investigate potential paleolakes from the Navua Valles in the West, through the Hadriacus Mons volcano in the center, to the Ausonia Montes in the East. We have identified three groups of candidate paleolakes at the source regions of major drainages and a fourth paleolake type scattered along the lower reaches of these drainages. Each paleolake group has a distinct character, determined by different formative processes, including precipitation and groundwater for lakes at the channel sources, and fluvially transported water at the lower channel reaches. Only one of these 34 basins had been cataloged previously in paleolake basin databases. Several of these sites are at proximity to the Hadriacus volcanic center, where active dikes during the Hesperian could have produced hydrothermal systems and habitable environments. Deposits within these paleolake depressions and at the termini of channels connected to these candidate paleolakes contain the geological and potentially biological record of these environments.

We mapped the northwestern Tharsis region to the east of Olympus Mons and described three distinct channel-and-island morphologies within three channel groups. Islands include irregular and streamlined islands in both lava flows and fluvial systems and residual islands in collapsed systems. We interpret these channels to have formed by a combination of tectonic, collapse, lava, and fluvial (hydrothermal) processes, which produced fissures, pits, flows, and channels with streamlined islands, respectively. This formation model is consistent with the traditional model of Martian fossae-sourced channel systems, where both lava and water were transported along these same channels, in some cases multiple times forming potential habitats. We also considered a lava flow formation model for the observed features. We determined the approximate age of the channel-forming activity to be Late Amazonian, contemporaneous with other, distinctly lava flow processes in the Tharsis region.

Maps are one of the most important tools for communicating geospatial information between producers and receivers. Geospatial data, tools, contributions in geospatial sciences, and the communication of information and transmission of knowledge are matter of ongoing cartographic research. This applies to all topics and objects located on Earth or on any other body in our Solar System. In planetary science, cartography and mapping have a history dating back to the roots of telescopic space exploration and are now facing new technological and organizational challenges with the rise of new missions, new global initiatives, organizations and opening research markets. The focus of this contribution is to introduce the community to the field of planetary cartography and its historic foundation, to highlight some of the organizations involved and to emphasize challenges that Planetary Cartography has to face today and in the near future.

Reference surfaces, coordinate systems and projections are the prerequisites for the geospatial analysis of planetary surfaces. In the followings we discuss how these parameters are defined and used on different types of planetary bodies, including rocky planets, satellites, irregular bodies and gas giants.

We studied optical microscopic and micro-Raman spectroscopic signatures of shocked olivine from the ALH 77005 Martian meteorite sample. The purpose of this study is to document pressure and temperature-related effects in olivine over the entire sample, which can aid in understanding structural changes due to shock metamorphism and the post-shock thermal annealing processes of lherzolitic Martian meteorites. According to the optical microscope observations, three areas may be discernible in olivine of the ALH 77005 in the vicinity of the melt pocket. The first area is the thermally undisturbed part of a grain, which contains a high density of shock-induced planar microdeformations such as Planar Deformation Features (PDFs) and Planar Fractures (PFs). Compared to the first area, the second area shows less shock-induced microstructures, while the third area is a strongly recrystallized region, but not formed from a melt. A common Raman spectral feature of these olivines is a regular doublet peak cen...

Place-naming processes for the features on other planetary bodies are controlled by the International Astronomical Union's (IAU) Working Group on Planetary Nomenclature. This article examines the development of the nomenclature of the surroundings of the Mars Society's Mars Desert Research Station (MDRS), located in Utah, USA, a simulation facility for future Mars stations. The development of this nomenclature system is also representative of the system of local place names in terrestrial remote research and military stations and may foreshow how names will be “born” in a future permanent Mars or Lunar Base.

Planetary maps are powerful tools for the visualization of the formerly unknown planetary surfaces. The appropriate use of visualization and nomenclature is essential for making planetary maps that can be used by both professionals and the general public. This article describes an international mapping project that has produced several maps of the terrestrial planets and the Moon. The maps were published separately, as educational wall maps, and also appeared together in a world atlas. To select the most effective visual tools and nomenclature, we conducted a map reader perception study at the Eötvös Loránd University, Hungary, which is discussed in detail. The second part of the article describes the current system of planetary nomenclature, highlighting some of its problems, with special attention to its localization for bi- or multilingual planetary maps.

The International Cartographic Association (ICA) Commission on Planetary Cartography was officially established on the basis of the ICA Planetary Cartography Working Group at the ICA Congress in Ottawa in August 1999. Its goal is to develop materials and information intended to aid in the global dissemination of planetary cartographic information. The overall theme of this effort is the harmonization of international planetary cartographic activities. The commission's activities can help especially in those countries not actively involved in ongoing spacecraft missions, bringing together scientists from diverse backgrounds (planetary science, earth science, cartography) who have not interacted previously, along with map and atlas publishers. The Planetary Cartography Database, the Multilingual Planetary Maps, and the Multilingual Glossary can serve as a reliable resource for cartographers who wish to produce and study planetary maps.