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The article develops an explanation of corporal punishment (CP) as an expression of family violence by developing a multi-level, conciliatory model of human behavior. The synthesis builds upon a review of the relevant analytic approaches and empirical evidence spanning multiple levels of human behavior to include five interrelated frameworks: (1) behavioral investment; (2) socialization; (3) cultural justification; (4) social location; and (5) societal context. The analytic levels highlight the various explanatory principles that address questions relevant mainly to investigators who study behavior in terms of different levels of informational complexity. The paper outlines the most important factors that shape the use and non-use of CP within family settings. The model identifies key ontogenetic and biophysiological factors linked to the fitness of parents' offspring, along with primary socialization processes and cultural justification mechanisms that increase the probability of the intergenerational transmission of violence. In addition, the model identifies the sociological dimensions of family relationships and the importance of social locational variables in shaping parental usage of CP, as well as the importance of communities and institutions as situated within sociocultural contexts. The main conclusion suggests that to understand and explain more fully why human beings use violence in the context of familial relationships—including corporal punishment practices—analysts must consider the different influences and possible impacts of factors across all five levels. [ABSTRACT FROM AUTHOR]

Modern Mars is bipolar, cold, and oxidizing, while early Mars was characterized by icy highlands, episodic warmth and reducing atmosphere. The timing and association of the climate and redox transitions remain inadequately understood. Here we examine the spatiotemporal distribution of the low surface iron abundance in the ancient Martian terrains, revealing that iron abundance decreases with elevation in the older Noachian terrains but with latitude in the younger Noachian terrains. These observations suggest: (a) low-temperature conditions contribute to surface iron depletion, likely facilitated by anoxic leaching through freeze-thaw cycles under a reducing atmosphere, and (b) temperature distribution mode shifted from elevation-dominant to latitude-dominant during the Noachian period. Additionally, we find iron leaching intensity decreases from the Early to Late Noachian epoch, suggesting a gradual atmospheric oxidation coupled with temperature mode transition during the Noachian period. We think atmospheric oxidation led to Mars becoming cold and bipolar in its early history. The study reveals anoxic leaching in ancient Martian terrains occurred during seasonal freeze-thaw cycles. Findings suggest that gradual atmospheric oxidation drove Mars to become cold and bipolar in its early history. [ABSTRACT FROM AUTHOR]

Background: Bicondylar tibial plateau fractures pose many treatment challenges due to their complex fracture patterns and associated soft tissue compromise. We aim to evaluate outcomes of acute ORIF (aORIF) versus staged ORIF (sORIF) of high energy bicondylar tibial plateau fractures. Methods: We retrospectively reviewed 186 patients at two high-volume Level I trauma centers. One hundred one patients underwent aORIF and 85 underwent sORIF between 2011 and 2019. Clinical outcomes of interest included operative time, wound dehiscence, superficial and deep infection, nonunion, flap coverage, arthrodesis, and early conversion to arthroplasty. Results: Patients had a median follow up of 12 months (6–98 months). The sORIF group had a higher ISS (p = 0.02) and a higher rate of open fractures (24.7% vs 11.9%, p = 0.03). The groups were statistically similar in other demographics and co-morbidities. Operative time was significantly shorter in the aORIF group (157 vs 213 min., p < 0.001). There was no statistical difference in wound dehiscence, deep infection, flap coverage, nonunion, unplanned reoperation, or post-traumatic arthritis between groups. However, aORIF was associated with a significantly lower rate of superficial infection (p = 0.01), arthroplasty (p = 0.003) and unplanned reoperation (p = 0.005). Subgroup analysis of only the 41C3 fractures showed a lower rate of superficial infections in the aORIF group (p = 0.04). No difference in complications was found between the fracture subgroups. Conclusion: We found no increased risk of complications with aORIF compared to sORIF for bicondylar tibial plateau fractures. While not all injuries may be appropriate for aORIF, our results demonstrate the safety of aORIF when patients are properly selected by experienced fracture surgeons. Level of evidence: Level III. [ABSTRACT FROM AUTHOR]

Many interpretations have been proposed to explain the presence of jarosite within Martian surficial sediments, including the possibility that it precipitated within paleo-ice deposits owing to englacial weathering of dust. However, until now a similar geochemical process was not observed on Earth nor in other planetary settings. We report a multi-analytical indication of jarosite formation within deep ice. Below 1000 m depth, jarosite crystals adhering on residual silica-rich particles have been identified in the Talos Dome ice core (East Antarctica) and interpreted as products of weathering involving aeolian dust and acidic atmospheric aerosols. The progressive increase of ice metamorphism and re-crystallization with depth, favours the relocation and concentration of dust and the formation of acidic brines in isolated environments, allowing chemical reactions and mineral neo-formation to occur. This is the first described englacial diagenetic mechanism occurring in deep Antarctic ice and supports the ice-weathering model for jarosite formation on Mars, highlighting the geologic importance of paleo ice-related processes on this planet. Additional implications concern the preservation of dust-related signals in deep ice cores with respect to paleoclimatic reconstructions and the englacial history of meteorites from Antarctic blue ice fields. The authors report in-situ formation of jarosite witin the Talos Dome ice core (East Antarctica) and show that this ferric-potassium sulfate mineral is present in ice deeper than 1000 meters and progressively increases with depth. This has implications for the presence and formation mechanisms of jarosite observed on Mars. [ABSTRACT FROM AUTHOR]

Even though the concept of behavior is central to modern psychology, there is no consensus regarding what the term behavior means. The current paper focuses on disentangling two separate conceptions of the term that have added to the confusion. One meaning of the term behavior pertains to natural scientific epistemology, specifically the requirements of empirical methodology and its reliance on data that are measurable and available to public observation. The second meaning pertains to ontology and relates to the fact that at a descriptive level there are different kinds of behavioral patterns in the universe. Put simply, inanimate material objects behave differently from living organisms, which behave differently from animals, which behave differently from people. This paper introduces a "Periodic Table of Behavior" derived from Henriques', Review of General Psychology, 7, 150–182, (2003, 2011) Tree of Knowledge System to map the different kinds of behaviors that are described and examined by different sciences. It concludes by using the formulation to clarify the relationship between the methodological and ontological description of behavior and argues how the basic science of psychology can be effectively defined as the science of mental behavior going forward. [ABSTRACT FROM AUTHOR]

Over 600 chloride-bearing deposits (chlorides) have been identified on the southern highlands of Mars. These chlorides have critical implications for hydrology and astrobiology: they are indicators of an evaporating super saturated solution, and they could have provided habitat environments for halophilic microorganisms and preserved organic matter. One of the prominent geomorphology characteristics of these chloride-bearing regions is the polygonal features within them. The origin of these polygonal features is still in debate. In this study, we have surveyed 153 locations of chlorides using 441 high resolution imaging science experiment (HiRISE) images to characterize the geomorphology of polygonal features. We identified 3 types of polygonal features of distinct geomorphologic characteristics: fractures, raised ridges, and transitional polygons between fractures and raised ridges. We evaluate previously proposed hypotheses of the formation of the polygonal features, and suggest that the 3 types of polygonal features are indicators of different stages of salt crust formation. Salt crust is usually formed through multiple groundwater activities, and it often occurs in playa environment on Earth. The unique hydrological and astrobiological implications of the chlorides with polygonal features make these deposits of high priority for future landed on and/or sample return exploration missions of Mars. [ABSTRACT FROM AUTHOR]

Large Hesperian-aged (~3.7 Ga) layered deposits of sulfate-rich sediments in the equatorial regions of Mars have been suggested to be evidence for ephemeral playa environments. But early Mars may not have been warm enough to support conditions similar to what occurs in arid environments on Earth. Instead cold, icy environments may have been widespread. Under cryogenic conditions sulfate formation might be blocked, since kinetics of silicate weathering are typically strongly retarded at temperatures well below 0 °C. But cryo-concentration of acidic solutions may counteract the slow kinetics. Here we show that cryo-concentrated acidic brines rapidly chemically weather olivine minerals and form sulfate minerals at temperatures as low as -60 °C. These experimental results demonstrate the viability of sulfate formation under current Martian conditions, even in the polar regions. An ice-hosted sedimentation and weathering model may provide a compelling description of the origin of large Hesperian-aged layered sulfate deposits on Mars. [ABSTRACT FROM AUTHOR]

The term 'pure sociology' reflects some of the most important disciplinary concerns that have helped shape the intellectual development of sociology in the United States, particularly in the effort to establish disciplinary boundaries and achieve academic legitimacy. To flesh out the thesis, the current paper recounts briefly the early discussions associated with pure sociology before examining the various usages in the U.S. since the establishment of the discipline. While selected classical theorists employed the concept in framing their discussions, pure sociology represents a distinctively American idiom. The etymological history coincides with the institutionalization of sociology in U.S. universities, while informing key debates about the nature of sociological analysis throughout the past 120 years. Drawing upon an electronic search of multiple databases, a content analysis highlights the prevalence of the different meanings that mainly U.S. social scientists have attached to the concept. The paper then traces the varying trajectories of the many different usages over time, concluding with a discussion of the ascendance of Donald Black's theoretical paradigm that has appropriated the term with considerable success. [ABSTRACT FROM AUTHOR]

Several irregularly shaped craters located within Arabia Terra, Mars, represent a new type of highland volcanic construct and together constitute a previously unrecognized Martian igneous province. Similar to terrestrial supervolcanoes, these low-relief paterae possess a range of geomorphic features related to structural collapse, effusive volcanism and explosive eruptions. Extruded lavas contributed to the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulphur and erupted fine-grained pyroclastics from these calderas probably fed the formation of altered, layered sedimentary rocks and fretted terrain found throughout the equatorial region. The discovery of a new type of volcanic construct in the Arabia volcanic province fundamentally changes the picture of ancient volcanism and climate evolution on Mars. Other eroded topographic basins in the ancient Martian highlands that have been dismissed as degraded impact craters should be reconsidered as possible volcanic constructs formed in an early phase of widespread, disseminated magmatism on Mars. [ABSTRACT FROM AUTHOR]

Sulfate-dominated sedimentary deposits are widespread on the surface of Mars, which contrasts with the rarity of carbonate deposits, and indicates surface waters with chemical features drastically different from those on Earth. While the Earth's surface chemistry and climate are intimately tied to the carbon cycle, it is the sulfur cycle that most strongly influences the Martian geosystems. The presence of sulfate minerals observed from orbit and in-situ via surface exploration within sedimentary rocks and unconsolidated regolith traces a history of post-Noachian aqueous processes mediated by sulfur. These materials likely formed in water-limited aqueous conditions compared to environments indicated by clay minerals and localized carbonates that formed in surface and subsurface settings on early Mars. Constraining the timing of sulfur delivery to the Martian exosphere, as well as volcanogenic HO is therefore central, as it combines with volcanogenic sulfur to produce acidic fluids and ice. Here, we reassess and review the Martian geochemical reservoirs of sulfur from the innermost core, to the mantle, crust, and surficial sediments. The recognized occurrences and the mineralogical features of sedimentary sulfate deposits are synthesized and summarized. Existing models of formation of sedimentary sulfate are discussed and related to weathering processes and chemical conditions of surface waters. We also review existing models of sulfur content in the Martian mantle and analyze how volcanic activities may have transferred igneous sulfur into the exosphere and evaluate the mass transfers and speciation relationships between volcanic sulfur and sedimentary sulfates. The sedimentary clay-sulfate succession can be reconciled with a continuous volcanic eruption rate throughout the Noachian-Hesperian, but a process occurring around the mid-Noachian must have profoundly changed the composition of volcanic degassing. A hypothetical increase in the oxidation state or in water content of Martian lavas or a decrease in atmospheric pressure is necessary to account for such a change in composition of volcanic gases. This would allow the pre mid-Noachian volcanic gases to be dominated by water and carbon-species but late Noachian and Hesperian volcanic gases to be sulfur-rich and characterized by high SO content. Interruption of early dynamo and impact ejection of the atmosphere may have decreased the atmospheric pressure during the early Noachian whereas it remains unclear how the redox state or water content of lavas could have changed. Nevertheless, volcanic emission of SO rich gases since the late Noachian can explain many features of Martian sulfate-rich regolith, including the mass of sulfate and the particular chemical features (i.e. acidity) of surface waters accompanying these deposits. How SO impacted on Mars's climate, with possible short time scale global warming and long time scale cooling effects, remains controversial. However, the ancient wet and warm era on Mars seems incompatible with elevated atmospheric sulfur dioxide because conditions favorable to volcanic SO degassing were most likely not in place at this time. [ABSTRACT FROM AUTHOR]

Ongoing research on martian meteorites and a new set of observations of carbonate minerals provided by an unprecedented series of robotic missions to Mars in the past 15 years help define new constraints on the history of martian climate with important crosscutting themes including: the CO budget of Mars, the role of Mg-, Fe-rich fluids on Mars, and the interplay between carbonate formation and acidity. Carbonate minerals have now been identified in a wide range of localities on Mars as well as in several martian meteorites. The martian meteorites contain carbonates in low abundances (<1 vol.%) and with a wide range of chemistries. Carbonates have also been identified by remote sensing instruments on orbiting spacecraft in several surface locations as well as in low concentrations (2-5 wt.%) in the martian dust. The Spirit rover also identified an outcrop with 16 to 34 wt.% carbonate material in the Columbia Hills of Gusev Crater that strongly resembled the composition of carbonate found in martian meteorite ALH 84001. Finally, the Phoenix lander identified concentrations of 3-6 wt.% carbonate in the soils of the northern plains. The carbonates discovered to date do not clearly indicate the past presence of a dense Noachian atmosphere, but instead suggest localized hydrothermal aqueous environments with limited water availability that existed primarily in the early to mid-Noachian followed by low levels of carbonate formation from thin films of transient water from the late Noachian to the present. The prevalence of carbonate along with evidence for active carbonate precipitation suggests that a global acidic chemistry is unlikely and a more complex relationship between acidity and carbonate formation is present. [ABSTRACT FROM AUTHOR]

Clays form on Earth by near-surface weathering, precipitation in water bodies within basins, hydrothermal alteration (volcanic- or impact-induced), diagenesis, metamorphism, and magmatic precipitation. Diverse clay minerals have been detected from orbital investigation of terrains on Mars and are globally distributed, indicating geographically widespread aqueous alteration. Clay assemblages within deep stratigraphic units in the Martian crust include Fe/Mg smectites, chlorites and higher temperature hydrated silicates. Sedimentary clay mineral assemblages include Fe/Mg smectites, kaolinite, and sulfate, carbonate, and chloride salts. Stratigraphic sequences with multiple clay-bearing units have an upper unit with Al-clays and a lower unit with Fe/Mg-clays. The typical restriction of clay minerals to the oldest, Noachian terrains indicates a distinctive set of processes involving water-rock interaction that was prevalent early in Mars history and may have profoundly influenced the evolution of Martian geochemical systems. Current analyses of orbital data have led to the proposition of multiple clay-formation mechanisms, varying in space and time in their relative importance. These include near-surface weathering, formation in ice-dominated near-surface groundwaters, and formation by subsurface hydrothermal fluids. Near-surface, open system formation of clays would lead to fractionation of Mars' crustal reservoir into an altered crustal reservoir and a sedimentary reservoir, potentially involving changes in the composition of Mars' atmosphere. In contrast, formation of clays in the subsurface by either aqueous alteration or magmatic cooling would result in comparatively little geochemical fractionation or interaction of Mars' atmospheric, crustal, and magmatic reservoirs, with the exception of long-term sequestration of water. Formation of clays within ice would have geochemical consequences intermediate between these endmembers. We outline the future analyses of orbital data, in situ measurements acquired within clay-bearing terrains, and analyses of Mars samples that are needed to more fully elucidate the mechanisms of martian clay formation and to determine the consequences for the geochemical evolution of the planet. [ABSTRACT FROM AUTHOR]

This article reports on a multi-method impact evaluation of a therapeutic summer camp program for children and youth with learning disabilities and related psychosocial problems. The study examines the degree to which program objectives were achieved through a pre-camp, post-camp, follow-up design using a series of standardized instruments, camp evaluations, and interviews with parents. The results indicate that the campers reported less social isolation, experienced modest improvements in self-esteem, and expressed high levels of satisfaction with the camp. The measures for social skills generally failed to register significant changes, although parents reported improvements in the areas of cooperation, responsibility, and self-control. [ABSTRACT FROM AUTHOR]

The Eridania region in the southern highlands of Mars once contained a vast inland sea with a volume of water greater than that of all other Martian lakes combined. Here we show that the most ancient materials within Eridania are thick (>400 m), massive (not bedded), mottled deposits containing saponite, talc-saponite, Fe-rich mica (for example, glauconite-nontronite), Fe- and Mg-serpentine, Mg-Fe-Ca-carbonate and probable Fe-sulphide that likely formed in a deep water (500-1,500 m) hydrothermal setting. The Eridania basin occurs within some of the most ancient terrain on Mars where striking evidence for remnant magnetism might suggest an early phase of crustal spreading. The relatively well-preserved seafloor hydrothermal deposits in Eridania are contemporaneous with the earliest evidence for life on Earth in potentially similar environments 3.8 billion years ago, and might provide an invaluable window into the environmental conditions of early Earth. [ABSTRACT FROM AUTHOR]