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Impact cratering is one of the fundamental processes throughout the history of the Solar System. The formation of new impact craters on planetary bodies has been observed with repeat images from orbiting satellites. However, the time gap between images is often large enough to preclude detailed analysis of smaller‐scale features such as secondary impact craters, which are often removed or buried over a short time period. Here we use a seismic event detected on Mars by the NASA InSight mission to investigate secondary cratering at a new impact crater. We strengthen the case that the seismic event that occurred on Sol 1034 (S1034a) is the result of a new impact cratering event. Using the exact timing of this event from InSight, we investigated the resulting new impact crater in orbital image data. The S1034a impact crater is approximately 9 m in diameter but is responsible for over 900 secondary impact events in the form of low albedo spots that are located at distances of up to almost 7 km from the primary crater. We suggest that the low albedo spots formed from relatively low energy ejecta, with individual ejecta block velocities less than 200 m s−1. We estimate that the low albedo spots, the main evidence of secondary impact processes at this new impact event, fade within 200–300 days after formation. Plain Language Summary: On 23 October 2021, the seismometer instrument on the NASA InSight lander detected a seismic event on Mars. The nature of the seismic signal shared characteristics with other events attributed to meteorites impacting the surface of Mars. Reanalysis of images taken by cameras on orbiting spacecraft identified a new impact crater whose location and time of formation matched with the seismic analysis. Our study shows that this 9 m diameter crater has produced over 900 additional, or secondary, impact features up to 7 km away. These secondary features are characterized as being dark spots, often with a tail that points away from the direction of impact, which fade over time. The relatively high number of secondary features from this small impact event is likely due to the low porosity of the rock that was impacted at the surface. We estimate that the dark spots disappear in 200–300 days, thus removing a key set of features used in identifying new impact events on Mars. This timescale places useful limits for future image searches attempting to identify small new impact craters on Mars, and suggests that other such small impact events have been captured in existing data sets and not yet recognized. Key Points: A new 9‐m‐diameter impact crater on Mars identified with in situ seismic and orbital image dataOver 900 low albedo spots identified as a result of secondary ejecta processesSmall impact events have likely been captured in existing data sets and not yet recognized [ABSTRACT FROM AUTHOR]

Metaphor generation is both a creative act and a means of learning. When learning a new concept, people often create a metaphor to connect the new concept to existing knowledge. Does the manner in which people generate a metaphor, via sudden insight (Aha! moment) or deliberate analysis, influence the quality of generation and subsequent learning outcomes? According to some research, deliberate processing enhances knowledge retention; hence, generation via analysis likely leads to better concept learning. However, other research has shown that solutions generated via insight are better remembered. In the current study, participants were presented with science concepts and descriptions, then generated metaphors for the concepts. They also indicated how they generated each metaphor and rated their metaphor for novelty and aptness. We assessed participants' learning outcomes with a memory test and evaluated the creative quality of the metaphors based on self‐ and crowd‐sourced ratings. Consistent with the deliberate processing benefit, participants became more familiar with the target science concept if they previously generated a metaphor for the concept via analysis compared to via insight. We also found that metaphors generated via analysis did not differ from metaphors generated via insight in quality (aptness or novelty) nor in how well they were remembered. However, participants' self‐evaluations of metaphors generated via insight showed more agreement with independent raters, suggesting the role of insight in modulating the creative ideation process. These preliminary findings have implications for understanding the nature of insight during idea generation and its impact on learning. [ABSTRACT FROM AUTHOR]

This research aimed to examine the compound effects of polyacrylamide (PAM) and cadmium (Cd) on plant growth subsequent to the mixing of municipal sludge with soil and to explore the potential ecological risks associated with the use of sludge. A pot experiment was performed wherein four gradients (0, 5, 15, and 20 g/[kg dry sludge]) were established corresponding to different PAM concentrations to assess the effects on the physiological and biochemical parameters of Brassica campestris L. ssp. chinensis Makino and Brassica campestris L. and the effects on Cd and PAM concentrations in soil. The findings indicated that the biomass of both plants increased when the total PAM concentration ranged from 5 g to 15 g/(kg dry sludge). Concurrently, polyacrylamide (PAM) downplayed the uptake of Cd by the plants, reduced phytotoxicity, and increased the activities of antioxidant enzymes such as superoxide dismutase (SOD) and peroxidase (POD) in the roots. However, the biomass of Brassica campestris L. ssp. chinensis Makino and Brassica campestris L. decreased significantly when the total PAM concentration was exceeded 15 g/(kg dry sludge), and the toxic effect of Cd on pants was enhanced to some extent. Especially when the PAM concentration was 20 g/(kg dry sludge), apparent cell damage was observed in root cells. It was further noted that Brassica campestris L. portrayed a higher tolerance towards higher proportions of sludge compared with Brassica campestris L. ssp. chinensis Makino. Sludge holds a wider scale of applicability in landscaping than in agriculture. A fusion of polyacrylamide (PAM) and antioxidant enzymes could potentially counteract the effects of Cd within a specific concentration range, serving as a defense mechanism against stress. The data obtained from this study are crucial for unraveling anti‐stress responses and detoxification mechanisms employed by different plant species under the influence of factors such as PAM, Cd, and others, thus providing novel insights into research related to land use involving sludges. [ABSTRACT FROM AUTHOR]

Aim Methods Results Conclusion Cognitive disturbances typically precede the onset of overt psychotic symptoms and represent a neurobiological marker for psychosis risk that is also associated with poor functional outcomes. The Measure of Insight into Cognition‐Self Report (MIC‐SR) is a widely used 12‐item questionnaire that assesses the perceived frequency of cognitive impairment in the domains of executing functioning, attention, and memory. However, the MIC‐SR is not available in Spanish, one of the most widely spoken languages worldwide. The present study aimed to provide a Spanish version of the MIC‐SR and examine its psychometric properties in psychosis‐risk and non‐clinical Mexican young adults.The sample comprised 621 participants who completed a battery of self‐report measures via an online survey. Of the participants, 478 were non‐clinical, and 143 met the screening criteria for a clinical high‐risk for psychosis (CHR‐positive).Confirmatory Factor Analyses supported a one‐factor model, consistent with the findings for the original MIC‐SR. The results showed adequate fit indices for the general model and the independent models for both groups, with high Cronbach's alpha coefficients. Furthermore, the CHR‐positive group showed more frequent subjective cognitive problems on each of the 12 items, higher total scores, and higher average frequency than the non‐clinical group.To our knowledge, this is the first translation of the MIC‐SR into Spanish. Using the MIC‐SR at the CHR stage may contribute to our understanding of cognitive processes associated with the onset of a psychotic disorder and provide valuable information in the context of detection and early intervention efforts. [ABSTRACT FROM AUTHOR]

We investigate the geodynamic and melting history of Mars using 3D spherical shell models of mantle convection, constrained by the recent InSight mission results. The Martian mantle must have produced sufficient melt to emplace the Tharsis rise by the end of the Noachian–requiring on the order of 1–3 × 109 km3 of melt after accounting for limited (∼10%) melt extraction. Thereafter, melting declined; however, abundant evidence for limited geologically recent volcanism necessitates some present‐day melt even in the cool mantle inferred from InSight data. We test models with two mantle activation energies and a range of crustal Heat Producing Element (HPE) enrichment factors and initial core‐mantle boundary temperatures. We also test the effect of including a hemispheric (spherical harmonic degree‐1) step in lithospheric thickness to model the Martian dichotomy. We find that a higher activation energy (350 kJ mol−1) rheology produces present‐day geotherms consistent with InSight results, and crustal HPE enrichment factors of 5–10‐times produce localized melting near or up to present‐day. The 10‐times crustal HPE enrichment is consistent with both InSight and geochemical results and also produces present‐day geoid power spectra consistent with Mars. However, calculations that match the present‐day geoid power spectra require more than 60% melt extraction to produce the Tharsis swell. The addition of a degree‐1 hemispheric dichotomy, as an equatorial step in lithospheric thickness, does not significantly improve upon melt production or the geoid. Plain Language Summary: Mars' mantle needed to produce an extremely high volume of melt by ∼3.7 billion years ago in order to build the immense volcanic plateau of Tharsis. There is also abundant evidence for small volumes of geologically recent volcanism, yet the InSight mission results are consistent with a relatively cool present‐day mantle. We use 3D numerical models of the Martian mantle to determine what properties can produce a melting history and present interior temperatures consistent with InSight results and Mars' volcanic history. We test sets of models with two different sensitivities of the mantle viscosity to changes in temperature (i.e., activation energy), and a range of enrichment factors in Heat Producing Elements in the crust. We also test the effect of including a simplified version of the Martian hemispheric dichotomy. Our models with the higher activation energy and 10‐times crustal enrichment in HPEs (consistent with Mars' crustal composition) produce melt near the present‐day as well as temperature profiles consistent with InSight. However, it is very difficult to produce sufficient melt to form Tharsis in such a cool mantle, without assuming most of the melt produced in the mantle reaches the surface. Addition the simplified dichotomy does not significantly improve our results. Key Points: Our results favor a higher activation energy mantle rheology and 10‐times crustal heat producing element enrichment factorEven with the cool mantle consistent with InSight results, we obtain models having melt up to present‐dayProducing sufficient melt to form Tharsis requires a degree of melt extraction 6‐times as efficient as Earth's mid‐ocean ridges [ABSTRACT FROM AUTHOR]

Thermal tides are atmospheric planetary‐scale waves with periods that are harmonics of the solar day. In the Martian atmosphere thermal tides are known to be especially significant compared to any other known planet. Based on the data set of pressure timeseries produced by the InSight lander, which is unprecedented in terms of accuracy and temporal coverage, we investigate thermal tides on Mars and we find harmonics even beyond the number 24, which exceeds significantly the number of harmonics previously reported by other works. We explore comparatively the characteristics and seasonal evolution of tidal harmonics and find that even and odd harmonics exhibit some clearly differentiated trends that evolve seasonally and respond to dust events. High‐order tidal harmonics with small amplitudes could transiently interfere constructively to produce meteorologically relevant patterns. Plain Language Summary: In analogy to the string of a guitar, which can oscillate in integer harmonics, planetary atmospheres exhibit oscillations that are harmonics of the solar day (Harmonic 1 with a period of 24 hr; harmonic 2, 12 hr; harmonic 3, 8 hr; etc.). These oscillations are part of the so‐called "atmospheric thermal tides", which retain a complex global structure. They are conceptually related to ocean gravitational tides, and they have been observed in atmospheres of the solar system whose main source of energy is the light from the sun: Earth, Mars, Venus, and Titan. On Mars, thermal tides are particularly strong and they play a key role in atmospheric dynamics, presenting interactions with meteorological phenomena such as dust storms. Most studies on thermal tides focus on low‐order harmonics (1, 2, 3, and sometimes 4). In this study, we use a particularly sensitive pressure sensor that landed on Mars with the InSight mission to explore the existence of high‐order harmonics, and we find clear harmonics with very small amplitudes even beyond harmonic 24, which corresponds to 24 oscillations per solar day. We compare the characteristics of those harmonics and analyze their seasonal behavior, and we find that even and odd harmonics exhibit clearly different behaviors. Key Points: Analysis of an unprecedented data set of pressure obtained by InSight suggests that tidal harmonics beyond 24 are present on MarsEven and odd modes exhibit distinct patterns with a seasonal dependency centered on equinoxes and solstices, and response to dust events [ABSTRACT FROM AUTHOR]

This study investigates the impact of wastewater irrigation on soil dielectric parameters, focusing on the often‐overlooked aspect of dielectric properties in contaminated soil. Wastewater, a significant contributor to soil and groundwater degradation, has long‐term effects on soil physical, chemical, and dielectric characteristics. Experimental measurements conducted overtime at 2.45 and 5.8 GHz frequencies reveal a correlation between wastewater irrigation and changes in dielectric properties. Emphasizing time variation as a pivotal independent variable, the study sheds light on its substantial influence on soil dielectric behavior. Notably, the research introduces an alternative methodology for the comprehensive evaluation of wastewater‐induced pollution effects on soil properties. This approach is substantiated by meticulous physicochemical analyses conducted on both pollution sources and the affected soil. The study further presents a robust response surface method‐based model, showcasing impressive accuracy with dielectric properties (ε′ and ε″) and penetration depth with R2 values of 0.9845, 0.9831, and 0.9528, respectively. Beyond unveiling crucial insights into the intricate interplay of wastewater and soil dielectric behavior, this research contributes to the development of effective strategies for pollution monitoring and management in soil ecosystems. [ABSTRACT FROM AUTHOR]

Aim: Deep brain stimulation (DBS) is a safe and effective treatment option for people with refractory obsessive‐compulsive disorder (OCD). Yet our understanding of predictors of response and prognostic factors remains rudimentary, and long‐term comprehensive follow‐ups are lacking. We aim to investigate the efficacy of DBS therapy for OCD patients, and predictors of clinical response. Methods: Eight OCD participants underwent DBS stimulation of the nucleus accumbens (NAc) in an open‐label longitudinal trial, duration of follow‐up varied between 9 months and 7 years. Post‐operative care involved comprehensive fine tuning of stimulation parameters and adjunct multidisciplinary therapy. Results: Six participants achieved clinical response (35% improvement in obsessions and compulsions on the Yale Brown Obsessive Compulsive Scale (YBOCS)) within 6–9 weeks, response was maintained at last follow up. On average, the YBOCS improved by 45% at last follow up. Mixed linear modeling elucidated directionality of symptom changes: insight into symptoms strongly predicted (P = 0.008) changes in symptom severity during DBS therapy, likely driven by initial changes in depression and anxiety. Precise localization of DBS leads demonstrated that responders most often had their leads (and active contacts) placed dorsal compared to non‐responders, relative to the Nac. Conclusion: The clinical efficacy of DBS for OCD is demonstrated, and mediators of changes in symptoms are proposed. The symptom improvements within this cohort should be seen within the context of the adjunct psychological and biopsychosocial care that implemented a shared decision‐making approach, with flexible iterative DBS programming. Further research should explore the utility of insight as a clinical correlate of response. The trial was prospectively registered with the ANZCTR (ACTRN12612001142820). [ABSTRACT FROM AUTHOR]

Self‐reflection is broadly considered a core competency for psychologists; however, there is an absence of measures of self‐reflection, limiting the extent to which self‐reflection can be assessed in both research and practice contexts. Whilst the Self‐Reflection and Insight Scale (Grant et al., 2002) has been validated in a range of formats with different populations, it has not yet been validated with psychologists. Further, the psychometric properties of a short version of the scale (Silvia, 2021) have not been examined for use with psychologists. This study tested the factor structure, internal consistency and convergent and divergent validity of the Self‐Reflection and Insight Scale with registered psychologists (N = 123), finding both the full scale and short version to have sound psychometrics. However, as there were low loading items across both versions of the measure, and the short version also excluded high‐loading items, the SRIS‐Revised (SRIS‐R) was formed through model improvement, retaining a total of 14 items. This revised version of the scale captures high loading items without redundancy of low‐loading items, resulting in a measure that parsimoniously captures the construct of self‐reflection as relevant to psychologists. The SRIS‐R demonstrated good internal consistency (α =.882), convergent, divergent and construct validity. Scores on the SRIS‐R were used to test whether there was a correlation between self‐reflection and years of professional registration, with this not being significant. [ABSTRACT FROM AUTHOR]

The InSight mission deployed one seismic station on Mars, providing a chance to apply single‐station‐based autocorrelation analysis to investigate Martian subsurface structures. However, recent analysis indicated the low‐frequency autocorrelation signals may originate from quasi‐periodic high‐amplitude instrumental "glitches" rather than the reflection response of deep Mars. In this study, we detected and removed these high‐amplitude glitches in raw seismic data and employed autocorrelation on the clean vertical component waveforms filtered between 0.05 and 0.1 Hz. We observed signals at the expected times for the olivine‐wadsleyite transition and core‐mantle boundary (CMB) as estimated by other methods. This result suggests that the low‐frequency autocorrelation signals are the reflection response from the olivine‐wadsleyite transition in the mantle and the Martian CMB region, rather than a noise phenomena. A grid search method to fit the observed PcP waveform was used to identify a layer intermediate in velocity between the Martian mantle and core at the Martian CMB. Plain Language Summary: The InSight mission deployed one seismic station on Mars at the end of 2018 to measure the interior structure of Mars. A recent study autocorrelated the InSight ambient noise data to retrieve reflection signals from subsurface discontinuities. Two seismic signals that reflected from deep within Mars, the olivine‐wadsleyite transition, a pressure‐temperature dependent mineral phase change in the mantle, and the core‐mantle boundary (CMB), are observed. However, some analyses suggested that the arrival times of these signals coincide with the recurrence time of high‐amplitude glitches within the raw seismic data, leading to an incorrect interpretation of the autocorrelation function (ACF). To resolve this issue, we detected and removed the high‐amplitude glitches before further processing the ambient noise data. The autocorrelation analysis of clean continuous vertical‐component waveforms recovers signals at times corresponding to the olivine‐wadsleyite transition and CMB, whereas ACF of glitch‐only waveforms does not. This suggests that signals on the low‐frequency ACF are from the seismic discontinuities at olivine‐wadsleyite transition and CMB rather than being noise artifacts. We further identified velocity layering near Martian CMB by matching the complexity of the PcP signal observed in the ACF of clean data set with synthetic seismograms. Key Points: Autocorrelation of clean Seismic Experiment for Interior Structure waveforms recovers the prominent signals reflected from deep MarsThe autocorrelation tests on raw, clean and glitch‐only data suggest the signals identified are from deep Mars rather than instrumental noiseA velocity transition model of the Martian core‐mantle boundary better fits the observed PcP phase than a sharp velocity drop [ABSTRACT FROM AUTHOR]

Background and Aims: Cannabis use disorder (CUD) prevalence has increased, while perceived risks of cannabis use and CUD treatment need have decreased. Chronic cannabis use may also impair the neural and behavioral mechanisms of insight, further hampering treatment‐seeking. This study aimed to measure whether CUD is characterized by reduced self‐monitoring in drug‐related contexts (objectively‐assessed insight), subserved by functional neural abnormalities in error‐processing and manifested clinically as decreased awareness of the need to change. Design: Case–control laboratory study was used. Setting: University setting was in Alabama, USA. Participants: There were 42 CUD participants and 47 age‐, sex‐, and nicotine use‐matched controls. Measurements: Participants completed a probabilistic choice task, adapted for the first time for CUD, in which they selected pleasant, unpleasant, neutral, and cannabis‐related images according to their preference. Reduced versus accurate insight was operationalized as the correspondence between self‐reported and actual most chosen image type. Neurophysiological error‐processing during an inhibitory control task was recorded using electroencephalography. Participants with CUD completed measures of cannabis problem recognition and motivation to change. Findings Compared with controls, the CUD group made significantly more cannabis selections on the choice task (mean difference [MD] = 8.11, 95% confidence interval [CI] [4.88 11.35], p < 0.001) and had significantly reduced insight into cannabis choice (odds ratio [OR] = 9.69, 95% CI [1.06 88.65], p = 0.04). CUD participants with reduced insight on the choice task had significantly decreased neurophysiological reactivity to errors on the inhibitory control task (error‐related negativity) compared with CUD participants with accurate insight (MD = 2.64 μV, 95% CI [0.74 μV 4.54 μV], p = 0.008) and controls (MD = 4.05 μV, 95% CI [1.29 μV 6.80 μV], p = 0.005). Compared with CUD participants with accurate insight on the choice task, CUD participants with reduced insight reported significantly less agreement that they had a cannabis problem (MD = ‐5.06, 95% CI [−8.49–1.62], p = 0.003). Conclusions: People with CUD who show reduced insight on a drug‐related choice task may also have decreased early neural error‐processing and less cannabis problem recognition. [ABSTRACT FROM AUTHOR]

Gaining awareness of psychosis (i.e., insight) is linked to depression, particularly in the post‐acute phase of psychosis. Informed by social rank theory, we examined whether the insight–depression relationship is explained by reduced social rank related to psychosis and whether self‐compassion (including uncompassionate self‐responding [UCS] and compassionate self‐responding [CSR]) and mindfulness buffered the relationship between social rank and depression in individuals with first episode psychosis during the post‐acute phase. Participants were 145 young people (Mage = 20.81; female = 66) with first episode psychosis approaching discharge from an early psychosis intervention centre. Questionnaires and interviews assessed insight, depressive symptoms, perceived social rank, self‐compassion, mindfulness and illness severity. Results showed that insight was not significantly associated to depression and thus no mediation analysis was conducted. However, lower perceived social rank was related to higher depression, and this relationship was moderated by self‐compassion and, more specifically, UCS. Mindfulness was related to depression but had no moderating effect on social rank and depression. Results supported previous findings that depressive symptoms are common during the post‐acute phase. The role of insight in depression for this sample is unclear and may be less important during the post‐acute phase than previously considered. Supporting social rank theory, the results suggest that low perceived social rank contributes to depression, and reducing UCS may ameliorate this effect. UCS, social rank and possibly mindfulness may be valuable intervention targets for depression intervention and prevention efforts in the recovery of psychosis. [ABSTRACT FROM AUTHOR]

The DSM‐5 highlights two essential psychological features of anorexia nervosa (AN): recalcitrant fear of gaining weight and body image disturbance. Prominent accounts grant false beliefs about body weight and shape a central role in the explanation of AN behavior. In this article, we propose a stronger emphasis on recalcitrant fear. We show that such fear can explain AN behavior without the intermediary of a false belief, and thus without the associated explanatory burdens and conceptual difficulties. We illustrate how shifting the emphasis from false belief to recalcitrant fear can supplement a number of different non‐doxastic models of AN. [ABSTRACT FROM AUTHOR]

Background: Clinicians recognize insight as important for safe independent medical practice. Clinical education literature focuses on self‐reflection. The aim of this review is to describe how clinical educators conceptualize reflection and ask is it analogous to how clinicians conceptualize insight? Methods: Using PRISMA guidelines, a systematic review of the literature around insight and reflection in postgraduate medical education was undertaken. A thematic analysis of the concepts of insight and reflection was performed. Results: A total of 75 reports were included in the analysis. The literature focussed predominantly on reflection with little discussion of insight. Three main themes were generated: episodic reflection; cyclic reflection; reflection as a state. Reflection as a state seemed to be the professional quality most often aspired to but was less well defined in terms of educational interventions. When more than one model was described, it was often with a reflective state being the ideal that episodic or cyclic reflection may approximate. It is not clear that it is possible to progress up the hierarchy. Conclusion: We present a novel description of a hierarchy from discrete episodes of reflection, to cyclic processes that involve reflection, through to a state in which the practitioner is reflective. There is no unified understanding of how an individual ascends this hierarchy, or a cohesive description of what insight is for an independent medical practitioner. This review highlights the need for research into how practicing clinicians conceptualize and characterize insight in their training and practice. [ABSTRACT FROM AUTHOR]

Aims: Schizophrenia is a psychiatric disorder presenting a lack of insight. Although insight changes over time, longitudinal studies of insight in schizophrenia are scarce. Furthermore, most previous studies on insight and intelligence have not measured full‐scale IQ and have not been able to examine the relationship between detailed dimensions of cognitive function and insight. In this study, we assessed insight at two time points and assessed dimensions of cognitive function. Methods: A total of 163 patients with schizophrenia participated in the study. We evaluated insight at two time points to understand the patterns of change and examined the association between insight and clinical variables. Additionally, we examined the relationship between the dimensions of cognitive function and insight. Results: The patients were divided into three groups based on their change in insight over time: stable at a low level of insight (poor insight), stable at a high level of insight (good insight), and changed in insight over time (unstable insight). Those in the poor insight group had lower general intelligence scores than those in the good insight and unstable insight groups. Regarding cognitive function, verbal comprehension was associated with the level of insight at baseline and follow‐up. Regarding psychiatric symptoms, the poor insight group exhibited more severe symptoms than the other two groups, especially regarding positive symptoms. Conclusions: Our classification of patients based on changes in insight revealed that poor insight patients had impaired cognitive function, especially verbal comprehension, and more severe positive symptoms than good insight or unstable insight patients. [ABSTRACT FROM AUTHOR]

On 4 May 2022 the InSight seismometer SEIS‐VBB recorded the largest marsquake ever observed, S1222a, with an initial magnitude estimate of MWMa ${M}_{W}^{\mathrm{M}\mathrm{a}}$ 4.6. Understanding the depth and source properties of this event has important implications for the nature of tectonic activity on Mars. Located ∼37° to the southeast of InSight, S1222a is one of the few non‐impact marsquakes that exhibits prominent surface waves. We use waveform modeling of body waves (P and S) and surface waves (Rayleigh and Love) to constrain the focal mechanism, assuming a double‐couple source, and find that S1222a likely resulted from reverse faulting in the crust (source depth near 22 km). We estimate the scalar moment to be 2.5 × 1015–3.5 × 1015 Nm (magnitude MW 4.2–4.3). Our results suggest active compressional tectonics near the dichotomy boundary on Mars, likely due to thermal contraction from planetary cooling. Plain Language Summary: The InSight lander's sensitive seismometer recorded over 1,000 seismic events during the course of its mission, consisting of both marsquakes and impacts. Like on Earth, it is thought that the majority of quakes on Mars result from faulting events that release stress within the planetary interior. Understanding the nature of these events, including their magnitude, depth, and faulting style, provides valuable clues into planetary deformation and its driving forces. In this study, we use seismic waveform modeling to constrain the properties of the S1222a event, the largest marsquake recorded during the InSight mission. We find that S1222a likely resulted from reverse (compressional) faulting within the crust of Mars and estimate that the event was equivalent to a 4.2–4.3 magnitude event on Earth. The compressional faulting may indicate ongoing thermal contraction due to planetary cooling, which, prior to the InSight lander mission, was expected to be one of the primary drivers of seismic activity on Mars. Key Points: We performed a moment tensor inversion of S1222a based on waveform fitting of both body and surface wavesThe scalar moment of S1222a is between 2.5 × 1015–3.5 × 1015 NmOur preferred solution is a NW‐SE oriented reverse fault, indicating compressional tectonics near the dichotomy boundary [ABSTRACT FROM AUTHOR]

This study examined the relationship between implicit environmental clues in a creativity task and individual differences in state change and personality traits. In two experiments, participants completed a Remote Associates Test. Some solution words were implicitly primed as clues. In Experiment 1, the clue priming effect turned from negative to positive depending on task progress, which is related to arousal state. Clue priming can hinder people's generating ideas depending on arousal. In Experiment 2, considering participants' personality traits as a moderator, we further examined the relationship between sensitivity to environmental clues and arousal measured by heart rate. The results confirmed Experiment 1's outcomes and revealed that the relationship is moderated by extraversion. For extraverted participants, an implicit clue had a negative effect in a high‐arousal state but a positive effect in a low‐arousal state. The facilitative or obstructive influences of external factors can be determined by the interaction of internal factors (i.e., solvers' traits and states). Thus, extraverts and introverts differ in how they receive and utilize external information. [ABSTRACT FROM AUTHOR]

Accurate information about marsquake locations is crucial for understanding the tectonic activity, subsurface structures, and dynamics of Mars. We designed a varying‐parameter scheme for polarization analysis to determine the back‐azimuths of marsquakes. For two Martian meteorite impact events with ground‐truth locations known from orbital images, our scheme yields back‐azimuths that are ∼5° and ∼14° closer to the true values than those reported previously, demonstrating our method's advantages in constraining back‐azimuths. We applied this method to determine the back‐azimuths of 44 Low Frequency marsquakes and 39 were reliably relocated. Nearly half of these marsquakes occur in Cerberus Fossae, while the rest are broadly distributed, including along the dichotomy boundary and within the northern lowlands and southern highlands. Although further studies are required to understand the mechanisms of these marsquakes, the widespread seismicity implies that present‐day Mars, especially the ancient southern highlands, is more tectonically active than previously thought. Plain Language Summary: Identifying seismic activity on Mars is crucial for advancing our understanding of the planet's present‐day properties and tectonic processes. From February 2019 to December 2022, the InSight seismograph captured nearly one hundred Low Frequency marsquakes. As these marsquakes have similar ground vibration characteristics to tectonic earthquakes, they are important to understand tectonic‐related activities on Mars. However, there is only a single seismograph on Mars, and some of the data for Low Frequency marsquakes are noisy, making it challenging to precisely determine their locations. To improve the accuracy of marsquake locations, we devised a scheme using sliding time and frequency windows to effectively constrain the orientation of marsquakes relative to the seismograph. With this method, we successfully relocated 39 Low Frequency marsquakes. Our new findings indicate that a significant portion, approximately half, of these marsquakes are concentrated in the Cerberus Fossae region, while the remaining events are distributed across various tectonic units. Interestingly, we have also identified marsquakes within the ancient southern highlands, an area that has previously had limited reports of seismic activity. Although the origin of marsquakes may differ from region to region, the widespread distribution of marsquakes suggests that Mars is more tectonically active than previously thought. Key Points: The varying‐parameter polarization analysis scheme can effectively improve the accuracy of back‐azimuth estimates for marsquakesSeveral additional Low Frequency marsquakes have been identified within the southern highlands of MarsThe widespread Martian seismicity implies that Mars is more tectonically active than previously thought [ABSTRACT FROM AUTHOR]

Convective vortices (whirlwinds) and dust devils (dust‐loaded vortices) are one of the most common phenomena on Mars. They reflect the local thermodynamical structure of the atmosphere and are the driving force of the dust cycle. Additionally, they cause an elastic ground deformation, which is useful for retrieving the subsurface rigidity. Therefore, investigating convective vortices with the right instrumentation can lead to a better understanding of the Martian atmospheric structures as well as the subsurface physical properties. In this study, we quantitatively characterized the convective vortices detected by NASA's InSight (∼13,000 events) using meteorological (e.g., pressure, wind speed, temperature) and seismic data. The evaluated parameters, such as the signal‐to‐noise ratio, event duration, asymmetricity of pressure drop profiles, and cross‐correlation between seismic and pressure signals, are compiled as a catalog. Using these parameters, we investigated (a) the vortex structure and (b) the subsurface physical properties. Regarding the first topic, we tried to illustrate the vertical vortex structure and its link to the shape of the pressure profiles by combining the asymmetrical features seen in the observed pressure drops and the terrestrial observations of dust devils. Our results indicate that most of the vortices move with the wall tilted in the advection direction. Concerning the second topic, selecting the highly correlated events between pressure perturbation and ground response, we estimated the subsurface rigidity at the InSight landing site down to 100 m depth. Our results indicate that the subsurface structure can be modeled with two layers having a transition at 5–15 m depth. Plain Language Summary: As frequently observed on Earth, convective vortices or dust‐loaded vortices are also seen on Mars. They reflect the local atmospheric structure and are the main driving force to lift the fine dust from the ground. In 2018, NASA's InSight succeeded in installing the meteorological and geophysical packages on Mars. That brought us, in particular, meteorological data with an extremely high temporal resolution, contributing to resolving local phenomena such as convective vortices. In this study, using InSight's meteorological (e.g., pressure, air temperature) and seismic data, we quantitatively characterize convective vortices to understand this phenomenon from both meteorological and geophysical aspects. Especially focusing on the asymmetricity of pressure drop profiles at vortex encounters and the correlation between the pressure variations and seismic signals, we investigated (a) a link between the shape of pressure drop profiles and the vertical vortex structure and (b) the ground rigidity structure by measuring the ground responses against the vortex‐related pressure variations. Consequently, first, we found that most of the vortices move with the wall tilted in the advection direction. Second, our results indicated that the subsurface structure can be modeled with two layers down to 100 m with a transition at 5–15 m depth. Key Points: We quantitatively characterized the Martian convective vortices observed by InSight's seismometer and meteorological instrumentsFocusing on the pressure drop profiles, we inferred a link between the asymmetricity and the vertical vortex structureWith the cataloged parameters, we performed a compliance analysis and evaluated the ground rigidity at the InSight landing site [ABSTRACT FROM AUTHOR]

The InSight seismometers have recorded more than 1,300 events. Ninety‐eight of these, named the low‐frequency (LF) family, show energy predominantly below 1 Hz down to ∼0.1 Hz. The Marsquake Service identified seismic phases and computed distances for 42 of these marsquakes, 24 of which have backazimuths. Hence, the locations of the majority of LF family events remain undetermined. Here, we use an envelope shape similarity approach to determine event classes and distances, and introduce an alternative method to estimate the backazimuth. In our analysis, we use the highest quality marsquakes with known distances as templates, including the largest event S1222a, and assign new distances to similar group of events for which distance estimates were not previously available. We find the Tharsis region to be more active than initially perceived on the basis of 5 newly located events near Valles Marineris and Olympus Mons. We relocate two marsquakes with little or no S‐wave energy in the NE of the Elysium Bulge. The event epicenters in Cerberus Fossae follow a north‐south trend due to uncertainties in location, while the fault system is in the NW‐SE direction; therefore, these events are re‐projected along the observed fault system based on our interpretations. The marsquakes in our interpreted catalog are predominantly observed in the northern hemisphere of Mars above the equatorial dichotomy boundary. Plain Language Summary: InSight's seismometer recorded more than 1,300 events since landing on the surface of Mars in November 2018 until it retired in December 2022. Most of the events InSight recorded are at high frequencies ≥2.4 Hz. The rest of the events, named the low‐frequency family, produce signals that travel through the planet's interior, allowing us to understand the interior structure when event locations can be determined. In order to use the single‐station approaches for computing the distance and the angle between the station and an event, at least two clear seismic phase arrivals (such as P‐ and S‐waves for distance and P‐wave for event angle) are required. However, marsquakes are often weak and do not always exhibit clear seismic phases; therefore, they cannot be assigned distances using traditional techniques. Here, we use the well‐understood, highest‐quality events as templates to investigate and assign a source region to the weaker seismic signals. Seismicity on Mars occurs mostly along or north of the boundary between the southern highlands and northern lowlands. Valles Marineris is seismically more active than previous catalogs of located events imply. Further, we show evidence that two events likely originate from the Olympus Mons region. Key Points: We use a similarity analysis and high quality marsquake templates from InSight to estimate distances of additional eventsCombining this with new backazimuth estimates we can relocate marsquakes and update the seismicity map of MarsOur results suggest clusters of seismicity have occurred nearby Valles Marineris and Olympus Mons [ABSTRACT FROM AUTHOR]

Estimating the rupture process of a quake constrains the tectonic setting of its source region. In terrestrial seismology, the rupture process can be described with a classical ω2 model. In this study, we focus on one key source parameter of S1222a, the corner frequency, to investigate its origin. However, estimating the corner frequency of S1222a is complicated by S1222a's non‐classical spectra which deviate from the ω2 model. To explain S1222a's spectra, we take into account the site effect at the InSight landing site. Through numerical simulation, we demonstrate that the spectral fitting is greatly improved after considering the site effect. We further estimated the source spectrum and stress drop of S1222a. The obtained stress drop resembles the values for regional tectonic earthquakes and shallow moonquakes but differs from the Cerberus Fossae marsquakes, which favors a different tectonic origin from the Cerberus Fossae marsquakes for S1222a. Plain Language Summary: The source of a quake is a key piece of information to uncover the dynamic process at the source region. In terrestrial seismology, the source of a quake can be described with a classical model in which the spectra decay with frequency at a certain speed. In this study, we focus on one key source parameter of S1222a, the corner frequency, to explore the generating process of S1222a. However, S1222a exhibits non‐classical spectra which cannot be explained by the classical model, making it difficult to estimate S1222a's source spectrum. To explain S1222a's spectra, we hypothesized that the seismic records are contaminated by wave reverberations in the subsurface layers, namely site effect. We validated our hypothesis with a numerical method. After considering site effect, S1222a's source spectrum and stress drop can be better estimated. The obtained stress drop value is close to those for regional tectonic earthquakes and shallow moonquakes but differs from the values observed for some marsquakes located at Cerberus Fossae, a seismically active region on Mars. Thus, we conclude that S1222a has a different tectonic origin from the Cerberus Fossae marsquakes. Key Points: We constructed a numerical model to simulate the site effect at the InSight landing site to better explain the spectra of S1222aWe estimated the corner frequency of S1222a to be 0.76 (0.58–1.07) Hz, which corresponds to a stress drop of 3.62 (0.80–20.26) MPaThe corner frequency and stress drop estimation favor that S1222a has a different tectonic origin from the Cerberus Fossae marsquakes [ABSTRACT FROM AUTHOR]

To date, three Mars landers carried seismometers: Viking 1 and 2 in 1976 (Viking 1 seismometer failed) and InSight in 2018. In 574 Sols (one Sol is one solar day on Mars), Viking detected one possible marsquake on Sol 80 and one discounted marsquake on Sol 53. Both events were recorded in Event Mode, a two‐channel (amplitude and frequency at 1 Hz) compression technique. In contrast, in 1440 Sols, InSight confirmed 1319 full waveform marsquakes. InSight's technology and capability were significantly better than Viking's, with wind and lander noise being significant for both missions. This project developed three evaluation tools: (a) Comparison and re‐evaluation of Viking Sol 80 and 53 with Viking wind data, (b) a recovered Viking tool to convert InSight waveforms to the Viking compressed Event Mode format, and (c) a new analysis tool to convert Viking compressed Event Mode approximate "reconstruction" to time series similar to InSight format. Evaluation using these tools allows answering the question "What would the Viking Seismology Team has concluded given the new information from InSight and the evaluation tools developed for this project?" Findings from these analyses confirm that both Viking Sol 80 and Sol 53 were marsquakes. The plausible conclusion that Sol 80 was a marsquake also provides potential information for estimating the crustal thickness in Utopia Planitia. Combining data and analysis from only two Mars landers containing working seismometers, landing 42 years apart, is planetary seismic archaeology. Plain Language Summary: Viking 1 and 2 (1976), the first successful Mars landers, each carried one seismometer. Viking 1 seismometer failed; Viking 2 seismometer worked and in 574 Sols (one Sol is one solar day on Mars), recorded two potential marsquakes (Sol 80 and Sol 53). Confirming a marsquake requires that these events are not wind and are similar to earthquakes or marsquakes. Sol 80 was a night time event with typically low wind, but had no wind data. Sol 53 was a day time event, typically with higher winds and correlated with wind. Both were similar to California seismic events. InSight (2018), in 1440 Sols, confirmed 1319 marsquakes. Wind and lander noise were significant for both missions. Viking's unique triggered and compressed Event Mode at 1 Hz was compared with InSight's 20 Hz waveform data used for this project and each was converted to the other's format. The objective of "What would the Viking Seismology Team have concluded given this new information?" is answered by demonstrating that both Viking seismic events, Sol 80 and Sol 53 are marsquakes. Combining data and analysis from the only two Mars landers containing seismometers, landing 42 years apart, is planetary seismic archaeology. Key Points: Viking 1976 possible marsquakes are separated from wind and compared with InSight 2018 confirmed marsquakesDeveloped Viking Lander seismic simulation; Viking Event Mode reconstruction; InSight data detrending and deglitchingViking Mission to Mars 1976 two possible marsquakes, Sol 80 and 53, are resolved as marsquakes [ABSTRACT FROM AUTHOR]

Multilanders and rovers on Mars have observed the diurnal variation in surface pressure with two significant peaks at dawn and twilight (around 8:00 a.m. and 8:00 p.m.) at different locations near the equinox. The Dynamic Meteorology Laboratory Martian General Circulation Model (GCM) simulates similar phase‐locked surface pressure fluctuations. The surface pressure peaks at a certain local time occur at most mid‐ and low‐latitude locations, as GCM simulations suggested. By reconstructing the surface pressure variation from the horizontal mass flux obtained in the GCM simulations, we find that the pressure fluctuations are due to the diurnal variation in the horizontal wind divergence and convergence in the Martian tropical troposphere. The diurnal variation in surface pressure corresponds to the migrating diurnal tidal wind, with the enhanced convergence due to the overlap of the 4‐hr and 6‐hr tides before 8:00 a.m. and 8:00 p.m. Although the amplitudes of the 4‐hr and 6‐hr tides are smaller than those of diurnal tides, the convergences/divergences caused by the 4‐hr/6‐hr tidal winds at different altitudes are in phase and added up together to create a mass flux comparable to that induced by diurnal/semidiurnal components and lead to rapid pressure fluctuations. The 4‐hr/6‐hr tidal amplitudes and the two pressure peaks at dawn and twilight are the strongest near the equinox. Plain Language Summary: With the help of observations of Martian landers and rovers, the near‐surface pressure fluctuations in different locations are recorded, which are present near dawn and twilight with sudden pressure peaks. Previous studies reported surface pressure fluctuations and their response to the local topography. The sudden pressure peaks presented at the same local time in different locations imply a possible relationship between the pressure peaks and the solar tides. In this study, the pressure fluctuations recorded by different landers are attributed to the diurnal variation in the horizontal wind divergence and convergence in the Martian troposphere. The zonal wind variation with periods of 4 and 6 hr mainly contributes to the observed fluctuations. The migrating diurnal/semidiurnal tidal winds offer a background for the diurnal pressure cycle. Key Points: Insight and other landers at different locations observe the phase‐locked surface pressure fluctuations in the Martian tropicsThe surface pressure fluctuations are primarily attributed to the mass flux due to the horizontal wind in the Martian troposphereThe linear superposition of the 4‐hr and 6‐hr tidal winds leads to the local morning and evening rapid pressure fluctuations [ABSTRACT FROM AUTHOR]

We present the first detection of normal modes on Mars using the vertical records from InSight's broad‐band seismometer following the marsquake that occurred on sol 1222. The proposed catalog lists 60 potential eigenfrequencies between 3 and 12 mHz. Due to their low signal‐to‐noise ratio, these normal modes were detected using the phasor walkout approach. The normal modes amplitudes are consistent with the upper limit of the S1222a magnitude and with high quality factors. Additionally, we provide the first detection of a Martian hum before the quake for several of these frequencies. The proposed frequencies are at about 1‐sigma of those predicted by published models based on body wave travel time inversions. Our detection of normal modes is the first made on a terrestrial planet other than Earth and opens the way for future interior models that incorporate both normal modes frequencies, surface waves velocities and body wave travel times. Plain Language Summary: The frequencies of a planet's global oscillations are closely linked to its internal structure. Thanks to the powerful magnitude 4.7 marsquake that occurred on sol 1222 and to the low long period noise of the very broad band Insight seismometer, we detected 60 normal mode frequencies. Furthermore, we discovered evidence of continuous vibrations on Mars, called Martian hum, as several eigenfrequencies were present before the marsquake occurred. Mars is now the second terrestrial planet after the Earth for which these planetary tones are observed. Key Points: We present the first observational evidence of free oscillations excited by a seismic event and background oscillations on MarsWe extracted normal modes hidden in low signal‐to‐noise ratio seismic record using a phasor walkout analysisNormal mode frequencies can be used to narrow down published Mars interior models obtained from body wave travel time inversions [ABSTRACT FROM AUTHOR]

Standard X‐ray photoelectron spectroscopy (XPS) analysis is thought of by many as a non‐destructive form of analysis; however, both the interaction of the X‐ray photons and the subsequent electron cascade can cause significant changes to the analysed area. This XPS Insights paper gives a brief overview to this phenomenon, supported by specific examples and experimental advice to assess and minimise damage during analysis. [ABSTRACT FROM AUTHOR]

In an attempt to improve the quality of the seismic signals provided by the seismometer of the InSight mission (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) on Mars, part of the tether linking the seismometer to the InSight lander was buried by some regolith using the scoop of the articulated robotic arm. The regolith in a source area was scraped into piles, scooped and dumped by the scoop from a height of ∼50 cm above the surface onto the tether. Part of the regolith was carried away by the wind and dispersed 1–2 m downwind, as evidenced by the comparison between images taken from the lander before and after the regolith pouring. Using both ballistic trajectory and wind dispersion effects as a sorter, the grain size range was determined through numerical fluid mechanics simulations. The trajectory of the poured grains is determined by the Martian atmospheric and gravimetry conditions, the initial conditions of scoop pouring and grain lithology. The spatial grain distribution on the ground shows a downwind decrease in grain size from the pouring point, with a size ranging from 1 mm near the dump point to ∼100 μm at the farthest area observed on the images. We find that the deposit of grains coarser than 500 μm is controlled mainly by gravity. Grains finer than 100 μm are present in the regolith, but they are not quantifiable with this method because they are blown away by the wind. Plain Language Summary: The soil on which the lander of the geophysical InSight mission on Mars has landed is partially known, mainly through visual observations by the lander's cameras and calculations based on their thermal properties (derived from both orbiter and lander measurements). Some soil scraped by the scoop of the lander's robotic arm was dumped on the tether connecting the InSight seismometer, so as to improve the quality of the seismic signals. During these dumpings, it was observed that some particles were blown away by Martian winds that were simultaneously recorded by the lander instruments. Given that they are subjected to the combined effect of gravity and wind, larger particles rapidly fall below the scoop, whereas smaller ones are blown away; the smaller the particle, the larger the distance. The trajectory of the poured particles was numerically calculated using fluid mechanics to account for wind effects, and the resulting downwind deposit was compared to that given by photos. It was shown that particles larger than 500 μm fell close to the pile formed below the scoop, whereas smaller ones (>100 μm) fell at distances of 2–4 m. Smaller particles (<100 μm) including dust (<5–10 μm) were blown further away. Key Points: The grain size distribution of the InSight Martian regolith is better constrained by using wind as a sorter during the burial of a tetherBased on image observations and numerical fluid mechanics simulations, the regolith mainly contains grains between 100 μm and 1 mmGrains smaller than 100 μm are not quantifiable because they have been blown away by the wind [ABSTRACT FROM AUTHOR]

Using seismic recordings of event S1222a, we measure dispersion curves of Rayleigh and Love waves, including their first overtones, and invert these for shear velocity (VS) and radial anisotropic structure of the Martian crust. The crustal structure along the topographic dichotomy is characterized by a fairly uniform vertically polarized shear velocity (VSV) of 3.17 km/s between ∼5 and 30 km depth, compatible with the previous study by Kim et al. (2022), https://doi.org/10.1126/science.abq7157. Radial anisotropy as large as 12% (VSH > VSV) is required in the crust between 5 and 40 km depth. At greater depths, we observe a large discontinuity near 63 ± 10 km, below which VSV reaches 4.1 km/s. We interpret this velocity increase as the crust‐mantle boundary along the path. Combined gravimetric modeling suggests that the observed average crustal thickness favors the absence of large‐scale density differences across the topographic dichotomy. Plain Language Summary: The first detection and analysis of surface waves on Mars (Kim et al., 2022, https://doi.org/10.1126/science.abq7157) revealed that the crustal structure away from the InSight lander is fairly uniform between 5 and 30 km depth in the northern lowlands. This is strikingly different from the crustal structure inferred beneath the lander. The largest marsquake recorded during the InSight mission to Mars, S1222a, provides the first clear signals of both types of surface waves—called Rayleigh and Love waves—as well as their first overtones. We analyze the speed at which these waves travel changes with their frequency to see deeper into Mars than possible with previous data. We find that the crustal structure along the path to S1222a, which covers a different part of the northern lowlands, is similar to that found previously, suggesting that uniform velocities in the depth range of 5–30 km may be characteristic for this region. By combining our seismic data with variations in the strength of gravity, we determine that the density of the crust in the northern lowlands and the southern highlands is similar. Finally, by analyzing both types of surface waves, we find that the speed of horizontally polarized waves is up to 12% faster than that of vertically polarized waves. Key Points: By jointly analyzing Rayleigh and Love waves, and their overtones in the S1222a record, we obtain the seismic velocity structure of Mars down to 90 km depthRadial anisotropy up to 12% (VSH > VSV) is required in the crustal structure along the path to S1222aAbsence of large‐scale density differences across the martian dichotomy better explains the average crustal thickness along the propagation path [ABSTRACT FROM AUTHOR]

The heat flow and physical properties package measured soil thermal conductivity at the landing site in the 0.03–0.37 m depth range. Six measurements spanning solar longitudes from 8.0° to 210.0° were made and atmospheric pressure at the site was simultaneously measured using InSight's Pressure Sensor. We find that soil thermal conductivity strongly correlates with atmospheric pressure. This trend is compatible with predictions of the pressure dependence of thermal conductivity for unconsolidated soils under martian atmospheric conditions, indicating that heat transport through the pore filling gas is a major contributor to the total heat transport. Therefore, any cementation or induration of the soil sampled by the experiments must be minimal and soil surrounding the mole at depths below the duricrust is likely unconsolidated. Thermal conductivity data presented here are the first direct evidence that the atmosphere interacts with the top most meter of material on Mars. Plain Language Summary: A soil's ability to transport heat is a fundamental parameter that holds information on quantities like soil bulk porosity, composition, grain size, and the state of cementation or induration. In the soil, heat is transported through grain‐to‐grain contacts as well as through the pore filling CO2 gas. The heat flow and physical properties package (HP3) of the InSight Mars mission measured soil thermal conductivity at the landing site repeatedly over the course of a martian year. As atmospheric pressure changes between seasons due to the redistribution of CO2 across the planet, we found that soil thermal conductivity also changes. Thermal conductivity increased for increased atmospheric pressure, a behavior typical for unconsolidated material. This implies that the amount of cement or induration of the sampled soil must be minimal. Key Points: We measured thermal conductivity of the martian soil and found that its conductivity strongly correlates with atmospheric pressureWe conclude that heat conduction through the pore‐filling gas is significant and that cementation of the soil must be minimalOur data show that the atmosphere directly interacts with the top most meter of material on Mars [ABSTRACT FROM AUTHOR]

The seismic activity of a planet can be described by the corner magnitude, events larger than which are extremely unlikely, and the seismic moment rate, the long‐term average of annual seismic moment release. Marsquake S1222a proves large enough to be representative of the global activity of Mars and places observational constraints on the moment rate. The magnitude‐frequency distribution of relevant Marsquakes indicates a b $b$‐value of 1.06. The moment rate is likely between 1.55×1015Nm/a $1.55\times {10}^{15}\mathrm{N}\mathrm{m}/\mathrm{a}$ and 1.97×1018Nm/a $1.97\times {10}^{18}\mathrm{N}\mathrm{m}/\mathrm{a}$, with a marginal distribution peaking at 4.9×1016Nm/a $4.9\times {10}^{16}\mathrm{N}\mathrm{m}/\mathrm{a}$. Comparing this with pre‐InSight estimations shows that these tended to overestimate the moment rate, and that 30% or more of the tectonic deformation may occur silently, whereas the seismicity is probably restricted to localized centers rather than spread over the entire planet. Plain Language Summary: The seismic moment rate is a measure for how fast quakes accumulate deformation of the planet's rigid outer layer, the lithosphere. In the past decades, several models for the deformation rate of Mars were developed either from the traces quakes leave on the surface, or from mathematical models of how quickly the planet's interior cools down and shrinks. The large marsquake that occurred on the 4th of May 2022 now allows a statistical estimation of the deformation accumulated on Mars per year, and thus to confront these models with reality. It turns out that, although there is a considerable overlap, the models published prior to InSight tend to overestimate the seismic moment rate, and hence the ongoing deformation on Mars. Possible explanations are that 30% or more of the deformation occurs silently, that is, without causing quakes, or that not the entire planet is seismically active but only specific regions. Key Points: A single large marsquake suffices to constrain the global seismic moment ratePre‐InSight estimations tended to overestimate the moment rateEither a significant part of the ongoing deformation occurs silent, or seismic activity is restricted to some activity centers, or both [ABSTRACT FROM AUTHOR]

NASA's InSight has detected a large magnitude seismic event, labeled S1222a. The event has a moment magnitude of MWMa ${\mathrm{M}}_{\mathrm{W}}^{\text{Ma}}$4.7, with five times more seismic moment compared to the second largest event. The event is so large that features are clearly observed that were not seen in any previously detected events. In addition to body phases and Rayleigh waves, we also see Love waves, minor arc surface wave overtones, and multi‐orbit surface waves. At long periods, the coda event exceeds 10 hr. The event locates close to the North‐South dichotomy and outside the tectonically active Cerberus Fossae region. S1222a does not show any evident geological or tectonic features. The event is extremely rich in frequency content, extending from below 1/30 Hz up to 35 Hz. The event was classified as a broadband type event; we also observe coda decay and polarization similar to that of very high frequency type events. Plain Language Summary: After 3 years of seismic monitoring of Mars by InSight Seismic Experiment for Interior Structure instrument, we detected a marsquake largest ever observed during the mission. The event is larger by factor of 5 in seismic moment compared to previously detected events. With such an energetic event, we discovered various seismic features that was never observed before. For the first time, we were able to detect body waves and surface waves with their overtones. The large variety of detected seismic phases will enable us to probe the internal structure of Mars. Second, the event was located outside a well‐known seismically active region of Cerberus Fossae. This might indicate that event do not come from the same fault system with other major marsquakes. Finally, this event shows simultaneously features of marsquakes that were previously classified into different types. S1222a is classified as a broadband event with a wide frequency range of seismic energy. At the same time, the coda shape and decay at high frequency resembles that of very high frequency type events. It was an open question how different types of marsquakes are excited of what makes such differences and such event will be a key to uncover such mystery of marsquakes. Key Points: InSight detected on 4 May 2022 a MWMa ${\mathrm{M}}_{\mathrm{W}}^{\text{Ma}}$4.7 marsquake, S1222a, which is the largest seismic event detected so farThe exceptional signal‐to‐noise allows multiple phases to be identified, with a rich collection of surface wavesS1222a was located 37° southeast of the InSight landing site and close to the Martian dichotomy boundary [ABSTRACT FROM AUTHOR]

The magnetometer of the InSight mission operated on the Martian surface from November 2018 until May 2022. Previously, satellites have provided information on the Martian magnetic field environment from orbit; however, the degree to which external fields penetrate to and interact with the surface could not be studied prior to the InSight landing. Here, we present an overview of the complete surface magnetic field data from InSight sols 14 to 1241 that display different external magnetic field phenomena, transient and periodic. Periodic observations range from short period waves (100–1000s of seconds), diurnal variations, ∼26 sol Carrington rotations, to seasonal fluctuations. Transient events are observed in response to space weather and dust movement. We find that ionospheric variations are the dominant contribution as seen from the surface, while contributions from the undisturbed interplanetary magnetic field are more subtle. We discuss limitations associated with a single point measurement and opportunities that future missions could enable. Including magnetometers on future missions at a variety of locations for long‐duration continuous observations will be of great value in understanding a range of external field phenomena and will enable further investigations in different crustal magnetic field settings. Plain Language Summary: The magnetometer of the InSight mission has measured the magnetic field at the planetary surface for the first time. Although satellites previously sampled the magnetic field globally from orbit, InSight enables a local view from the surface. Here, we focus on time‐varying magnetic fields driven by the Sun and the uppermost region of the atmosphere (the ionosphere); this includes the interplanetary magnetic field and the ionosphere interacting with the planet. A range of physical phenomena can be observed. Some of those are periodic, such as the diurnal signature or seasonal variations, some are transient, such as the effect of space weather. We find that ionospheric variations are the dominant signal at the surface. We discuss limitations of such observations due to the single point measurement and possibilities future missions will provide. Key Points: InSight's magnetometer provides the first surface recordings of the Martian magnetic field environment over 1241 solsTransient and periodic external fields with timescales of minutes up to a year are observed and their origins discussedTime variations in the surface magnetic field are primarily driven by the ionosphere, affected by atmospheric seasonal variations [ABSTRACT FROM AUTHOR]

We compared problem‐solving in four sets of classical insight and analytic problems in the verbal and spatial domains, and examined the impact of externalization (verbalization or sketching). In a within‐participants factorial design, we presented 24 classical insight and analytic problems, half verbal and half spatial. Participants solved these problems either while thinking aloud, while sketching, or in a baseline condition where neither was allowed. Higher solving accuracy was found in the analytic problems than in the insight ones as well as in the verbal problems than in the spatial ones. The verbal problems were also found to be solved faster than were spatial ones; in particular, verbal‐insight problems were solved faster than spatial‐insight and verbal‐analytic ones. Therefore, spatial‐insight problems stand out as particularly hard among the ones typically found in the literature. Surprisingly, no effects of externalization were found on problem‐solving speed or accuracy. We discuss the implications of our results for the theses that insight problems involve special processes. [ABSTRACT FROM AUTHOR]

We quantify the volume and distribution of water, cement, sediments, and fractured rocks within the Martian crust beneath NASA's InSight (Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport mission) lander by using rock physics models to interpret shear wave velocities (Vs) measured from InSight data. The models assume that Mars' crust comprises sediments and fractured rocks whose pores and fractures host variable combinations of gas, liquid water, and mineral cements. Measured Vs in the upper crust (0–8 km) can be explained by layers of minimally (<2%) cemented sediments and gas‐filled fractured basalts. Measured Vs in the deeper crust (8–20 km) can be explained by fractured basalts or more felsic igneous rocks (modeled here as 100% plagioclase feldspar) that is unfractured or has up to 23% porosity. Open pores in the deeper crust could host gas, liquid water, and up to 2% cement. Modeled Vs are too low for a seismically detectable ice‐saturated cryosphere in the upper crust and temperatures are too high to freeze liquid water in the deeper crust. Notably, with Vs alone, we are unable to distinguish between liquid water and gas within the pores. Plain Language Summary: Liquid water may have existed on Mars as oceans, rivers, or ground water. Surface water was likely lost to space, buried as liquid water and ice, and/or incorporated in subsurface minerals and mineral cements. The InSight lander on Mars has a seismometer whose measurements can be used to estimate the velocity of seismic shear waves. Seismic velocities change based on rock type and the material that fills the pores within rocks (e.g., liquid water, gas, or ice and other mineral cements). We show that the measured seismic velocities in the upper (0–8 km) crust can be explained by layers of gas‐filled basalts and minimally (2%) cemented sediments rather than ice‐filled sediment or basalt. Measured seismic velocities in a deeper (8–20 km) crust can be explained by fractured basalt. More feldspar‐rich rocks could explain the velocities in the deeper crust and they could be unfractured or have up to 23% porosity. Fractures within the deeper crust could host liquid water, gas, and up to a couple percent of mineral cements. Key Points: Mars' upper crust (0–8 km) beneath Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport mission (InSight) comprises fractured gas‐filled rocks and weakly cemented sedimentsMars' deeper crust (8–20 km) beneath InSight could comprise fractured basalts or more‐felsic igneous rocks with 0%–23% porosityNo seismically detectable cryosphere exists in the crust and pores in the deeper crust host gas, liquid water, or up to 2% cement [ABSTRACT FROM AUTHOR]

A North/South difference in crustal thickness is likely at the origin of the Martian dichotomy in topography. Recent crustal thickness maps were obtained by inversion of topography and gravity data seismically anchored at the InSight station. On average, the Martian crust is 51–71 km thick with a southern crust thicker by 18–28 km than the northern one. The origin of this crustal dichotomy is still debated although the hypothesis of a large impact is at present very popular. Here, we propose a new mechanism for the formation of this dichotomy that involves a positive feedback between crustal growth and mantle melting. As the crust is enriched in heat‐producing elements, the lid of a one‐plate planet is hotter and thinner where the crust is thicker, inducing a larger amount of partial melt below the lid and hence a larger rate of melt extraction and crustal growth. We first demonstrate analytically that larger wavelength perturbations, that is, hemispherical perturbations, grow faster because smaller wavelengths are more attenuated by thermal diffusion. We then use a parameterized thermal evolution model with a well‐mixed mantle topped by two different lids characterized by their thermal structures and thicknesses to study the growth of the crust in the two hemispheres. Our results demonstrate that this positive feedback can generate a significant crustal dichotomy. Plain Language Summary: The dichotomy is the most noticeable feature of the Martian surface. The highest elevations in the South are likely due to a larger crustal thickness than in the North, as is the case on Earth below mountain belts. This difference in thickness was recently constrained by the Insight mission. We show here that a positive feedback between crustal thickening and mantle melting could have generated this dichotomy. Indeed, as the crust is enriched in heat‐producing elements, the temperature profile is warmer where the crust is thicker. This results in hotter rocks at lower pressures leading to more melting, and therefore more melt extraction and crustal thickening beneath thicker crustal regions. Since lateral heat diffusion tends to attenuate short wavelength perturbations, the longest wavelengths, that is, hemispherical perturbation, will grow the fastest. In this study, we develop a thermal evolution model that takes into account the extraction of the crust in two different hemispheres. Our results show that small initial perturbations can generate large differences in crustal thickness. This mechanism alone could explain the dichotomy in crustal thickness; it would also act to significantly amplify an initial dichotomy generated by another mechanism such as a large impact or a degree‐one mantle convection. Key Points: On one‐plate planets, regions of thicker crusts are hotter leading to a positive feedback mechanism between crust growth and melt extractionThis mechanism is favored at larger wavelengths because smaller wavelengths are more attenuated by lateral thermal diffusionThis mechanism can explain the hemispheric difference in thickness of the Martian crust [ABSTRACT FROM AUTHOR]

Anxiety is one of the most common and debilitating mental health disorders, and is related to changes in interoception (perception of bodily states). While anxiety is more prevalent in women than men, gender differences in interoception-anxiety associations are often overlooked. Here, we examined gender-specific relationships between anxiety and interoception in the breathing domain, utilising multicentre data pooled from four study sites (N = 175; 51% women). State anxiety scores were quantified via the Spielberger State-Trait Anxiety Inventory, and breathing-related interoceptive dimensions via an inspiratory load task to quantify sensitivity, decision bias, metacognitive bias (confidence in interoceptive decisions), and metacognitive insight (congruency between performance and confidence). Regression analyses revealed a significant negative relationship between state anxiety and metacognitive bias (β = -0.28; p = 0.01) and insight (β = -0.09; 95% highest density interval [HDI] in a hierarchical Bayesian regression = [-0.18, -0.004]) across the whole sample, while state anxiety did not relate to interoceptive sensitivity nor decision bias. While no mean interoceptive effects relating to gender were observed, the relationship between anxiety and metacognitive insight towards breathing was driven by women (women: β = -0.18; HDI = [-0.31, -0.05]; men: β = 0.02; HDI = [-0.12, 0.15]) with a significant interaction effect (β difference = -0.20; HDI = [-0.37, -0.01]), which did not hold for trait anxiety nor depression measures. In summary, state anxiety was associated with decreased metacognitive bias across all participants, while decreased interoceptive insight was only associated with anxiety in women but not men. Therefore, treatment programmes focusing on interoceptive metacognitive bias may be useful for all anxiety patients, while interoceptive insight might represent a specific treatment target for women with anxiety., (© 2025 The Author(s). European Journal of Neuroscience published by Federation of European Neuroscience Societies and John Wiley & Sons Ltd.)

The dual‐process theory that two different systems of thought coexist in creative thinking has attracted considerable attention. In the field of creative thinking, divergent thinking (DT) is the ability to produce multiple solutions to open‐ended problems in a short time. It is mainly considered an associative and fast process. Meanwhile, insight, the new and unexpected comprehension of close‐ended problems, is frequently marked as a deliberate and time‐consuming thinking process requiring concentrated effort. Previous research has been dedicated to revealing their separate neural mechanisms, while few studies have compared their differences and similarities at the brain level. Therefore, the current study applied Activation Likelihood Estimation to decipher common and distinctive neural pathways that potentially underlie DT and insight. We selected 27 DT studies and 30 insight studies for retrospective meta‐analyses. Initially, two single analyses with follow‐up contrast and conjunction analyses were performed. The single analyses showed that DT mainly involved the inferior parietal lobe (IPL), cuneus, and middle frontal gyrus (MFG), while the precentral gyrus, inferior frontal gyrus (IFG), parahippocampal gyrus (PG), amygdala (AMG), and superior parietal lobe were engaged in insight. Compared to insight, DT mainly led to greater activation in the IPL, the crucial part of the default mode network. However, insight caused more significant activation in regions related to executive control functions and emotional responses, such as the IFG, MFG, PG, and AMG. Notably, the conjunction analysis detected no overlapped areas between DT and insight. These neural findings implicate that various neurocognitive circuits may support DT and insight. [ABSTRACT FROM AUTHOR]

NASA's Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission records several high‐frequency (>0.5 Hz) dispersive seismic signals on Mars. These signals are due to the acoustic‐to‐seismic coupling of infrasound generated by the entry and impact of meteorites. This dispersion property is due to infrasound propagating in a structured atmosphere, and we refer to this dispersive infrasound as guided infrasound. We propose to model the propagation of guided infrasound and the seismic coupling to the ground analytically; we use a 1D layered atmosphere on a three‐layer solid subsurface medium. The synthetic ground movements fit the observed dispersive seismic signals well and the fitting indicates that the regolith beneath InSight is about 40‐m in thickness. We also examine and validate the previously‐published subsurface models derived from InSight ambient seismic vibration data. Plain Language Summary: Under particular weather conditions, the Martian atmosphere displays a special sound‐wave velocity profile, where the wave velocity becomes larger with increasing altitude within a few hundred meters. When an infrasound signal—a low‐frequency (<20 Hz) sound wave inaudible to humans—propagates through such a structure, the infrasound exhibits dispersion: its propagation velocity depends on its frequency. We refer to such infrasound as guided infrasound. Guided infrasound can deform the ground, and have been recorded by the seismometer of NASA's Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission on the Martian surface. We propose to model these recordings using the physics of sound waves traveling above a compliant solid ground. We show that our modeling results can fit well the seismic recordings of guided infrasound on Mars. We apply our modeling to the subsurface models from a different InSight seismic observation to check if these models can explain our seismic recordings. This modeling constitutes a new tool to investigate the subsurface structure of Mars, and is also useful for the investigation of Titan and Venus. Key Points: We analytically compute the dispersion relationship of guided infrasound in 1D atmospheric models from Mars and EarthWe model the ground response to guided infrasound to fit the corresponding seismic observation due to meteorite impacts on MarsWe utilize the seismic recording due to guided infrasound to constrain the subsurface structures [ABSTRACT FROM AUTHOR]

Purpose: It is important to investigate the negative factors affecting medication compliance to continue the treatment of schizophrenia. Design and Methods: In this descriptive and analytical study, the effects of insight, loneliness, and hope levels on medication adherence in 202 patients with schizophrenia were studied. Findings: The correlation was positive between medication adherence and insight, negative between medication adherence and loneliness, and no correlation between medication adherence and hope. A 1‐point increase in insight scores increased medication adherence 1.226 times and a 1‐point increase in loneliness scores decreased medication adherence 0.946 times. Medication adherence was 0.499 times lower in nonsmokers compared to smokers. Practice Implications: Further studies on patients with schizophrenia should be conducted to evaluate factors affecting medication adherence and preventing smoking in schizophrenia. [ABSTRACT FROM AUTHOR]

Utilizing low‐frequency events reported by the Marsquake Service (MQS), we selected waveform data collected from the InSight mission to characterize the origins of three potential marsquakes. S0173a and S0235b were determined to originate near the Cerberus Fossae region. Our calculated backazimuths and epicentral distances were in agreement with those provided by the InSight team. The third event, S0325ab, likely originated southeast of the lander with an epicentral distance of 38.4°, uniquely placing it near the boundary between the Martian highlands and lowlands. We then estimated potential double‐couple faulting mechanisms associated with each of the marsquakes using the relative amplitudes and polarities of the P, SH, and SV waves, in a novel method. S0173a and S0173ab can be explained with a composite mechanism that begins as a thrust faulting, followed by an oblique normal‐faulting mechanism. Given the low level of seismicity on Mars, it is likely that these events did not occur independently but instead form a doublet resulting from a single origin. Though its weaker, S0325a and S0325ab could also represent a doublet that begins with E‐W extension and ends with N‐S extension. Our preferred explanation for S0235b is a single faulting mechanism representing vertical dip‐slip with a small normal‐faulting component. The strike of one fault plane aligns roughly with the exposed faults that represent the Cerberus Fossae. We propose that these diverse faulting mechanisms from different locations represent intra‐crustal deformation in the form of volcano‐tectonic quakes related to magmatic activity, including possible dike propagation in the lower crust. Plain Language Summary: We investigated the data recorded by the first seismometer successfully installed on the surface of Mars, in order to better understand its geological activity and ways in which it is still changing. We analyzed signals from three prominent marsquakes to infer their epicenters and the type of slip that caused them. By comparing the unique properties of these marsquakes to the mechanisms we see on Earth, we attempted to characterize the ways in which Mars deforms. This project adapted methods used on Earth when seismic data is collected from a single station to tackle the difficult task of working with data from one seismometer on the Martian surface in an unfamiliar noise environment. Using this method, we were able to independently reproduce and provide additional details for the results published by the NASA InSight mission team. We find that seismic activity on Mars is not restricted to a single region and represents various faulting styles, sometimes occurring just a few seconds apart. We hypothesize that the analyzed marsquakes are induced by magmatic activity in the lower crust, near the crust‐mantle boundary. Key Points: Two estimated epicenters of three low‐frequency marsquakes are near Cerberus FossaeDiverse faulting mechanisms of marsquakes are estimated from single‐station relative body wave amplitudes, using a novel misfit definitionThe origins of the analyzed marsquakes may be volcano‐tectonic, related to magmatic activity in the lower crust [ABSTRACT FROM AUTHOR]

Aim: We aimed to investigate whether gaining insight through psychoeducation for first‐episode schizophrenia is associated with increased suicidality. Methods: We conducted a secondary analysis of a prospective cohort study that included inpatients with first‐episode schizophrenia who attended a group psychoeducation program during their admission. The group psychoeducation program consisted of four weekly sessions provided by a multidisciplinary team. The primary outcome was the correlation between changes in insight and suicidality. We also examined whether change in insight was associated with changes in hopelessness and depression. We measured insight using the Birchwood Insight Scale. Suicidality, hopelessness and depression were measured using the Calgary Depression Rating Scale for Schizophrenia. Results: A total of 125 people participated in the educational program. The Spearman's correlation coefficient between changes in insight and suicidality was −0.14 (95% confidence interval, −0.31 to 0.04; p =.12). Similarly, gain in insight did not significantly correlate with change in depression (0.01, 95% confidence interval, −0.17 to 0.18; p =.93) and change in hopelessness (0.01, 95% confidence interval, −0.16 to 0.19; p =.88). Conclusions: We observed almost no association between gaining insight and suicidality after a group psychoeducation program in inpatients with first‐episode schizophrenia. [ABSTRACT FROM AUTHOR]

This paper explores insight and the development of the thinking voice in the psychoanalytic process. It begins with music and images, narrating an important Australian historical event. The composers have created a dreaming space, and for this paper, a metaphor for the analytic space and the creative process. At once physical, aural and visual, it also exists within and reflects the patient's and analyst's shared historical and cultural frame. It is a liminal space, for exploration, crossing, and a product of the alchemy created between patient and analyst. Pickering's (2016) and Grier's (2019) consideration of musicality as an essential part of the analytic experience assists recognition of the multidimensional nature of the space created between patient and analyst. Ferro and Civitarese's (2015) conceptualization of the space where patient and analyst dream one another, and Baranger and Baranger's (2008) discussion of the bi personal field are pertinent here. Symington's idea of insight as an essential 'thing in itself', within the individual patient helps articulation of insight as a product of an internalized linking, or parental intercourse, enabling movement to a separate third position. [ABSTRACT FROM AUTHOR]

Kruger and Dunning (1999) described a metacognitive bias in which insight into performance is linked to competence: poorer performers are less aware of their mistakes than better performers. Competence‐based insight has been argued to apply generally across task domains, including a recent report investigating social cognition using a variety of face‐matching tasks. Problematically, serious statistical and methodological criticisms have been directed against the traditional method of analysis used by researchers in this field. Here, we further illustrate these issues and investigate new sources of insight within unfamiliar face matching. Over two experiments (total N = 1077), where Experiment 2 was a preregistered replication of the key findings from Experiment 1, we found that insight into performance was multi‐faceted. Participants demonstrated insight which was not based on competence, in the form of accurate updating of estimated performance. We also found evidence of insight which was based on competence: the difference in confidence on correct versus incorrect trials increased with competence. By providing ways that we can move beyond problematic, traditional approaches, we have begun to reveal a more realistic story regarding the nature of insight into face perception. [ABSTRACT FROM AUTHOR]

Aim: This study aims to evaluate the disability, insight and self‐care agency of schizophrenia patients. Design and Method: This descriptive study was conducted with 100 patients in remission who had a diagnosis of schizophrenia at community mental health centers. Results: The schizophrenia patients had poor insight and moderate self‐care agency. The self‐care agency of schizophrenia patients is a neglected issue in medicine, and is associated with positive and negative symptoms, insight and disability. Implementation Results: The results can guide community mental health center nurses to increase the quality of life of schizophrenia patients in remission and to help reintegrate them into society. [ABSTRACT FROM AUTHOR]

Insight and intuition are important concepts in creativity research and creative behavior with applications in a wide variety of professional and business domains. Understanding and articulating their similarities and differences is important theoretically and practically. Researchers and practitioners can benefit from the application of new techniques which can distinguish between these two phenomena based on individuals' subjective experiences as articulated in written or spoken accounts. Subtle language cues provide objective, quantifiable data (linguistic markers) to identify and analyze a variety of cognitive and affective psychological processes. Computer‐assisted text analysis (CATA) based on the theory of natural language use offers researchers a systematic and objective framework for extracting and interpreting such markers. This Brief Report proposes the use of CATA for the identification of the linguistic markers of insight and intuition and outlines ways in which the method could be applied in future research. Using CATA, it was possible to identify a preliminary set of linguistic markers which could be used to distinguish between insight and intuition. [ABSTRACT FROM AUTHOR]

Aim: To investigate correlates of insight dimensions in Chinese adult patients with early psychosis. Methods: Insight dimensions including awareness of mental disorder (AMD), illness consequences (AIC) and medication effect (AME) were measured. A wide array of variables encompassing demographics, premorbid adjustment, onset profiles, symptomatology, treatment characteristics and psychological factors were comprehensively assessed. Results: Of 130 participants, 53.1%, 47.7% and 56.2% were categorized with good AMD, AIC and AME, respectively. Good AMD was associated with female gender, fewer positive and disorganization symptoms, more severe depression and greater self‐stigma. Good AIC was related to female gender, more severe depression and greater self‐stigma. Younger age of onset, fewer positive symptoms and greater service satisfaction associated with good AME. Conclusions: Poor insight is prevalent in early psychosis. Differential relationships of insight dimensions with other illness variables underscore the importance of multidimensional approach in insight evaluation, and suggest potential treatment target for insight enhancement. [ABSTRACT FROM AUTHOR]

A high‐sensitivity pressure sensor was deployed as part of the Mars Interior Exploration using Seismic Investigations, Geodesy and Heat Transport lander on Elysium Planitia in November 2018. We use pressure records from 1 October to 31 December 2019 (Sol 301–389) for frequencies between 0.1 and 0.5 Hz to infer relative sound‐speed changes in the Martian atmosphere using the autocorrelation infrasound interferometry method. We find that relative sound‐speed changes are up to ±15%, follow a similar pattern to Martian‐daily variations of atmospheric temperature and horizontal wind velocity, and are similar to those inferred from in‐situ observations and Martian climatology. The relative sound‐speed changes and horizontal wind speed variations are synchronous, while temperature peaks ∼1.88 hr after these time series. The strong and continuous emergence of coherent phases in the autocorrelation codas suggests the presence of continuous infrasound on Mars. Plain Language Summary: We study the Martian atmosphere using the pressure data collected by the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) lander. We apply a novel method to determine relative changes of sound‐speed, which in turn are related to changes in wind velocity and atmospheric temperature. Compared to Earth, Mars daily variations of sound‐speed are ∼10 times larger and the attenuation of acoustic waves is ∼2 orders of magnitude higher. Nevertheless, inferred relative sound‐speed changes are highly similar to temperature and horizontal wind velocity time series. Our analysis also indicates that the pressure sensor onboard the InSight lander samples a persistent background acoustic signal, which permits continuous monitoring of the highly variable Martian atmosphere. Key Points: Autocorrelation infrasound interferometry retrieves relative sound‐speed changes from the pressure data recorded by the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport landerIn the Martian atmosphere, the relative sound‐speed changes are up to ±15% and follow a similar trend to temperature and wind velocityPersistent emergence of coherent phases in the autocorrelation codas suggests the presence of continuous infrasound on Mars [ABSTRACT FROM AUTHOR]

Objectives: Awareness of difficulties shown by people with dementia is known to vary, but few studies have explored changes in awareness over time. Investigating this could further the understanding of surrounding concepts and reasons for impaired awareness. Recognising emerging or diminishing awareness could facilitate discussions about diagnosis and appropriate post-diagnostic support.Methods: Using longitudinal data from the Improving the experience of Dementia and Enhancing Active Life (IDEAL) cohort, awareness in community-dwelling people with mild-to-moderate dementia was assessed at three timepoints over 2 years. A validated checklist was used to evaluate awareness of difficulties associated with dementia. We examined changes in awareness for people with low awareness at baseline, and used case-matching to describe differences in characteristics between people who gained awareness, and those who continued with low awareness.Results: At baseline, 83 people from a sample of 917 showed low awareness. The majority of those remaining in the study at later timepoints had gained awareness, some as late as four or more years after diagnosis. Case-matched comparisons revealed few distinguishing characteristics: cases with stable low awareness had similar or better cognitive and functional ability than those who gained and retained awareness at 12 and 24 months, but may have had more co-morbidities.Conclusions: Self-reported awareness of difficulties can change and may increase over time in people with mild-to-moderate dementia. There may be individual reasons for ongoing low awareness, not explained by cognitive or functional ability. This challenges the view that a single record of low awareness represents a fixed disease-related symptom, and highlights the complex, individual and dynamic nature of awareness. [ABSTRACT FROM AUTHOR]

The InSight lander rests on a regolith‐covered, Hesperian to Early Amazonian lava plain in Elysium Planitia within a ∼27‐m‐diameter, degraded impact crater called Homestead hollow. The km to cm‐scale stratigraphy beneath the lander is relevant to the mission's geophysical investigations. Geologic mapping and crater statistics indicate that ∼170 m of mostly Hesperian to Early Amazonian basaltic lavas are underlain by Noachian to Early Hesperian (∼3.6 Ga) materials of possible sedimentary origin. Up to ∼140 m of this volcanic resurfacing occurred in the Early Amazonian at 1.7 Ga, accounting for removal of craters ≤700 m in diameter. Seismic data however, suggest a clastic horizon that interrupts the volcanic sequence between depths of ∼30 and ∼75 m. Meter‐scale stratigraphy beneath the lander is constrained by local and regional regolith thickness estimates that indicate up to 10–30 m of coarse‐grained, brecciated regolith that fines upwards to a ∼3 m thick loosely‐consolidated, sand‐dominated unit. The maximum depth of Homestead hollow, at ∼3 m, indicates that the crater is entirely embedded in regolith. The hollow is filled by sand‐size eolian sediments, with contributions from sand to cobble‐size slope debris, and sand to cobble‐size ejecta. Lander‐based observations indicate that the fill at Homestead hollow contains a cohesive layer down to ∼10–20 cm depth that is visible in lander rocket‐excavated pits and the HP3 mole hole. The surface of the landing site is capped by a ∼1 to 2 cm‐thick loosely granular, sand‐sized layer with a microns‐thick surficial dust horizon. Plain Language Summary: The InSight lander has geophysical instruments that are designed to determine the interior structure of Mars. Understanding the results from these instruments requires a geological analysis of materials beneath the landing site at Elysium Planitia. This study presents data that describe the vertical sequence of rocks and soils beneath the lander, as well as the geologic history. The results indicate that InSight rests on a 1.7‐billion‐year‐old lava plain that is covered in a 10–30 m thick regolith that was produced by impact cratering and modified by wind. The uppermost portion of the regolith is a ∼3 m thick horizon of sand. InSight rests on sand within a degraded impact crater. The sandy material contains a slightly cohesive horizon that is only ∼1–2 cm beneath the lander and is up to 10–20 cm thick. The sandy horizon overlies rock fragments that get progressively larger with depth. Bedrock of basaltic lava exists beneath the regolith down to a depth of ∼170 m. The bedrock is interrupted by weaker materials between depths of ∼30 and 75 m. Beneath ∼170 m, the sequence is dominated by ancient (3.7–4.1 billion years old), possibly sedimentary materials. Key Points: InSight rests on Early Amazonian basaltic lava with an up to 10–30 m thick regolith. The upper 3 m of the regolith is sand dominatedThe regolith contains a 10–20 cm thick cohesive horizon or duricrust. This horizon rests 1–2 cm beneath the landerThe upper 1–2 cm of the regolith comprises loosely‐consolidated sand to pebbles. Sand is rarely mobilized under current wind conditions [ABSTRACT FROM AUTHOR]

Background: We conducted a historical cohort study of patients with schizophrenia to identify more robust risk factors at discharge that contribute to readmission within a year. Methods and Findings: The subjects underwent brief psychoeducation during hospitalization. Multivariate analysis was conducted using factors selected in the univariate analysis. Using logistic regression analysis, the number of hospital admissions (P =.01) and Schedule for Assessment of Insight Japanese version score (P =.04) were identified as risk factors for readmission, with odds ratios of 0.70 and 1.18, respectively. Conclusions: These results suggest that improvement in insight and early intervention may lead to a more stable community life. [ABSTRACT FROM AUTHOR]