Investigating ejecta plume and tail of (65803) Didymos binary system

Data acquired by spaceborne spectrometers operating in the visual (VIS) and near-infrared (NIR) spectral ranges, are commonly exploited to derive the microphysical properties of planetary atmospheric aerosols (e.g. Adriani et al., 2015; Sindoni et al., 2017; Fedorova et al., 2024; Oliva et al., 2016; Oliva et al., 2018; D’Aversa et al., 2022). The precision with which these properties can be constrained, depends on several parameters (e.g. optical constants, surface albedo spectrum, particles’ shape and size distribution, ecc.) and on the spectral information content in the data. VIS wavelengths alone (~ 0,4 – 0,7 μm) provide information on aerosols’ composition, particles’ density and sizes, allowing the estimation of the optical depth integrated along the line of sight (Oliva et al., 2016). However, in order to constrain these parameters with enhanced precision, the NIR range (~ 0,7 – 3,0 μm) is also required, since it allows to assess how the spectral shape bends towards longer wavelengths (Oliva et al., 2018).Our goal is to exploit the combined nadir datasets of the UVIS (0.2 – 0.65 µm) and LNO (2.2 – 3.8 µm) channels of the NOMAD spectrometer (Neefs et al., 2015) to contrain the microphysical properties of Martian dust (Oliva et al., 2025). The two spectral ranges present a large gap among each other, and this introduces biases in the retrieved parameters due to the unconstrained spectral information in the missing wavelengths. In order to benchmark these biases, we exploit MEx/OMEGA (Bibring et al., 2004) VNIR (0,35 – 1,05 µm) and SWIR-C (0.93 - 2.73 µm) channels’ data. Such an extended interval allows the retrieval of Martian dust clouds’ height and microphysical properties (e.g. Oliva et al., 2018; D’Aversa et al., 2022), that can be used as a proxy for the NOMAD retrievals. By studying dust’s densities and sizes 1) from the full OMEGA spectrum and 2) from the spectrum only covering UVIS and LNO wavelengths, we can derive the bias in the retrieved parameters. Moreover, this analysis allows to calibrate how many UVIS and LNO spectral points need to be considered in the retrieval, in order to balance the information content of the two channels.Preliminary results suggest that dust densities are systematically overestimated (as well as grains’ sizes to a lesser degree) if NIR wavelengths are completely neglected, while such a bias is reduced if LNO range is taken into account.ReferencesAdriani et al., 2015. Faint luminescent Ring over Saturn’s polar hexagon. Astrophys. J. Lett. 808 (1), 5. L16.Bibring et al., 2004. Omega: Observatoire pour La minéralogie, l’eau, Les Glaces Et l’activité. ESA SP-1240: Mars Express: The Scientific Payload. ESA Publications Division, Estec, Noordwijk, The Netherlands, pp. 37–49.D’Aversa et al., 2022. Vertical distribution of dust in the Martian atmosphere: OMEGA/Mex limb observations. Icarus 371, 114702.Fedorova et al., 2024. Distribution of atmospheric aerosols during the 2007 Mars dust storm (MY 28): Solar infrared occultation observations by SPICAM. Icarus 415, 116030Oliva et al., 2016. Clouds and hazes vertical structure of a Saturn’s giant vortex from Cassini/VIMS-V data analysis. Icarus 278, 215–237.Oliva et al., 2018. Properties of a Martian local dust storm in Atlantis Chaos from OMEGA/MEX data. Icarus.Oliva et al., 2025. Martian dust characterization: reanalysis of TGO/NOMAD UVIS and LNO channels’ nadir data. XX Congresso Nazionale di Scienze Planetarie, Pescara, 3-7 Febbraio 2025.Neefs et al, 2015. NOMAD spectrometer on the ExoMars trace gas orbiter mission: part 1—design, manufacturing and testing of the infrared channelsApplied Optics 54, 28, 8494-8520.Sindoni et al., 2017. Characterization of the white ovals on Jupiter’s southern hemisphere using the first data by the Juno/JIRAM instrument. Geophys. Res. Lett. https://doi.org/10.1002/2017gl072940.AcknowledgementsExoMars is a space mission of the European Space Agency (ESA) and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB- BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/V002295/1, ST/V005332/1, ST/Y000234/1 and ST/X006549/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique – FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and BELSPO BrainBe SCOOP Project. US investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canada Space Agency.

A dynamic category of asteroids, known as near-Earth asteroids, includes a group of potentially hazardous asteroids (PHAs) with orbits that have an increased likelihood of colliding with Earth. One effective strategy to avert such collisions involves deflecting a PHA, ensuring it deviates from a collision course with Earth. Calculations have demonstrated that one promising deflection method is the kinetic mitigation approach, wherein a rapidly moving human-made object impacts the PHA, deflecting it from the collision course. The Double Asteroid Redirection Test (DART) mission, led by NASA’s Planetary Defense Coordination Office, was specifically designed to assess the kinetic mitigation method. It impacted the moon in the binary asteroid system (65803) Didymos. The mission would be considered successful if the DART kinetic impact caused at least a 73-second change in the binary orbital period, measured with an accuracy of 7.3 seconds. The mission objectives also included measuring the efficiency of momentum transfer to Didymos’s moon, Dimorphos, by estimating the momentum enhancement factor β, determining the location and surface characteristics of the spacecraft impact site, and assessing the dynamical changes in the Didymos system resulting from the DART impact. Launched on November 24, 2021, the DART spacecraft impacted Dimorphos on September 26, 2022. A CubeSat named LICIACube (Light Italian CubeSat for Imaging of Asteroids), supplied by Agenzia Spaziale Italiana, separated from the DART spacecraft 15 days before the impact. LICIACube provided crucial information about the initial minutes following the impact. A network of ground-based and space-based telescopes also monitored the Didymos system. The mission results demonstrated the high efficiency of the kinetic mitigation method, with the impact altering the binary orbital period by −33.24 minutes, determined with an accuracy of less than 2 seconds. The enhancement factor β was estimated to be between 2.4 and 4.9 (the range resulting from different estimations of Dimorphos’s mass), thus significantly exceeding the minimal estimated value equal to unity. The mission yielded valuable information about impact dynamics and the formation of impact ejecta, as well as about the shapes, surface, and interior characteristics of asteroids in binary systems and small asteroids in general. Extensive spectral, photometric, and polarimetric observations by telescopes on Earth and in space allowed for the characterization of dust in the impact ejecta and its long-term evolution, as well as physical changes in the Didymos system. Remaining gaps in understanding DART’s kinetic impact consequences are slated to be addressed by the European Space Agency’s Hera mission, scheduled for launch in 2024.

DIDYMOS AT DIFFERENT ROTATIONAL PHASES: a subtle but persistent spectral variability

NASA’s Double Asteroid Redirection Test (DART) is designed to be the first demonstration of a kinetic impactor for planetary defense against a small body impact hazard. The target is the smaller component of the Didymos-Dimorphos binary asteroid system. The DART impact will abruptly change the relative velocity of the secondary (Dimorphos), increasing the binary eccentricity and exciting librations in the secondary. The observed change in the binary orbit period will be used to infer the “beta factor”, or the momentum transfer efficiency, an important parameter used in planetary defense. The post-impact spin and librational dynamics are expected to be highly dependent on the momentum transferred to the target (i.e., beta) and the shape of the secondary, which is still unconstrained.In this work, we explore the possible post-impact spin state of Dimorphos, as a function of its shape and beta, assuming it has an ellipsoidal shape and that both bodies have a uniform density. We have conducted attitude dynamics simulations with a modified 3-D spin-orbit model, accounting for the secondary’s shape and the primary’s oblateness, to understand the underlying dynamical structure of the system. In addition, we have used the radar-derived polyhedral shape model of Didymos in high-fidelity Full Rigid Two-Body Problem (FR2BP) simulations to capture the fully three-dimensional nature of the problem. We consider the outcomes from a simplified planar impact, where the DART momentum is transferred within the binary orbit plane, opposite the motion of Dimorphos, in addition to a more realistic case that accounts for the full DART velocity vector (which contains out-of-plane components).With both simulation tools, we produce the expected signatures of the 1:1 and 2:1 secondary resonances between the free and forced libration periods, corresponding to axial ratios of a/b = 1.414 and a/b = 1.087, respectively. For moderate values of beta (~3), we find that the libration amplitude can exceed ~40 degrees in most cases. For some possible axial ratios, it is even possible to achieve a libration amplitude exceeding 40 degrees with beta values as low as 1. In addition, both codes reveal that the secondary may be attitude unstable in many cases, and can enter a chaotic tumbling state for larger values of beta (~5). In some cases, Dimorphos is able to break from its assumed 1:1 spin-orbit resonance.In the case with a more realistic impact geometry (where some momentum is transferred out-of-plane), the results are relatively similar. The most noticeable difference is in the cases that result in a chaotic tumbling state. In those cases, the characteristic timescale for entering the chaotic tumbling state is much shorter – typically only several orbit periods are required. We also discuss the feasibility of detecting the post-impact spin state of Dimorphos with ground-based observations.This study was supported in part by the DART mission, NASA Contract # NNN06AA01C to JHU/APL. The work of K.T. and I.G. is supported by the EC Horizon 2020 research and innovation programme, under grant agreement No. 870377 (project "NEO-MAPP"). Some of the simulations herein were carried out on The University of Maryland Astronomy Department’s YORP cluster, administered by the Center for Theory and Computation.

Introduction: NASA’s Double Asteroid Redirection Test (DART) aims to test a controlled deflection of a Near-Earth asteroid, by impacting the smaller component of the 65803 Didymos asteroid system, Dimorphos. ESA’s Hera mission [1] will arrive at Dimorphos several years after the DART impact and will perform detailed characterisation of Dimorphos and of the impact outcome. Past studies of the DART impact outcome [e.g., 2–4] have shown that the amount by which Dimorphos can be deflected is strongly dependent on its surface, subsurface and internal properties. Moreover, [4] showed that in order to validate the predictive capabilities of our numerical models and to understand and ultimately reproduce the asteroid deflection technique, we need a measure of both the impact deflection efficiency (often referred to in terms of β, where β = change in momentum of the asteroid/impactor momentum) and the crater size and morphology. Small asteroids, of less than ~10 km in diameter, are believed to be rubble-pile objects, aggregates held together only by self-gravity or small cohesive forces [5]. Moreover, recent results of the SCI impact on Ryugu [6] inferred that at least the near-surface of the asteroid may not be dominated by strength and impact events are controlled to a large extent by gravity, despite its very low value. These findings might also be applicable to Dimorphos. Studies by [7] suggest that for a low cohesion target, an impact on the same magnitude as DART might have a large enough specific impact energy to cause global deformation of the target. Here we numerically simulate DART-like impacts on weak homogeneous and rubble-pile asteroids that use realistic material models and aim to evaluate the resulting target morphology and the global shape change caused by such impacts. Additionally, we aim to quantify the deflection efficiency, given different target scenarios.Numerical Model: Here we use Bern’s parallel Smooth Particle Hydrodynamics (SPH) impact code [8, 9] to model DART-like impacts (500 kg projectiles at 6 km/s) on spherical asteroid targets, and track the evolution of the target for up to 2 hours after the impact. Bern’s SPH code has been previously validated against laboratory experiments and benchmarked against other codes [e.g., 10, 11]. Recently, the code has been validated against laboratory experiments of impacts into heterogeneous targets [12]. To quantify the effects of the target properties and structures on the post-impact morphology, degree of shape change and on the momentum transfer efficiency, we considered the following target scenarios: 1) Homogeneous spherical targets with low cohesion (Y0 = 0 to 50 Pa) and varying coefficient of internal friction (f = 0.4 to 1.0); To describe the shear response, the target material was modelled using a simple pressure-dependent strength model typical of pre-damaged rock materials [13]. The initial target porosity was kept constant at 40%. 2) Rubble-pile spherical targets with three different distributions of boulders, embedded into a cohesionless matrix material: 2a) grid distribution of 2.5 m in diameter boulders, with one boulder diameter spacing between each boulder in the x, y, and z directions; 2b) random distribution of 2.5 m boulders; 2c) Random distribution of boulders with random sizes between 2 and 10 m. In all rubble-pile target scenarios, the boulders had a tensile strength of YT = 1 MPa and the matrix material was modelled the same as in (1), with Y0 = 0 Pa and f = 0.6.Results and discussion:Homogeneous asteroids: The size and morphology of the DART crater is of paramount importance for determining the asteroid’s near-surface properties and structure. In the strength dominated impact scenarios, the cohesion is the dominant force that stops the crater cavity from growing. Therefore, with decreasing target cohesion, more material is displaced or gets ejected above escape speed. We found that for homogeneous asteroids, impacts into targets stronger than Y0~10 Pa create well defined bowl-shaped craters, while impacts into weaker targets create morphologies that do not resemble an impact crater anymore (e.g., Fig. 2, [14]). For these scenarios the curvature of the target also plays a major role. Fig. 1 shows the momentum enhancement factor, β, as a function of target cohesion, for four different coefficients of internal friction. Our results suggest that for a low friction, cohesionless target, the momentum enhancement can be as high as 6. Rubble-pile asteroids: Fig. 2 shows the final target morphologies from DART-like impacts into a (1) cohesionless homogeneous target and (2a, b, c) rubble-pile targets with different boulder size-frequency distributions. In all four impact scenarios, the DART impact produced target morphologies that are dissimilar to cratering and changed the global morphology of the asteroid. Initial simulation results revealed that the presence of boulders in the target can decrease the deflection efficiency by up to 40% compared to an impact into a homogeneous target. At the same time, the initial boulder size-frequency distribution on the surface of the asteroid seems to also influence β. Conclusions: The DART impact on cohesionless spherical bodies is likely to produce morphologies that are dissimilar to cratering and change the global morphology of the asteroid. Our modelling results together with future Hera mission observations will provide constraints regarding the evolution of the shapes and structures of small asteroids. Future work will investigate impact events into low-cohesion asteroids with more diverse asteroid shapes and boulder distributions. Acknowledgements: This work has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 870377.

Near-earth asteroid (66391) Moshup (1999 KW4) observing campaign: Results from a global planetary defense characterization exercise

Radar observations and a physical model of binary near-Earth asteroid 65803 Didymos, target of the DART mission

The Hera mission has been approved for development and launch in the new ESA Space Safety Programme by the ESA Council at Ministerial Level, Space19+, in November 2019. Hera will both offer a high science return and contribute to the first deflection test of an asteroid, in the framework of the international NASA- and ESA-supported Asteroid Impact and Deflection Assessment (AIDA) collaboration.The impact of the NASA DART (Doube Asteroid Redirection Test) spacecraft on the natural satellite of Didymos in October 2022 will change its orbital period around Didymos. As Didymos is an eclipsing binary, and close to the Earth on this date, the change can be detected by Earth-based observers. ESA’s Hera spacecraft will rendezvous Didymos four years after the impact. Hera’s instruments will perform the measurements necessary to understand the effect of the DART impact on Didymos’ secondary, in particular its mass, its internal structure, the direct determination of the momentum transfer and the detailed characterization of the crater left by DART. This new knowledge will also provide unique information on many current issues in asteroid science.From small asteroid internal and surface structures, through rubble-pile evolution, impact cratering physics, to the long-term effects of space weathering in the inner Solar System, Hera will have a major impact on many fields. For instance, collisions play a fundamental role in our Solar System history, from planet formation by collisional accretion to cratering of solid surfaces and asteroid family formation by collisional disruption. The fully documented hypervelocity impact experiment provided by DART and Hera will feed collisional models with information obtained at actual asteroid scale and for an impact speed (~6 km/s) that is close to the average impact speed between asteroids in the main belt. Moreover, Hera will perform the first rendezvous with an asteroid binary, characterize the smallest object ever visited (165 m in diameter) and provide the first direct measurement of an asteroid interior. Additionally, studies using Hera data will in turn affect our understanding of the asteroid population as a whole. The scientific legacy of the Hera mission will extend far beyond the core aims of planetary defense.Acknowledgment: The authors acknowledge funding support from ESA and from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 870377 (project NEO-MAPP), from the European Space Agency and from the French space agency CNES.

Space Qualification is a vital component of successful spacecraft design. The entire scope of the space qualification process is extremely large. This thesis will focus primarily on the Attitude Control System and Space Environment model, with the intent of furthering the verification of the design for the Joint Australian Engineering Satellite (JAESAT). The Attitude Control System proposed for use aboard JAESAT is a combination of permanent magnets with hysteresis rod damping. This system has proved effective on many previous satellite missions, however analysis must be undertaken to optimise the control provided for the individual design proposed. The Space Environment will affect the operation of many of the subsystems aboard JAESAT. Knowledge of the magnitude of such affects is essential to prevent complications through improved design. To do this requires an accurate model of the Space Environment local to JAESAT. Several models for different environmental characteristics are presented as part of this dissertation. Further detailed modelling was performed using the Space Environment Information System, an online software package provided by the European Space Agency. Some of the many results that have been obtained from the Space Environment Information System are presented in graphical format. A detailed model of the Attitude Control System was constructed using Matlab. The environmental disturbance torques were calculated using the environmental conditions previously modelled. Several simulations were conducted yielding mixed results. Generally, it was found that a permanent magnet strength of 14 A.m2 and spin rate of 0.4 revolutions per minute is sufficient to control JAESAT to within 1° of the magnetic field vector. Numerical simulation of the hysteresis rod damping however, has been shown to be ineffective and additional testing is required to successfully implement the hysteresis effects in the system simulation. An analysis of the model revealed that there were minimal sources of error present in the simulation process. The only significant source of error was due to the numerical integration of the equations associated with the satellite motion. Another possible source of model inaccuracy was due to the variation between the numerically simulated space environment and the actual space environment. This dissimilarity however, will only result in small changes of satellite orientation and will not have any effect on the satellite attitude. In the future, the Space Environment and Attitude Control System model that was constructed should be updated to reflect any changes in satellite design and orbit parameters. Simulations of the final Attitude Control System hardware should also be conducted in order to show that adequate attitude control is maintained throughout a period of several orbits. The hysteresis rods should be tested in order to determine their damping properties, and can then be incorporated in the satellite attitude simulations. Based upon numerous simulation results and research, it was concluded that the Attitude Control System that has been proposed was sufficient to provide the required level of attitude control for JAESAT. The successful verification of the Attitude Control System operation implies that the system is Space Qualified. Exact specifications for the Attitude Control System hardware are dependant upon the satellite orbit and design requirements. The model of the space environment is also sufficiently accurate to use in the verification of other satellite systems.

Objective and description The primary objective for compiling this dataset was to create data on the topic of youth participation in international environmental negotiations. While current research concentrates on youth protests, especially with regards to climate change, the YouthEarth dataset produces data on youth participation in formal negotiation processes beyond climate governance by also including biodiversity and sustainable development as case studies. It traces the evolution of youth participation across time and negotiation processes. It also compiles metadata about the anonymized youth participants and their organizations. More precisely, the dataset contains all youth-related participations to international environmental conferences between 1993 and 2024. The international environmental conferences covered are the yearly UNFCCC COPs (from COP1 in 1995 to COP29 in 2024) and UN summits of the CSD (from CSD1 1993 to CSD20 in 2013) and HLPF (from HLPF1 in 2013 to HLPF12 in 2024), and the biannual CBD COPs (from COP1 in 1994 to COP16 in 2024). The dataset is made of in 1 .csv file that contains 2 sheets (YouthEarthDatabase; Parameters). The detailed description of the data is expected to be published soon in a peer-reviewed open access journal. Credit author statement Anaëlle Vergonjeanne: Conceptualization, investigation, data curation, formal analysis. Amandine Orsini: Conceptualization, methodology, investigation, supervision, project administration, funding acquisition. Yi hyun Kang: Data collection, conceptualization, methodology. Juan Felipe Duque: Data collection. Acknowledgement We acknowledge the financial support of the FRS-FNRS Fonds de la Recherche Scientifique – FNRS (Belgium National Fund for Research) under Grant n° T.0020.21 for the 4-year (2021-2024) PDR project “Youth Earth” (https://www.crespo.be/youth-earth/).

<p>The Earth’s outer radiation belt response to geospace disturbances is extremely variable spanning from a few hours to several months. In addition, the numerous physical mechanisms, which control this response, depend on the electron energy, the time-scale and the types of geospace disturbances. As a consequence, the various models that currently exist are either specialized, orbit-specific data-driven models, or sophisticated physics-based ones. In this paper we present a new approach for radiation belt modelling using Machine Learning methods driven solely by solar wind speed and pressure, Solar flux at 10.7 cm and the Russell-McPherron angle. We use Van Allen Probes data to train our model and show that it can successfully reproduce and predict the electron fluxes of the outer radiation belt in a broad energy (0.033–4.062 MeV) and L-shell (2.5–5.9) range and, moreover, it can capture the long-term modulation of the semi-annual variation. We also present validation studies of the model’s performance using data from other missions which are outside the spatio-temporal training regime such as the E>0.8 MeV electron flux measurements from GOES-15/EPEAD at geostationary orbit.</p><p>This work has received funding from the European Union’s Horizon 2020 research and innovation programme "SafeSpace" under grant agreement No 870437 and from the European Space Agency under the "European Contribution to International Radiation Environment Near Earth (IRENE) Modelling System" activity under ESA Contract No 4000127282/19/NL/IB/gg.</p>

Event Abstract Back to Event On the role of rTJP in moral judgments: a tDCS study Laëtitia Leloup1*, Diana Dongo Miletich1, 2, Gaëlle Andriet1, Yves Vandermeeren3, 4 and Dana Samson1 1 Université catholique de Louvain-La-Neuve, Psychological Sciences Research Institute (IPSY), Belgium 2 Fonds de la Recherche Scientifique (FNRS), Belgium 3 Université catholique de Louvain (UCL), CHU Dinant Godinne, Belgium 4 Université catholique de Louvain (UCL), Institute of Neuroscience (IoNS), Belgium Abstract Representing and integrating information about intentions and consequences plays a crucial role in mature moral judgments(Cushman, 2008). It has been suggested that the rTPJ (right Temporo-Parietal Junction) is responsible for integrating intention information in moral judgments (Young, Cushman, Hauser, & Saxe, 2007 ; Young, Camprodon, Hauser, Pascual-Leone, & Saxe, 2010). In this study we investigated this hypothesis with tDCS (transcranial Direct Current Stimulation) in healthy participants. tDCS was used in order to enhance (anodal stimulation) or decrease (cathodal stimulation) the excitability of the rTPJ while participants made moral judgments. 72 right handed participants were randomly assigned to one of three tDCS conditions (anodal, cathodal, placebo) following a double-blind procedure. The first half of the moral judgments were processed without any stimulation (baseline) while the second half were processed under tDCS stimulation (anodal, cathodal, placebo). The scenarios presented to participants manipulated orthogonally the intention to harm (no intention to harm vs. intention to harm) and the consequence of the action (no consequence vs. harmful consequence). Results will be discussed in terms of the possible roles of the rTPJ in moral judgements. Short Comment Moral cognition alterations are frequent in brain-damaged patients and are problematic for the patients’ social and professional life (Cicerone, 1997). A better understanding of the cognitive mechanisms and the neural substrates underlying moral cognition can provide useful pointers to improve the diagnosis and rehabilitation of moral cognition impairments. Furthermore, this study also allows to see the effectiveness of tDCS for modulating complex cognitive functions. Keywords: Neuropsychology, Moral cognition, Moral judgments, transcranial direct current stimulation (tDCS), right temporo-parietal junction (rTPJ) Conference: Belgian Brain Council 2014 MODULATING THE BRAIN: FACTS, FICTION, FUTURE, Ghent, Belgium, 4 Oct - 4 Oct, 2014. Presentation Type: Poster Presentation Topic: Clinical Neuroscience Citation: Leloup L, Dongo Miletich D, Andriet G, Vandermeeren Y and Samson D (2014). On the role of rTJP in moral judgments: a tDCS study. Conference Abstract: Belgian Brain Council 2014 MODULATING THE BRAIN: FACTS, FICTION, FUTURE. doi: 10.3389/conf.fnhum.2014.214.00041 Copyright: The abstracts in this collection have not been subject to any Frontiers peer review or checks, and are not endorsed by Frontiers. They are made available through the Frontiers publishing platform as a service to conference organizers and presenters. The copyright in the individual abstracts is owned by the author of each abstract or his/her employer unless otherwise stated. Each abstract, as well as the collection of abstracts, are published under a Creative Commons CC-BY 4.0 (attribution) licence (https://creativecommons.org/licenses/by/4.0/) and may thus be reproduced, translated, adapted and be the subject of derivative works provided the authors and Frontiers are attributed. For Frontiers’ terms and conditions please see https://www.frontiersin.org/legal/terms-and-conditions. Received: 30 Jun 2014; Published Online: 12 Jul 2014. * Correspondence: Miss. Laëtitia Leloup, Université catholique de Louvain-La-Neuve, Psychological Sciences Research Institute (IPSY), Louvain-La-Neuve, Belgium, laetitia.leloup@uclouvain.be Login Required This action requires you to be registered with Frontiers and logged in. To register or login click here. Abstract Info Abstract The Authors in Frontiers Laëtitia Leloup Diana Dongo Miletich Gaëlle Andriet Yves Vandermeeren Dana Samson Google Laëtitia Leloup Diana Dongo Miletich Gaëlle Andriet Yves Vandermeeren Dana Samson Google Scholar Laëtitia Leloup Diana Dongo Miletich Gaëlle Andriet Yves Vandermeeren Dana Samson PubMed Laëtitia Leloup Diana Dongo Miletich Gaëlle Andriet Yves Vandermeeren Dana Samson Related Article in Frontiers Google Scholar PubMed Abstract Close Back to top Javascript is disabled. Please enable Javascript in your browser settings in order to see all the content on this page.

Landau‐Kleffner syndrome: 50 years after

The XXXth International Colloquium on Group Theoretical Methods in Physics (ICGTMP), also known as the Group30 conference, took place in Ghent (Belgium) from Monday 14 to Friday 18 July 2014. The conference was organised by Ghent University (Department of Applied Mathematics, Computer Science and Statistics, and Department of Mathematical Analysis). The website http://www.group30.ugent.be is still available.

The Institut Interuniversitaire des Sciences Nucléaires of the Belgian National Foundation for Scientific Research (Fonds de la Recherche Scientifique, or FNRS) has joined the CERN SCOAP3 project.