THE BEHAVIORAL EDUCATIONAL THOUGHT OF ABD AL-HAMID IBN BADIS AND ITS CIVILIZATIONAL DIMENSION

Sheikh Abdul Hamid bin Badis is considered one of the pioneers of renaissance and reform who had a prominent impact in the movement of renewal and social change to advance the nation change its deteriorating reality through an educational system and intellectual educational program within his comprehensive civilizational reform project, where he attached great importance to the consideration of education as the basis of any civilizational building. He has all his time and effort. His biggest bet was on changing man to change his reality and to pay attention to his reconstruction mission according to the Quranic civilizational cosmic vision. Keywords: Educational Thought, Education, The Civilizational Dimension, Abdul Hamid Bin Badis.

Montessori Approach to Science Education: Cosmic Vision as a Unique Area of Pupils’ Studies

The paper aims at recalling Maria Montessori’s essential assumptions about the child development and organization of the educational process as a basic issue considering the concept of science education. In the Montessori pedagogy, it is characterized by the form of the so-called Cosmic Education. Cosmic Education is a unique approach to work with children aged 6 to 12. Thus, the idea of Cosmic Education, the relationship between the child’s needs and the science education curriculum is elucidated. The essence of the Great and Key Lessons as centers of children’s exploration and research is discussed. The Montessorian way of learning about fundamental human needs is presented as an inspiration for school practice. The basis for collecting empirical material is the analysis of the content aiming at the current achievements within the selected topic characterization.

Community Access to CHEOPS

<p>Launched on 18 December 2019, CHEOPS (CHaracterising ExOPlanet Satellite) is the first exoplanet mission dedicated to the search for transits of exoplanets by means of ultrahigh precision photometry of bright stars already known to host planets. It is the first S-(small) class mission in ESA’s Cosmic Vision 2015-2025, and a partnership between Switzerland and ESA, with important contributions from 10 other member states.<br class="" /><br class="" />CHEOPS will provide the unique capability of determining accurate radii for a subset of planets in the super-Earth to Neptune mass range, for which masses have already been estimated from ground- based spectroscopic surveys. It will also provide precision radii for new planets discovered by ground- and space-based transit surveys, including TESS. By combining known masses with CHEOPS sizes, it will be possible to determine accurate densities for these smaller planets, providing key insight into their composition and internal structure. By identifying transiting exoplanets with high potential for in-depth characterisation – e.g. those that are potentially rocky and have thin atmospheres - CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres.</p> <p>In this poster we detail how the Community can access CHEOPS, with emphasis on the ESA-run Guest Observers Programme and the Annual Announcement of Opportunity for observing time Year 3 of CHEOPS, which is foreseen to come out in Quarter 4 2021.</p>

Ganymede’s interaction with the jovian plasma from hybrid simulation

<p>The JUICE (JUpiter ICy moon Explorer) mission, selected by the European Space Agency in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat (JUICE Red Book, 2014). The Galilean satellites are known to have thin atmospheres, technically exospheres (McGrath et al., 2004), produced by ion-induced sputtering and sublimation of the surface materials. These moons and tenuous atmosphere are embedded in the flowing plasma of the jovian. The interaction between the neutral environments of the Galilean satellites and the jovian plasma changes the plasma momentum, the temperature and generates strong electrical currents. In order to prepare the scientific return of the mission and the optimization of operation modes of plasma instruments, a modeling effort has been carried out at LATMOS (PhD R. Allioux, IRAP, 2012; L. Leclercq, LATMOS, 2015; O. Apurva, LATMOS, 2017). A 3D parallel multi-species hybrid model (Latmos Hybrid Simulation, LatHyS) has been developed to model and characterize the plasma environment of Ganymede (Leclercq et al, 2016; Modolo et al, 2016) and a 3D parallel multi-species exospheric model (Exospheric Global Model, EGM) to pattern the dynamic of the neutral envelopes of Ganymede (Turc et al, 2014; Leblanc et al, 2017). The presentation will examine the global structure of the interaction with the jovian plasma, to describe the formation of Alfvén wings, and to emphasize the phenomena related to the multi-species nature of the plasma. The simulation model supports the preparation of the JUICE mission and its Ganymede phase by characterizing boundary crossings.</p>

Ariel - The ESA M4 Space Mission to Focus on the Nature Of Exoplanets

<p>Ariel, the atmospheric remote-sensing infrared exoplanet large-survey, is the recently adopted M4 mission within the Cosmic Vision science programme of ESA. The goal of Ariel is to investigate the atmospheres of planets orbiting distant stars in order to address the fundamental questions on how planetary systems form and evolve and to investigate in unprecedented detail the composition of a large number of exoplanetary atmospheres. During its 4-year mission, Ariel will observe hundreds of exoplanets ranging from Jupiter- and Neptune-size down to super-Earth size, in a wide variety of environments, in the visible and the infrared. The main focus of the mission will be on warm and hot planets in orbits close to their star. Some of the planets may be in the habitable zones of their stars, however. The analysis of Ariel spectra and photometric data will allow to extract the chemical fingerprints of gases and condensates in the planets’ atmospheres, including the elemental composition for the most favourable targets. The Ariel mission has been developed by a consortium of more than 60 institutes from 15 ESA member state countries, including UK, France, Italy, Poland, Spain, the Netherlands, Belgium, Austria, Denmark, Ireland, Hungary, Sweden, Czech Republic, Germany, Portugal, with an additional contribution from NASA. In this talk, we will review the science goals of the mission and give insight into the current status, both from the ESA and the Ariel Mission Consortium point of view.  </p>

JANUS: the camera system onboard JUICE. Operational approach and scientific capabilities from operations case studies.

<p>The JUICE (JUpiter ICy moons Explorer) mission was selected in May 2012 as the first Large mission (L1) in the frame of the ESA Cosmic Vision 2015-2025 program and it will be launched in 2022. The mission aims to perform an in-depth characterization of the Jovian system, with an operational phase of about 3.5 years [1]. Main targets for this mission will be the vast Jovian system, including Jupiter itself, its magnetosphere, satellites, rings, neutral gas tori and the complex interplays among all those system components. Detailed investigations of three of Jupiter's Galilean icy satellites (Ganymede, Europa, and Callisto) will be achieved thanks to a large number of fly-bys and 9 months in orbit around Ganymede.</p> <p>JANUS (Jovis, Amorum ac Natorum Undique Scrutator) is the scientific camera system onboard JUICE [2]. Despite the resource limitations, and the environmental constraints, the instrument architecture and design will be able to satisfy the great variability of observing conditions for its different targets, benefiting from the spacecraft and orbit design to its maximum. The JANUS design has to cope with a wide range of targets, from Jupiter’s atmosphere, to solid satellite surfaces and their exospheres, rings, and transient phenomena like lightning. In order to obtain multispectral observations of scientific targets as well as specific observations in narrow bands, JANUS is equipped with a filter wheel mechanism with 13 wide and narrow-band filters, allowing wavelength coverage in the 340 - 1080 nm range. JANUS will greatly improve spatial coverage, resolution and time coverage on many targets in the Jupiter system. JANUS ground sampling ranges from 400 m/pixel to < 3 m/pixel for the three main Galilean satellites, and from few to few tens of km/pixel for Jupiter and other targets in the Jovian system, such as Io, the minor inner and outer irregular moons, and Jupiter’s rings. JANUS observations of Jupiter’s atmosphere will range from full mapping to regional imaging at spatial resolutions down to 10 km/pix. Global wind fields with accuracies better than 1.0 m/s will be obtained several times during the mission.</p> <p>Assuming the availability of scientific data volume (during operations about 20% of 1.4 Gbit/day is allocated to JANUS), JANUS observations will fully cover Ganymede in 4 colours with a resolution of about 100 m/pix as a goal, also providing regional DTMs. About 3% of the surface of Ganymede will be covered with a resolution of 10 - 30 m/pix for selected Regions of Interest, using both panchromatic and colour filters, and providing stereo images for the 3D reconstruction of the surface. This will represent dramatic improvements in imaging with respect to Galileo coverage in all the science targets covered by JUICE/JANUS.</p> <p>In addition to presenting the science goals that we are aiming to achieve during the JUICE science phase, we will show examples of a case study of operations, to highlight how the achievement of science goals is strictly related to the resources available to the instrument.</p> <p>References: [1] Grasset et al., (2013), <em>PSS, </em>78, 1-21. [2] Palumbo et al., (2014), <em>EGU conference</em></p> <p>Acknowledgements: The activity has been realized under the ASI-INAF contract 2018-25-HH.0. LML acknowledges financial support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa” award to the Instituto de Astrofısica de Andalucia (SEV-2017-0709) and from project PGC2018-099425-B-I00 (MCI/AEI/FEDER, UE).</p>

PAOS, the Physical Optics Propagation model of the Ariel optical system

<p>Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, is a medium-class space mission part of ESA's Cosmic Vision programme, due for launch in 2029. Ariel will survey a diverse sample of about 1000 extrasolar planets in the visible and infrared spectrum to answer questions about their composition, formation and evolution. Ariel mounts an off-axis Cassegrain telescope with a 1100 mm x 730 mm elliptical mirror and has two separate instruments (FGS and AIRS) that cover the 0.5-7.8 micron spectral range. To study the Ariel optical performance and related systematics, we developed PAOS, the Proper Ariel Optical Simulator, an End-to-End physical optics propagation model of the Ariel Telescope and subsystems based on PROPER, an optical propagation library for IDL, Python and Matlab. PAOS is a Python code that consists of a series of calls to PROPER library functions and procedures that reproduces the Ariel optical design, interleaved with additional code that can be specified according to the simulation. Using PAOS, we can investigate how diffraction affects the electromagnetic wavefront as it travels through the Ariel optical systems and the resulting PSFs in the photometric and spectroscopic channels of the mission. This enables to perform a large number of detailed analyses, both on the instrument side and on the optimisation of the Ariel mission. In particular, PAOS can be used to support the requirement on the maximum amplitude of the aberrations for the manufacturing of the Ariel primary mirror, as well as to develop strategies for in-flight calibration, e.g. focussing procedures for the FGS and AIRS focal planes, and to tackle systematics such as pointing jitter and vignetting. With the Ariel mission now in the process of finalizing the instrument design and the data analysis techniques, PAOS will greatly contribute in evaluating the Ariel payload performance with models to be included in the existing Ariel simulators such as ArielRad, the Ariel Radiometric model, and ExoSim, the Exoplanet Observation simulator, for the purpose of studying and optimising the science return from Ariel.</p>

Observability of Exo-Atmospheres in emission using Ariel

<p>Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, is a medium-class space mission part of ESA's Cosmic Vision program, due for launch in 2029. Ariel is the first mission dedicated to the spectroscopic observation of a diverse, statistical sample of about 1000 transiting exoplanets, obtaining spectra in transit, eclipse, or both, to answer questions about their composition, formation and evolution. Ariel has adopted a four-tiered approach in which all targets are observed with different SNRs to optimise the science return from the mission. Ariel has two separate instruments (FGS and AIRS) that will perform simultaneous observations across the 0.5-7.8 micron spectral range, which encompasses both the peak emission of exoplanets and the spectral signatures of key molecules. This will enable Ariel to collect statistical information on the composition and the thermal structure of exo-atmospheres, allowing it to reveal underlying trends in exoplanetary populations. In particular, transit spectroscopy is expected to provide the bulk of information on the chemical composition of exo-atmospheres, while eclipses are necessary to constrain their thermodynamic state. In this framework, I report a preliminary study of Ariel targets observed in emission: at first, I investigate the information content from Tier 1 data, where spectra from the full population of Ariel targets are observed with low SNR, and binned as if Ariel were a multi-band photometer to increase the SNR. I then investigate the effectiveness of Ariel in detecting chemical-physical trends in exoplanetary populations observed in Tier 2, designed to reach SNR in excess of 7 on spectra binned to roughly half the spectral resolution of the focal planes, as specified by the mission requirements.</p>

Determination of Venus’ Interior Structure with EnVision

The Venusian geological features are poorly gravity-resolved, and the state of the core is not well constrained, preventing an understanding of Venus’ cooling history. The EnVision candidate mission to the ESA’s Cosmic Vision Programme consists of a low-altitude orbiter to investigate geological and atmospheric processes. The gravity experiment aboard this mission aims to determine Venus’ geophysical parameters to fully characterize its internal structure. By analyzing the radio-tracking data that will be acquired through daily operations over six Venusian days (four Earth’s years), we will derive a highly accurate gravity field (spatial resolution better than ~170 km), allowing detection of lateral variations of the lithosphere and crust properties beneath most of the geological features. The expected 0.3% error on the Love number k2, 0.1° error on the tidal phase lag and 1.4% error on the moment of inertia are fundamental to constrain the core size and state as well as the mantle viscosity.

ArielRad: the Ariel radiometric model

ArielRad, the Ariel radiometric model, is a simulator developed to address the challenges in optimising the space mission science payload and to demonstrate its compliance with the performance requirements. Ariel, the Atmospheric Remote-Sensing Infrared Exoplanet Large-survey, has been selected by ESA as the M4 mission in the Cosmic Vision programme and, during its 4 years primary operation, will provide the first unbiased spectroscopic survey of a large and diverse sample of transiting exoplanet atmospheres. To allow for an accurate study of the mission, ArielRad uses a physically motivated noise model to estimate contributions arising from stationary processes, and includes margins for correlated and time-dependent noise sources. We show that the measurement uncertainties are dominated by the photon statistic, and that an observing programme with about 1000 exoplanetary targets can be completed during the primary mission lifetime.