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25 pages, 2274 KiB  
Article
Assessment of Flyby Methods as Applied to Close Encounters among Asteroids
by Nicolò Stronati, Marco Fenucci, Marco Micheli and Marta Ceccaroni
Aerospace 2024, 11(8), 647; https://doi.org/10.3390/aerospace11080647 - 9 Aug 2024
Viewed by 315
Abstract
Orbital flybys have been extensively studied for spacecraft missions, resulting in effective mathematical and physical models. However, these models’ applicability to natural encounters involving asteroids has not been explored. This paper examines the applicability of two such theories, patched conics (PC) and the [...] Read more.
Orbital flybys have been extensively studied for spacecraft missions, resulting in effective mathematical and physical models. However, these models’ applicability to natural encounters involving asteroids has not been explored. This paper examines the applicability of two such theories, patched conics (PC) and the Keplerian map (KM), to asteroid encounters. A review of the two methods will be provided, highlighting their assumptions and range of applicability. Simulations of asteroid–asteroid encounters will then be performed to evaluate their effectiveness in these scenarios. The simulation parameters are set by collecting data on actual asteroid–asteroid encounters, hereby presented, generally characterised by high close approach distances and small masses of the perturbing bodies, if compared to those used to build the flyby theories. Results show that the PC theory’s effectiveness diminishes with increasing approach distances, aligning with its assumptions. Moreover, the prediction of the model is better in the geometric configurations where the flyby has major effects on the orbital energy change. The KM theory has shown good effectiveness for encounters occurring outside the sphere of influence of the perturbing body, even for very high distances. This research investigates flyby models’ strengths and weaknesses in asteroid encounters, offering practical insights and future directions. Full article
(This article belongs to the Special Issue Advances in Asteroid Dynamics)
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Figure 1

Figure 1
<p>Bar chart of the absolute frequency of the encounter distances with respect to the perturbing body’s Hill’s radius. The plot includes only the encounters between 1 and 200 <math display="inline"><semantics> <msub> <mi>R</mi> <mi>H</mi> </msub> </semantics></math>. The bins for the bar chart have a uniform span of 2 <math display="inline"><semantics> <mrow> <msub> <mi>r</mi> <mi>P</mi> </msub> <mo>/</mo> <msub> <mi>R</mi> <mi>H</mi> </msub> </mrow> </semantics></math>.</p>
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<p>Relationship between the <math display="inline"><semantics> <mrow> <mo>Δ</mo> <mrow> <mo>(</mo> <mi>res</mi> <mo>)</mo> </mrow> </mrow> </semantics></math> of the detected single encounters and the encounter distance, relative to the Hill’s radius, <math display="inline"><semantics> <msub> <mi>R</mi> <mi>H</mi> </msub> </semantics></math>.</p>
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<p>Representation of the relative inclination between two different orbits. <math display="inline"><semantics> <msub> <mi>i</mi> <mrow> <mi>r</mi> <mi>e</mi> <mi>l</mi> </mrow> </msub> </semantics></math> is the inclination that one orbit has with respect to the perifocal plane of the other object, so this was taken as the new reference frame instead of the ecliptic.</p>
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<p>Relationship between the relative inclination, <math display="inline"><semantics> <msub> <mi>i</mi> <mrow> <mi>r</mi> <mi>e</mi> <mi>l</mi> </mrow> </msub> </semantics></math>, and the normalised relative velocity, <span class="html-italic">U</span>.</p>
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<p>Relationship between the relative velocity and the encounter distance, compared with the escape velocity, <math display="inline"><semantics> <mrow> <msub> <mi>v</mi> <mi>E</mi> </msub> <mo>/</mo> <msqrt> <mi>μ</mi> </msqrt> </mrow> </semantics></math> (red line). The <span class="html-italic">y</span>-axis is in logarithmic scale.</p>
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<p>Geometric representation of the planetocentric frame.</p>
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<p><math display="inline"><semantics> <mi>α</mi> </semantics></math> and <math display="inline"><semantics> <mi>β</mi> </semantics></math> angles for the analysed encounters.</p>
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<p><math display="inline"><semantics> <mi>γ</mi> </semantics></math> and <math display="inline"><semantics> <mi>β</mi> </semantics></math> angles for the analysed encounters.</p>
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<p>Relationship between <math display="inline"><semantics> <mi>γ</mi> </semantics></math> and <math display="inline"><semantics> <msub> <mi>i</mi> <mrow> <mi>r</mi> <mi>e</mi> <mi>l</mi> </mrow> </msub> </semantics></math>.</p>
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<p>Relationship between <math display="inline"><semantics> <mi>γ</mi> </semantics></math> and <span class="html-italic">U</span>.</p>
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<p>Hyperbolic trajectory of the massless particle around the secondary during a flyby. <math display="inline"><semantics> <msub> <mi mathvariant="bold">V</mi> <mi>P</mi> </msub> </semantics></math> represents the velocity vector of the secondary, <math display="inline"><semantics> <msubsup> <mi mathvariant="bold">v</mi> <mo>∞</mo> <mo>+</mo> </msubsup> </semantics></math> and <math display="inline"><semantics> <msubsup> <mi mathvariant="bold">v</mi> <mo>∞</mo> <mo>−</mo> </msubsup> </semantics></math> are, respectively, the velocities at the entry and exit points of the hyperbolic trajectory, and <math display="inline"><semantics> <mrow> <mn>2</mn> <mi>δ</mi> </mrow> </semantics></math> is the deflection angle between the two asymptotes of the hyperbola, caused by the flyby.</p>
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<p>Representation of the relative velocity vector, <math display="inline"><semantics> <mi mathvariant="bold">U</mi> </semantics></math>, in the <math display="inline"><semantics> <mrow> <mi>X</mi> <mi>Y</mi> <mi>Z</mi> </mrow> </semantics></math> planetocentric frame. <math display="inline"><semantics> <mrow> <mi>ϑ</mi> <mo>∈</mo> <mo>[</mo> <mn>0</mn> <mo>,</mo> <mn>2</mn> <mi>π</mi> <mo>)</mo> </mrow> </semantics></math> is the angle between the <span class="html-italic">Y</span>-axis and <math display="inline"><semantics> <mi mathvariant="bold">U</mi> </semantics></math>, while <math display="inline"><semantics> <mrow> <mi>ϕ</mi> <mo>∈</mo> <mo>[</mo> <mn>0</mn> <mo>,</mo> <mi>π</mi> <mo>]</mo> </mrow> </semantics></math> is the angle between the <math display="inline"><semantics> <mrow> <mi>Y</mi> <mi>Z</mi> </mrow> </semantics></math> plane and the <math display="inline"><semantics> <mrow> <mi>Y</mi> <mi>U</mi> </mrow> </semantics></math> plane.</p>
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<p>Representation of the synodic reference frame.</p>
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<p>Relative error of the <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>P</mi> <mi>C</mi> </mrow> </msub> </mrow> </semantics></math> with respect to <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>G</mi> <mi>V</mi> <mi>E</mi> </mrow> </msub> </mrow> </semantics></math> at different <math display="inline"><semantics> <mrow> <msub> <mi>r</mi> <mi>P</mi> </msub> <mo>/</mo> <msub> <mi>R</mi> <mi>H</mi> </msub> </mrow> </semantics></math> and <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>77</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>. The values above <math display="inline"><semantics> <mrow> <mn>0.6</mn> </mrow> </semantics></math> are blanked out in the heatmap for a better visualisation.</p>
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<p>Relative error of the <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>P</mi> <mi>C</mi> </mrow> </msub> </mrow> </semantics></math> with respect to <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>G</mi> <mi>V</mi> <mi>E</mi> </mrow> </msub> </mrow> </semantics></math> at different <math display="inline"><semantics> <mrow> <msub> <mi>r</mi> <mi>P</mi> </msub> <mo>/</mo> <msub> <mi>R</mi> <mi>H</mi> </msub> </mrow> </semantics></math> and <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>0</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>. The values above <math display="inline"><semantics> <mrow> <mn>0.6</mn> </mrow> </semantics></math> are blanked out in the heatmap for a better visualisation.</p>
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<p><math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>P</mi> <mi>C</mi> </mrow> </msub> </mrow> </semantics></math> for <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>77</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>. According to Equation (<a href="#FD12-aerospace-11-00647" class="html-disp-formula">12</a>), there is no effect of parameter <math display="inline"><semantics> <mi>γ</mi> </semantics></math>.</p>
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<p><math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>G</mi> <mi>V</mi> <mi>E</mi> </mrow> </msub> </mrow> </semantics></math> for <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>77</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>.</p>
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<p>Relative error of the <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>K</mi> <mi>M</mi> </mrow> </msub> </mrow> </semantics></math> with respect to <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>G</mi> <mi>V</mi> <mi>E</mi> </mrow> </msub> </mrow> </semantics></math> at different <math display="inline"><semantics> <mrow> <msub> <mi>r</mi> <mi>P</mi> </msub> <mo>/</mo> <msub> <mi>R</mi> <mi>H</mi> </msub> </mrow> </semantics></math> and <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>77</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>. The values above <math display="inline"><semantics> <mrow> <mn>0.6</mn> </mrow> </semantics></math> are blanked out in the heatmap for a better visualisation.</p>
Full article ">Figure 19
<p>Relative error of the <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>K</mi> <mi>M</mi> </mrow> </msub> </mrow> </semantics></math> with respect to <math display="inline"><semantics> <mrow> <mo>Δ</mo> <msub> <mi>E</mi> <mrow> <mi>G</mi> <mi>V</mi> <mi>E</mi> </mrow> </msub> </mrow> </semantics></math> at different <math display="inline"><semantics> <mrow> <msub> <mi>r</mi> <mi>P</mi> </msub> <mo>/</mo> <msub> <mi>R</mi> <mi>H</mi> </msub> </mrow> </semantics></math> and <math display="inline"><semantics> <mrow> <mi>β</mi> <mo>=</mo> <mn>0</mn> <mo> </mo> <mi>deg</mi> </mrow> </semantics></math>. The values above <math display="inline"><semantics> <mrow> <mn>0.6</mn> </mrow> </semantics></math> are blanked out in the heatmap for a better visualisation.</p>
Full article ">
15 pages, 1308 KiB  
Review
Considerations on Possible Directions for a Wide Band Polarimetry X-ray Mission
by Paolo Soffitta, Enrico Costa, Nicolas De Angelis, Ettore Del Monte, Klaus Desch, Alessandro Di Marco, Giuseppe Di Persio, Sergio Fabiani, Riccardo Ferrazzoli, Markus Gruber, Takahashi Hiromitsu, Saba Imtiaz, Philip Kaaret, Jochen Kaminski, Dawoon E. Kim, Fabian Kislat, Henric Krawczynski, Fabio La Monaca, Carlo Lefevre, Hemanth Manikantan, Herman L. Marshall, Romana Mikusincova, Alfredo Morbidini, Fabio Muleri, Stephen L. O’Dell, Takashi Okajima, Mark Pearce, Vladislavs Plesanovs, Brian D. Ramsey, Ajay Ratheesh, Alda Rubini, Shravan Vengalil Menon and Martin C. Weisskopfadd Show full author list remove Hide full author list
Galaxies 2024, 12(4), 47; https://doi.org/10.3390/galaxies12040047 - 8 Aug 2024
Viewed by 244
Abstract
The Imaging X-ray Polarimetry Explorer (IXPE) has confirmed that X-ray polarimetry is a valuable tool in astronomy, providing critical insights into the emission processes and the geometry of compact objects. IXPE was designed to be sensitive in the 2–8 keV energy range for [...] Read more.
The Imaging X-ray Polarimetry Explorer (IXPE) has confirmed that X-ray polarimetry is a valuable tool in astronomy, providing critical insights into the emission processes and the geometry of compact objects. IXPE was designed to be sensitive in the 2–8 keV energy range for three primary reasons: (1) celestial X-ray sources are bright within this range, (2) the optics are effective, and (3) most sources across various classes were expected to exhibit some level of polarization. Indeed, IXPE is a great success, and its discoveries are necessitating the revision of many theoretical models for numerous sources. However, one of IXPE’s main limitations is its relatively narrow energy band, coupled with rapidly declining efficiency. In this paper, we will demonstrate the benefits of devising a mission focused on a broader energy band (0.1–79 keV). This approach leverages current technologies that align well with theoretical expectations and builds on the successes of IXPE. Full article
(This article belongs to the Special Issue X-ray Polarization: A New Era Begins)
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Figure 1

Figure 1
<p>The modulation factor from [<a href="#B12-galaxies-12-00047" class="html-bibr">12</a>] for some low-pressure gas pixel detectors filled with isobutane as evaluated by Monte Carlo simulation.</p>
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<p>The REDSoX Rocket Experiment Demonstrator of a Soft X-ray polarimeter. The payload consists of the X-ray optics with Wolter type I mirror shells, 200 nm period critical angle transmission (CAT) gratings mounted on a 2.5 m focal length optical bench. A rocket flight was granted funding to completion. The target for this short flight will be decided with careful evaluation of its real performances.</p>
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<p>The sensitivity of the LEP (2–10 keV) and MEP (5–35 keV) foreseen for the new hard X-ray mission [<a href="#B61-galaxies-12-00047" class="html-bibr">61</a>].</p>
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<p>The configuration of the XL-Calibur focal plane instrument. One Beryllium scatterer is surrounded by four planes of CZT detectors, surrounded by a thick BGO shield to reduce the background [<a href="#B72-galaxies-12-00047" class="html-bibr">72</a>].</p>
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32 pages, 1059 KiB  
Article
Categorization of Attributes and Features for the Location of Electric Vehicle Charging Stations
by Andrea Mazza, Angela Russo, Gianfranco Chicco, Andrea Di Martino, Cristian Giovanni Colombo, Michela Longo, Paolo Ciliento, Marco De Donno, Francesca Mapelli and Francesco Lamberti
Energies 2024, 17(16), 3920; https://doi.org/10.3390/en17163920 - 8 Aug 2024
Viewed by 293
Abstract
The location of Electric Vehicle Charging Stations (EVCSs) is gaining significant importance as part of the conversion to a full-electric vehicle fleet. Positive or negative impacts can be generated mainly based on the quality of service offered to customers and operational efficiency, also [...] Read more.
The location of Electric Vehicle Charging Stations (EVCSs) is gaining significant importance as part of the conversion to a full-electric vehicle fleet. Positive or negative impacts can be generated mainly based on the quality of service offered to customers and operational efficiency, also potentially involving the electrical grid to which the EVCSs are connected. The EVCS location problem requires an in-depth and comprehensive analysis of geographical, market, urban planning, and operational aspects that can lead to several potential alternatives to be evaluated with respect to a defined number of features. This paper discusses the possible use of a multi-criteria decision-making approach, considering the differences between multi-objective decision making (MODM) and multi-attribute decision-making (MADM), to address the EVCS location problem. The conceptual evaluation leads to the conclusion that the MADM approach is more suitable than MODM for the specific problem. The identification of suitable attributes and related features is then carried out based on a systematic literature review. For each attribute, the relative importance of the features is obtained by considering the occurrence and the dedicated weights. The results provide the identification of the most used attributes and the categorization of the selected features to shape the proposed MADM framework for the location of the electric vehicle charging infrastructure. Full article
(This article belongs to the Special Issue Smart Electric Vehicle Charging Approaches for Demand Response)
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<p>Locating EVCS problem roadmap.</p>
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<p>Matrix of occurrence for the output attributes.</p>
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<p>Matrix of weights for the output attributes.</p>
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<p>Matrices for attribute subcategories: (<b>a</b>) occurrence, (<b>b</b>) weights.</p>
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<p>Matrices for attribute categories: (<b>a</b>) occurrence, (<b>b</b>) weights.</p>
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13 pages, 2715 KiB  
Technical Note
Laser Observations of GALILEO Satellites at the CBK PAN Astrogeodynamic Observatory in Borowiec
by Paweł Lejba, Piotr Michałek, Tomasz Suchodolski, Adrian Smagło, Mateusz Matyszewski and Stanisław Zapaśnik
Remote Sens. 2024, 16(15), 2862; https://doi.org/10.3390/rs16152862 - 5 Aug 2024
Viewed by 427
Abstract
The laser station (BORL) owned by the Space Research Centre of the Polish Academy of Sciences and situated at the Astrogeodynamic Observatory in Borowiec near Poznań regularly observes more than 100 different objects in low Earth orbit (LEO) and medium Earth orbit (MEO). [...] Read more.
The laser station (BORL) owned by the Space Research Centre of the Polish Academy of Sciences and situated at the Astrogeodynamic Observatory in Borowiec near Poznań regularly observes more than 100 different objects in low Earth orbit (LEO) and medium Earth orbit (MEO). The BORL sensor’s laser observation range is from 400 km to 24,500 km. The laser measurements taken by the BORL sensor are utilized to create various products, including the geocentric positions and movements of ground stations, satellite orbits, the components of the Earth’s gravitational field and their changes over time, Earth’s orientation parameters (EOPs), and the validation of the precise Galileo orbits derived using microwave measurements, among others. These products are essential for supporting local and global geodetic and geophysics research related to time. They are crucial for the International Terrestrial Reference Frame (ITRF), which is managed by the International Earth Rotation and Reference Systems Service (IERS). In 2023, the BORL laser station expanded its list of tracked objects to include all satellites of the European satellite navigation system GALILEO, totaling 28 satellites. During that year, the BORL laser station recorded 77 successful passes of GALILEO satellites, covering a total of 21 objects. The measurements taken allowed for the registration of 7419 returns, resulting in 342 normal points. The average RMS for all successful GALILEO observations in 2023 was 13.5 mm. Full article
(This article belongs to the Special Issue Advanced Remote Sensing Technology in Modern Geodesy)
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Figure 1
<p>The CBK PAN laser sensor in Borowiec consists of two independent laser modules: a smaller, nanosecond one in the foreground and a larger, picosecond one in the background.</p>
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<p>Number of tracked objects by BORL station in years 1992–2023.</p>
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<p>The constellation of GALILEO satellites [<a href="#B17-remotesensing-16-02862" class="html-bibr">17</a>].</p>
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<p>Artist’s view of a GALILEO Full Operational Capability (FOC). The green circle marks the panel with laser retroreflectors [<a href="#B18-remotesensing-16-02862" class="html-bibr">18</a>].</p>
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<p>Pass of GALILEO-212 (E03) registered by the BORL sensor on 3 May 2023, 23:12 UTC, showing slant ranges (<b>a</b>) and fit residuals (<b>b</b>) with 159 valid returns. The min. and max. distances to the satellite were 23,589 km and 23,790 km, respectively.</p>
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<p>Pass of GALILEO-104 (E20) registered by the BORL sensor on 21 May 2023, 21:27 UTC, showing slant ranges (<b>a</b>) and fit residuals (<b>b</b>) with 592 valid returns. The min. and max. distances to the satellite were 23,701 km and 24,115 km, respectively.</p>
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<p>Pass of GALILEO-208 (E08) registered by the BORL sensor on 22 May 2023, 20:59 UTC, showing slant ranges (<b>a</b>) and fit residuals (<b>b</b>) with 214 valid returns. The min. and max. distances to the satellite were 23,612 km and 23,958 km, respectively.</p>
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<p>Pass of GALILEO-202 (E14) registered by the BORL sensor on 21 September 2023, 22:37 UTC, showing slant ranges (<b>a</b>) and fit residuals (<b>b</b>) with 310 valid returns. The min. and max. distances to the satellite were 19,701 km and 20,292 km, respectively.</p>
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9 pages, 1716 KiB  
Article
Quantitative Edge Analysis Can Differentiate Pancreatic Carcinoma from Normal Pancreatic Parenchyma
by Maria Chiara Ambrosetti, Alberto Ambrosetti, Matilde Bariani, Giuseppe Malleo, Giancarlo Mansueto and Giulia A. Zamboni
Diagnostics 2024, 14(15), 1681; https://doi.org/10.3390/diagnostics14151681 - 2 Aug 2024
Viewed by 282
Abstract
This study aimed to introduce specific image feature analysis, focusing on pancreatic margins, and to provide a quantitative measure of edge irregularity, evidencing correlations with the presence/absence of pancreatic adenocarcinoma. We selected 50 patients (36 men, 14 women; mean age 63.7 years) who [...] Read more.
This study aimed to introduce specific image feature analysis, focusing on pancreatic margins, and to provide a quantitative measure of edge irregularity, evidencing correlations with the presence/absence of pancreatic adenocarcinoma. We selected 50 patients (36 men, 14 women; mean age 63.7 years) who underwent Multi-detector computed tomography (MDCT) for the staging of pancreatic adenocarcinoma of the tail of the pancreas. Computer-assisted quantitative edge analysis was performed on the border fragments in MDCT images of neoplastic and healthy glandular parenchyma, from which we obtained the root mean square deviation SD of the actual border from the average boundary line. The SD values relative to healthy and neoplastic borders were compared using a paired t-test. A significant SD difference was observed between healthy and neoplastic borders. A threshold SD value was also found, enabling the differentiation of adenocarcinoma with 96% specificity and sensitivity. We introduced a quantitative measure of boundary irregularity, which correlates with the presence/absence of pancreatic adenocarcinoma. Quantitative edge analysis can be promptly performed on select border fragments in MDCT images, providing a useful supporting tool for diagnostics and a possible starting point for machine learning recognition based on lower-dimensional feature space. Full article
(This article belongs to the Special Issue Abdominal Imaging: Recent Advances and Future Trends)
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<p>Postcontrast arterial MDCT axial image of adenocarcinoma of the tail of the pancreas (<b>a</b>). Screenshot of the GUI of the software used (<b>b</b>) with blue box positioned on normal parenchyma and the red box positioned on an adenocarcinoma of the tail of the pancreas. The graphic output of the results from the Canny edge detection and the subsequent average boundary line for both the boxes selected are visible.</p>
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<p>PMS values of cancerous and healthy pancreatic borders (whisker plot).</p>
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<p>Visual plot of PMS data of adenocarcinoma and normal parenchyma and separation between cancerous (red) and healthy (blue) pancreas edge fragments.</p>
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<p>ROC analysis of PMS values of healthy and neoplastic pancreatic margins.</p>
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15 pages, 1888 KiB  
Review
Direct and Indirect Measurements of the 19F(p,α)16O Reaction at Astrophysical Energies Using the LHASA Detector and the Trojan Horse Method
by Giovanni L. Guardo, Giuseppe G. Rapisarda, Dimiter L. Balabanski, Giuseppe D’Agata, Alessia Di Pietro, Pierpaolo Figuera, Marco La Cognata, Marco La Commara, Livio Lamia, Dario Lattuada, Catalin Matei, Marco Mazzocco, Alessandro A. Oliva, Sara Palmerini, Teodora Petruse, Rosario G. Pizzone, Stefano Romano, Maria Letizia Sergi, Roberta Spartá, Xuedou Su, Aurora Tumino and Nikola Vukmanadd Show full author list remove Hide full author list
Universe 2024, 10(7), 304; https://doi.org/10.3390/universe10070304 - 22 Jul 2024
Viewed by 485
Abstract
Fluorine is one of the most interesting elements in nuclear astrophysics. Its abundance can provide important hints to constrain the stellar models since fluorine production and destruction are strictly connected to the physical conditions inside the stars. The F19(p,α)16O [...] Read more.
Fluorine is one of the most interesting elements in nuclear astrophysics. Its abundance can provide important hints to constrain the stellar models since fluorine production and destruction are strictly connected to the physical conditions inside the stars. The F19(p,α)16O reaction is one of the fluorine burning processes and the correction evaluation of its reaction rate is of pivotal importance to evaluate the fluorine abundance. Moreover, the F19(p,α)16O reaction rate can have an impact for the production of calcium in the first-generation of Population III stars. Here, we present the AsFiN collaboration efforts to the study of the F19(p,α)16O reaction by means of direct and indirect measurements. On the direct measurements side, an experimental campaign aimed to the measurement of the F19(p,α0,π)16O reaction is ongoing, taking advantage of the new versatile arrays of silicon strip detectors, LHASA and ELISSA. Moreover, the Trojan Horse Method (THM) was used to determine the F19(p,α0)16O reaction S(E)-factor in the energy range of astrophysical interest (Ecm≈ 0–1 MeV), showing, for the first time, the presence of resonant structures within the astrophysical energy range. THM has been also applied for the study of the F19(p,απ)16O reaction; data analysis is ongoing. Full article
(This article belongs to the Special Issue Recent Outcomes and Future Challenges in Nuclear Astrophysics)
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<p>Available direct data for the <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">F</mi> <none/> <none/> <mprescripts/> <none/> <mn>19</mn> </mmultiscripts> </semantics></math>(p,<math display="inline"><semantics> <msub> <mi>α</mi> <mn>0</mn> </msub> </semantics></math>)<math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">O</mi> <none/> <none/> <mprescripts/> <none/> <mn>16</mn> </mmultiscripts> </semantics></math> reaction. The empty red circles show the data of [<a href="#B15-universe-10-00304" class="html-bibr">15</a>], the empty blue squares the data of [<a href="#B16-universe-10-00304" class="html-bibr">16</a>], the green triangles the data of [<a href="#B17-universe-10-00304" class="html-bibr">17</a>], the black stars the data of [<a href="#B20-universe-10-00304" class="html-bibr">20</a>] and the black circles the data of [<a href="#B19-universe-10-00304" class="html-bibr">19</a>].</p>
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<p>Picture of the detector LHASA used for the experiment.</p>
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<p>Comparison between experimental data (coloured points) and simulated one (black points) for the beam energy of 18.5 MeV (see text for details).</p>
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<p>Angular distribution for 725 keV in the center-of-mass system. The experimental points (blue symbols) are overlapped with a sum of the first 5-order Legendre polynomials (red line).</p>
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<p>Scheme of the TH reaction <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">H</mi> <none/> <none/> <mprescripts/> <none/> <mn>2</mn> </mmultiscripts> </semantics></math>(<math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">F</mi> <none/> <none/> <mprescripts/> <none/> <mn>19</mn> </mmultiscripts> </semantics></math>,<math display="inline"><semantics> <mi>α</mi> </semantics></math><math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">O</mi> <none/> <none/> <mprescripts/> <none/> <mn>16</mn> </mmultiscripts> </semantics></math>)n in QF kinematics.</p>
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<p>Sketch of the experimental setup.</p>
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<p>Experimental three-body Q-value. The main peak is due to the reaction channel of interest <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">H</mi> <none/> <none/> <mprescripts/> <none/> <mn>2</mn> </mmultiscripts> </semantics></math><math display="inline"><semantics> <msup> <mo>(</mo> <mn>19</mn> </msup> </semantics></math>F,<math display="inline"><semantics> <mi>α</mi> </semantics></math><math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">O</mi> <none/> <none/> <mprescripts/> <none/> <mn>16</mn> </mmultiscripts> </semantics></math>)n. The arrow indicates the theoretical value.</p>
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<p>Experimental momentum distribution (full dots) compared with theoretical distribution, given by the square of the Hulthèn wave function in momentum space (red solid line) (adapted from [<a href="#B7-universe-10-00304" class="html-bibr">7</a>]).</p>
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<p>THM triple differential cross-section of the <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">F</mi> <none/> <none/> <mprescripts/> <none/> <mn>19</mn> </mmultiscripts> </semantics></math>(p,<math display="inline"><semantics> <msub> <mi>α</mi> <mn>0</mn> </msub> </semantics></math>)<math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">O</mi> <none/> <none/> <mprescripts/> <none/> <mn>16</mn> </mmultiscripts> </semantics></math> reaction. The vertical error bars consider the statistical uncertainty only. The horizontal error bars are due to the size of the integration bin. The black line interpolates experimental data [<a href="#B7-universe-10-00304" class="html-bibr">7</a>].</p>
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<p>Comparison between the THM data (black dots [<a href="#B7-universe-10-00304" class="html-bibr">7</a>]) and the direct data obtained with the LHASA detector (red dots [<a href="#B25-universe-10-00304" class="html-bibr">25</a>]). The excellent agreement is a clear demonstration of the consistency and solidity of the direct and indirect approaches.</p>
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<p>S(E)-factor of the <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">F</mi> <none/> <none/> <mprescripts/> <none/> <mn>19</mn> </mmultiscripts> </semantics></math>(p,<math display="inline"><semantics> <msub> <mi>α</mi> <mi>π</mi> </msub> </semantics></math>)<math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">O</mi> <none/> <none/> <mprescripts/> <none/> <mn>16</mn> </mmultiscripts> </semantics></math> reaction as a function of the center-of-mass energy. Experimental data are from [<a href="#B17-universe-10-00304" class="html-bibr">17</a>] (open diamonds), [<a href="#B18-universe-10-00304" class="html-bibr">18</a>] (open stars), [<a href="#B45-universe-10-00304" class="html-bibr">45</a>] (open circles) and [<a href="#B46-universe-10-00304" class="html-bibr">46</a>] (open squares). The red solid line represents the result an R-matrix fit of data, considering the contribution of the 13.095 MeV state of <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">Na</mi> <none/> <none/> <mprescripts/> <none/> <mn>20</mn> </mmultiscripts> </semantics></math>. Dashed blue line represents the R-matrix fit without the contribution of the mentioned <math display="inline"><semantics> <mmultiscripts> <mi mathvariant="normal">Na</mi> <none/> <none/> <mprescripts/> <none/> <mn>20</mn> </mmultiscripts> </semantics></math> state [<a href="#B47-universe-10-00304" class="html-bibr">47</a>].</p>
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<p>Monte Carlo simulation for the expected reaction channels. See text for details.</p>
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<p>Picture of the experimental setup used for the experiment. A scaled version of the full ELISSA array (one ring on top) was coupled with the LHASA array (down in the picture).</p>
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25 pages, 541 KiB  
Review
Magnetocaloric Refrigeration in the Context of Sustainability: A Review of Thermodynamic Bases, the State of the Art, and Future Prospects
by Umberto Lucia and Giulia Grisolia
Energies 2024, 17(14), 3585; https://doi.org/10.3390/en17143585 - 21 Jul 2024
Viewed by 520
Abstract
At present, one of the main challenges that industry faces is its impact on global warming, linked to the greenhouse effect and ozone hole problems. These two environmental issues have not yet been solved completely and, concerning the industrial cold sector, countries are [...] Read more.
At present, one of the main challenges that industry faces is its impact on global warming, linked to the greenhouse effect and ozone hole problems. These two environmental issues have not yet been solved completely and, concerning the industrial cold sector, countries are making various decisions on refrigerants. Magnetic refrigeration potentially represents a less impactful refrigeration technology. In this review, the physical basis of magnetic refrigeration is analysed, in order to propose this technology for industrial use. Full article
(This article belongs to the Section A: Sustainable Energy)
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<p>A simplified scheme of a magnetic refrigeration cycle, considering adiabatic conditions.</p>
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<p>Temperature vs entropy, Ericsson (<b>a</b>) and Brayton (<b>b</b>) magnetic cycles.</p>
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<p>Working principle scheme of a linear AMR evolving with a Brayton-like thermodynamic cycle, where the magnet is displaced linearly (movement indicated with arrows). In phase (<b>a</b>) the magnetisation occurs. In (<b>b</b>) the heat is rejected to the hot sink, while the (<b>c</b>) phase represents demagnetisation, which is followed by (<b>d</b>), where the useful effect occurs.</p>
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<p>Simplified scheme of a single-effect device with linear motion for the permanent magnet in relation to the active magnetocaloric material (MCM) as described in Ref. [<a href="#B79-energies-17-03585" class="html-bibr">79</a>].</p>
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<p>Simplified scheme of a double-effect device (described in [<a href="#B79-energies-17-03585" class="html-bibr">79</a>]) with a moving magnet. The bidirectional pumps are able to provide the alternate carrier fluid flow; in order to work properly, the bidirectional flow has to be synchronised.</p>
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<p>Simplified scheme for moving the active magnetocaloric material device as described in [<a href="#B79-energies-17-03585" class="html-bibr">79</a>]. Configuration (<b>1</b>) presents a bidirectional pump and the linear motion of the active magnetocaloric material (two beds within a moving slider), where the magnet has a fixed position. Configuration (<b>2</b>) presents a unidirectional pump with three-way microvalves with the aim of improving the efficiency of the system. The external grey pipes contain dead fluid.</p>
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<p>According to the configuration of a moving active material (<a href="#energies-17-03585-f006" class="html-fig">Figure 6</a>), it is possible to evolve towards two different rotating systems, with the first being a continuous motion (<b>a</b>) and the other being a continuous or discontinuous rotation along the axis parallel to the fluid flow circuit (<b>b</b>).</p>
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18 pages, 4988 KiB  
Article
Living Walls and Green Façades: An Implementation Code for Energy Simulation
by Valeria Nesci, Ilaria Ballarini, Pietro Rando Mazzarino and Vincenzo Corrado
Buildings 2024, 14(7), 2040; https://doi.org/10.3390/buildings14072040 - 4 Jul 2024
Viewed by 433
Abstract
The impacts of climate change, excessive greenhouse gas emissions, and the current energy crisis have motivated the European Union to adopt mitigation and adaptation strategies. These strategies primarily focus on the building sector due to its crucial role in addressing these issues. Among [...] Read more.
The impacts of climate change, excessive greenhouse gas emissions, and the current energy crisis have motivated the European Union to adopt mitigation and adaptation strategies. These strategies primarily focus on the building sector due to its crucial role in addressing these issues. Among the strategies, the implementation of resilient technologies for the building envelope, such as vertical greenery systems (VGSs) is gaining ground. The literature analysis shows that existing models are not sufficiently detailed in their description of the overall thermo-physical phenomena of VGSs. The aim of this work is to overcome the research gaps by selecting and improving two mathematical models for green façades and living walls. A dedicated calculation code to estimate the effect of VGSs on a building’s energy performance and indoor thermal comfort has been developed and implemented within the EnergyPlus calculation software (version 23.2). A BESTest Case from ASHRAE 140 was chosen to test the models and to assess benefits of VGSs. The results show that adopting green solutions for the building envelope can contribute to achieving the building’s energy efficiency goals and that the modelling of these technologies can be easily carried out within a dynamic energy simulation of the building. Full article
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<p>VGS classification.</p>
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<p>Interaction between Python (version 3.8) and EnergyPlus environments.</p>
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<p>Model algorithm schema: (<b>a</b>) green façade, (<b>b</b>) living wall.</p>
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<p>Base case study (900FF BESTest Case of ANSI/ASHRAE 140-2020 standard).</p>
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<p>Final geometrical configuration of the case study.</p>
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<p>Simulation of the green façade. Comparison of external surface temperature profiles—10 December.</p>
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<p>Simulation of the green façade. Comparison of external surface temperature profiles—17 August.</p>
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<p>Simulation of the green façade. Comparison of the ideal thermal energy need for heating (<span class="html-italic">EP</span><sub>H,nd</sub>) and for cooling (<span class="html-italic">EP</span><sub>C,nd</sub>) on a monthly basis.</p>
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<p>Simulation of the green façade. Sensitivity analysis: LAI variation.</p>
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<p>Simulation of the living wall. Comparison of external surface temperature profiles—10 December.</p>
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<p>Simulation of the living wall. Comparison of external surface temperature profiles—17 August.</p>
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<p>Simulation of the living wall. Comparison of the ideal thermal energy need for heating (<span class="html-italic">EP</span><sub>H,nd</sub>) and for cooling (<span class="html-italic">EP</span><sub>C,nd</sub>) on a monthly basis.</p>
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<p>Simulation of the living wall. Sensitivity analysis: LAI variation.</p>
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<p>Simulation of the living wall. Sensitivity analysis: thickness substrate variation.</p>
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10 pages, 1350 KiB  
Article
Fitting the Crab Supernova with a Gamma-Ray Burst
by Remo Ruffini and Costantino Sigismondi
Universe 2024, 10(7), 275; https://doi.org/10.3390/universe10070275 - 25 Jun 2024
Viewed by 977
Abstract
Here, we reconsider the historical data, assuming a gamma-ray burst (GRB) as its source. A Supernova correlated with the GRB explains well the fading time observed by the ancient Chinese astronomers in the daytime and the nighttime, while the GRB power law explains [...] Read more.
Here, we reconsider the historical data, assuming a gamma-ray burst (GRB) as its source. A Supernova correlated with the GRB explains well the fading time observed by the ancient Chinese astronomers in the daytime and the nighttime, while the GRB power law explains the present X-rays and GeV emission of the Crab. On the grounds of a recent understanding of the first episode of binary-driven hypernova GRB (BDHN GRB) in terms of the collapse of a ten solar masses core, we propose the possible identification of the real Supernova event at an earlier time than Chinese chronicles. This work allows a new understanding of the significance of historical astronomical observations, including a fireball due to gamma-ray air shower observation and a plague of acute radiation syndrome, documented with several thousands of victims in the Eurasian area (Egypt, Iraq, and Syria). Full article
(This article belongs to the Section Stellar Astronomy)
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<p>The light curve of the GRB 190114C extrapolated for 10<sup>3</sup> years or 3·10<sup>10</sup> s. Each 10<sup>2</sup> factor in luminosity corresponds to 5 magnitudes (Pogson’s law).The Crab Nebula integrated flux values are represented by the three colored hexagons in Optical (red), X-rays (grey), and GeV (green). The apparent magnitudes are calculated if this GRB would have exploded at the distance of the Crab. Daytime visibility is better established with a magnitude brighter than m<sub>v</sub> = −5.4 (Venus is m<sub>v</sub> = −4.5 at its maximum), and the Supernova remained visible 23 days in the daytime, according to the <span class="html-italic">Sung-hui-yao</span> chronicle. After 21 months or 650 days, the optical afterglow of our reference GRB would reach the magnitude of Vega.</p>
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<p>Pictograph at the White Mesa (Arizona) already interpreted as the Crescent of the Moon and the Supernova since 1955. As with other pictographs of this type, the star appears always of similar size to the Moon, rayed or surrounded by circles, as in the case of fireball.</p>
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<p>The most famous “Supernova Pictograph” at the Penasco Blanco Canyon (New Mexico). The Supernova is as big as the Moon. In our vision, this was the dawn of 3 July 1054, at 11 UT, with the GRB exploded, around 10° above the east horizon still dark.</p>
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40 pages, 5502 KiB  
Review
Technological Elements behind the Renewable Energy Community: Current Status, Existing Gap, Necessity, and Future Perspective—Overview
by Shoaib Ahmed, Amjad Ali, Alessandro Ciocia and Antonio D’Angola
Energies 2024, 17(13), 3100; https://doi.org/10.3390/en17133100 - 24 Jun 2024
Cited by 1 | Viewed by 705
Abstract
The Renewable Energy Community (REC) in Europe promotes renewable energy sources (RESs), offering social, economic, and environmental benefits. This new entity could alter consumer energy relationships, requiring self-consumption, energy sharing, and full utilization of RESs. Modernizing energy systems within the REC requires addressing [...] Read more.
The Renewable Energy Community (REC) in Europe promotes renewable energy sources (RESs), offering social, economic, and environmental benefits. This new entity could alter consumer energy relationships, requiring self-consumption, energy sharing, and full utilization of RESs. Modernizing energy systems within the REC requires addressing self-consumption, energy sharing, demand response, and energy management system initiatives. The paper discusses the role of decentralized energy systems, the scenarios of the REC concept and key aspects, and activities involving energy generation, energy consumption, energy storage systems, energy sharing, and EV technologies. Moreover, the present work highlights the research gap in the existing literature and the necessity of addressing the technological elements. It also highlights that there is no uniform architecture or model for the REC, like in the case of microgrids. Additionally, the present work emphasizes the role and importance of technological elements in RECs, suggesting future recommendations for EMS, DSM, data monitoring and analytics, communication systems, and the software or tools to ensure reliability, efficiency, economic, and environmental measures. The authors also highlight the crucial role of policymakers and relevant policies, which could help in implementing these technological elements and show the importance of the RECs for a sustainable energy shift and transition. Full article
(This article belongs to the Section C: Energy Economics and Policy)
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<p>Representation of electric power system with distributed renewable energy sources.</p>
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<p>Energy community benefits [<a href="#B16-energies-17-03100" class="html-bibr">16</a>].</p>
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<p>Overall workflow.</p>
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<p>Renewable Energy Community technological activities.</p>
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<p>Types of Consumption, prosumer, and producer differences.</p>
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<p>Different schematic diagrams for the prosumers.</p>
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<p>ESS classification.</p>
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<p>Key elements of renewable energy community.</p>
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<p>Energy community architectures or layouts.</p>
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<p>EMS Platform of Prosumer.</p>
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<p>(<b>a</b>,<b>b</b>) DSM categories (<b>c</b>) Different DSM approaches and categories.</p>
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<p>Different Monitoring Systems.</p>
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<p>Communication technologies and applications [<a href="#B182-energies-17-03100" class="html-bibr">182</a>].</p>
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<p>Communication technologies and applications.</p>
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17 pages, 9960 KiB  
Article
A Comprehensive Signal Quality Assessment for BDS/Galileo/GPS Satellites and Signals
by Yijun Tian, Guorui Xiao, Rui Guo, Dongqing Zhao, Lu Zhang, Jie Xin, Jinglei Guo, Yuechao Han, Xuefan Du, Donghan He and Zheng Qin
Remote Sens. 2024, 16(13), 2277; https://doi.org/10.3390/rs16132277 - 21 Jun 2024
Viewed by 418
Abstract
With the modernization of global navigation satellite systems (GNSS), especially the rapid development of the BeiDou Navigation Satellite System (BDS), more observations of satellites and signals have become available. Using data of the globally distributed MGEX stations, a systematic and comprehensive evaluation of [...] Read more.
With the modernization of global navigation satellite systems (GNSS), especially the rapid development of the BeiDou Navigation Satellite System (BDS), more observations of satellites and signals have become available. Using data of the globally distributed MGEX stations, a systematic and comprehensive evaluation of signal characteristics for BDS-3, BDS-2, GPS, and Galileo is conducted in terms of carrier-to-noise ratio (C/N0), code noise, and multipath in the contribution. First, a comprehensive signal quality assessment method for BDS/Galileo/GPS satellites and signals is proposed, including C/N0 modeling and MP modeling. For BDS, the BDS-3 satellites apparently have higher signal power than the BDS-2 satellites at the same frequency such as B1I and B3I, and the signal B2a of BDS-3 is superior to other signals in regard to signal power, which is comparable with the superior Galileo E5 signals and GPS L5. Among all the signals, the observation accuracy of E5 is the highest regardless of receiver types, and next highest are BDS-3 B2a and GPS L5. Due to not being affected by the systematic code errors of BDS-2, the observations of BDS-3 satellites contain smaller multipath errors than that of BDS-2 satellites. As for the multipath suppression performance, the BDS-3 signal B2a, GPS L5, and Galileo E5 and E5b perform better than the other signals, which may be related to their wide signal bandwidths. Full article
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<p>Average <span class="html-italic">C/N0</span> values against the elevations of all the satellites for BDS B1I/B2I/B3I/B2a based on observations collected from MGEX stations during DOY 134–140 in 2019. Only the results of the representative receiver type JAVAD are plotted. (II: BDS-2; IIIs: BDS-3 experimental system; III: BDS-3).</p>
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<p>Average C/N0s against the elevations of different signals. The left panel is only for the BDS signals, while the right panel is for all the signals of BDS-3, Galileo, and GPS.</p>
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<p>Comparison of <span class="html-italic">C/N0</span> values at different signals for different receiver types. The horizontal axis in subfigure (<b>a</b>) represents 15 stations with the receiver type JAVAD, while that in subfigure (<b>b</b>) represents 24 stations with the receiver type LEICA, that in subfigure (<b>c</b>) represents 29 stations with the receiver type SEPT, and that in subfigure (<b>d</b>) represents 40 stations with the receiver type TRIMBLE.</p>
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<p>Time series of CC values of the BDS-3 C35 satellite at the B2a signal during DOY 134–140 in 2019. The satellite elevation over time is indicated by the gray line.</p>
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<p>Time series of CC values of the four selected BDS-3 satellites at B1I/B3I/B2a during DOY 134–140 in 2019.</p>
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<p>Time series of CC values for BDS-2 (C5, C6, and C12), Galileo (E12 and E31), and GPS (G15, G11, and G24) satellites at different signals during DOY 134–140 in 2019. Legends B1I (light green), B2I (bright green), and B3I (light blue) are for BDS satellites C5, C6, and C12. Legends E1 (light blue), E5a (light green), E6 (bright green), and E5b (light yellow) are for Galileo satellites E12 and E31. Legends L1 (light blue), L2 (light green), L5 (bright green) are for GPS satellites G15, G11 and G24.</p>
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<p>Comparison of average CC STD values in different stations. The horizontal axis in subfigure (<b>a</b>) represents 15 stations with receiver type JAVAD, while that in subfigure (<b>b</b>) represents 24 stations with receiver type LEICA, that in subfigure (<b>c</b>) represents 29 stations with receiver type SEPT, and that in subfigure (<b>d</b>) represents 40 stations with receiver type TRIMBLE. In each subgraph, the 4 panels are for BDS-3 B1I/B3I/B2a, BDS-2 B1I/B2I/B3I, GPS L1/L2/L5, and Galileo E1/E5a/E6/E5b/E5, respectively.</p>
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<p>Multipath values against satellite elevation for BDS-3 C19, C21, C23, and C35 satellites during DOY 134–140 in 2019. MPC stands for Multipath Combination.</p>
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<p>Multipath values against satellite elevation for BDS-2 (C5, C21, and C23), Galileo (E12 and E31), and GPS (G15, G11, and G24) satellites during DOY 134–140 in 2019. Legends B1I (light blue), B2I (light green) and B3I (bright green) are for BDS satellites C5, C6, and C12. Legends E1 (light blue), E5a (light green), E6 (bright green), and E5b (light yellow) are for Galileo satellites E12 and E31. Legends L1 (light blue), L2 (light green) and L5 (bright green) are for GPS satellites G15, G11 and G24.</p>
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<p>STDs of multipath combinations for different satellites. The four panels from top to bottom are for BDS-3, BDS-2, GPS, and Galileo satellites, respectively.</p>
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<p>Comparison of average MPC STD values in different stations. The horizontal axis in subfigure (<b>a</b>) represents 15 stations with receiver type JAVAD, while that in subfigure (<b>b</b>) represents 24 stations with receiver type LEICA, that in subfigure (<b>c</b>) represents 29 stations with receiver type SEPT, and that in subfigure (<b>d</b>) represents 40 stations with receiver type TRIMBLE. In each subgraph, the 4 panels are for BDS-3 B1I/B3I/B2a, BDS-2 B1I/B2I/B3I, GPS L1/L2/L5, and Galileo E1/E5a/E6/E5b/E5, respectively.</p>
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18 pages, 1120 KiB  
Article
An Enhanced FGI-GSRx Software-Defined Receiver for the Execution of Long Datasets
by Muwahida Liaquat, Mohammad Zahidul H. Bhuiyan, Saiful Islam, Into Pääkkönen and Sanna Kaasalainen
Sensors 2024, 24(12), 4015; https://doi.org/10.3390/s24124015 - 20 Jun 2024
Viewed by 469
Abstract
The Global Navigation Satellite System (GNSS) software-defined receivers offer greater flexibility, cost-effectiveness, customization, and integration capabilities compared to traditional hardware-based receivers, making them essential for a wide range of applications. The continuous evolution of GNSS research and the availability of new features require [...] Read more.
The Global Navigation Satellite System (GNSS) software-defined receivers offer greater flexibility, cost-effectiveness, customization, and integration capabilities compared to traditional hardware-based receivers, making them essential for a wide range of applications. The continuous evolution of GNSS research and the availability of new features require these software-defined receivers to upgrade continuously to facilitate the latest requirements. The Finnish Geospatial Research Institute (FGI) has been supporting the GNSS research community with its open-source implementations, such as a MATLAB-based GNSS software-defined receiver `FGI-GSRx’ and a Python-based implementation `FGI-OSNMA’ for utilizing Galileo’s Open Service Navigation Message Authentication (OSNMA). In this context, longer datasets are crucial for GNSS software-defined receivers to support adaptation, optimization, and facilitate testing to investigate and develop future-proof receiver capabilities. In this paper, we present an updated version of FGI-GSRx, namely, FGI-GSRx-v2.0.0, which is also available as an open-source resource for the research community. FGI-GSRx-v2.0.0 offers improved performance as compared to its previous version, especially for the execution of long datasets. This is carried out by optimizing the receiver’s functionality and offering a newly added parallel processing feature to ensure faster capabilities to process the raw GNSS data. This paper also presents an analysis of some key design aspects of previous and current versions of FGI-GSRx for a better insight into the receiver’s functionalities. The results show that FGI-GSRx-v2.0.0 offers about a 40% run time execution improvement over FGI-GSRx-v1.0.0 in the case of the sequential processing mode and about a 59% improvement in the case of the parallel processing mode, with 17 GNSS satellites from GPS and Galileo. In addition, an attempt is made to execute v2.0.0 with MATLAB’s own parallel computing toolbox. A detailed performance comparison reveals an improvement of about 43% in execution time over the v2.0.0 parallel processing mode for the same GNSS scenario. Full article
(This article belongs to the Special Issue GNSS Software-Defined Radio Receivers: Status and Perspectives)
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<p>FGI-GSRx sequential architecture. The green parts indicate the option to use a pre-stored output from acquisition and tracking.</p>
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<p>FGI-GSRx-v2.0.0 architecture. The green parts indicate the option to use a pre-stored output from acquisition and tracking.</p>
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<p>FGI-GSRx-v2.0.0 parallel tracking mode work flow.</p>
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<p>FGI-GSRx-v2.0.0 two-stage acquisition.</p>
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<p>Sky plots for GPS and Galileo satellites at the beginning of data collection.</p>
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<p>Processor usage utilization for the entire simulation interval for the sequential processing mode of FGI-GSRx.</p>
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<p>Galileo only: CPU usage for signal tracking of the v2.0.0 (<b>left</b>) Parallel processing mode. (<b>right</b>) Sequential processing with MATLAB parallel computing block.</p>
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<p>GPS only: CPU usage for signal tracking of the v2.0.0 (<b>left</b>) Parallel processing mode. (<b>right</b>) Sequential processing with MATLAB parallel computing block.</p>
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<p>GPS and Galileo: CPU usage for signal tracking of the v2.0.0 (<b>left</b>) Parallel processing mode. (<b>right</b>) Sequential processing with MATLAB parallel computing block.</p>
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<p>Position deviation plots generated by FGI-GSRx.</p>
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19 pages, 6411 KiB  
Review
The Hearth of the World: The Sun before Astrophysics
by Gábor Kutrovátz
Universe 2024, 10(6), 256; https://doi.org/10.3390/universe10060256 - 7 Jun 2024
Viewed by 538
Abstract
This paper presents a historical overview of conceptions about the Sun in Western astronomical and cosmological traditions before the advent of spectroscopy and astrophysics. Rather than studying general cultural ideas, we focus on the concepts developed by astronomers or by natural philosophers impacting [...] Read more.
This paper presents a historical overview of conceptions about the Sun in Western astronomical and cosmological traditions before the advent of spectroscopy and astrophysics. Rather than studying general cultural ideas, we focus on the concepts developed by astronomers or by natural philosophers impacting astronomy. The ideas we investigate, from the works of Plato and Aristotle to William Herschel and his contemporaries, do not line up into a continuous and integrated narrative, since the nature of the Sun was not a genuine scientific topic before the nineteenth century. However, the question recurringly arose as embedded in cosmological and physical contexts. By outlining this heterogeneous story that spreads from transcendence to materiality, from metaphysics to physics, from divinity to solar inhabitants, we receive insight into some major themes and trends both in the general development of astronomical and cosmological thought and in the prehistory of modern solar science. Full article
(This article belongs to the Special Issue Solar and Stellar Activity: Exploring the Cosmic Nexus)
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<p>The chariot of Helios depicted on a krater from around 430 BCE (now in the British Museum, London). (Source: Wikimedia Commons).</p>
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<p>Medieval and renaissance solar imagery often personified the Sun, as seen in, e.g., Johannes Sacrobosco’s <span class="html-italic">De sphaera mundi</span> [<a href="#B38-universe-10-00256" class="html-bibr">38</a>].</p>
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<p>Raphael’s fresco the <span class="html-italic">Disputation of the Holy Sacrament</span> (Apostolic Palace, Vatican, 1509–1510). The central axis, representing the Holy Spirit, is laden with solar symbolism. (Source: Wikimedia Commons).</p>
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<p>Johannes Kepler’s depiction of the immaterial force emitted by the Sun and magnetically shaping planetary orbit [<a href="#B58-universe-10-00256" class="html-bibr">58</a>]. Capital letters designate different positions of the Earth along its orbit, and the arrows indicate the Earth’s purported “magnetic axis” (which, for Kepler, is different from the actual magnetic axis going through the magnetic poles and is parallel with the orbital plane).</p>
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<p>Galileo Galilei’s illustration of illusory telescopic solar images, in contrast with genuine ones (not shown here), provided that the spots were caused by spiders and flies (<b>A</b>), undulating sashes (<b>B</b>), clouds (<b>C</b>), waterdrops (<b>D</b>) or different kinds of bubbles (<b>E</b>–<b>G</b>) [<a href="#B69-universe-10-00256" class="html-bibr">69</a>]. For details, see [<a href="#B68-universe-10-00256" class="html-bibr">68</a>] (pp. 211–216). The image is rotated to fit better.</p>
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<p>Athanasius Kircher’s imaginative drawing of a hectic solar surface, from his <span class="html-italic">Mundus subterraneus</span> (1665) [<a href="#B76-universe-10-00256" class="html-bibr">76</a>].</p>
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<p>René Descartes’s drawing of the Sun (S) among other stars (D, L, F, f, Y), each surrounded by their vortices indicated by the dotted curves [<a href="#B80-universe-10-00256" class="html-bibr">80</a>]. A, E, I, V, B, X are points where adjacent vortices meet. N is a comet, thought to be an interstellar traveller.</p>
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<p>William Herschel’s drawings of a sunspot, in [<a href="#B99-universe-10-00256" class="html-bibr">99</a>] (Plate XVIII), interpreted as “an opening in the luminous solar clouds” (p. 318). His “Fig. 1.” depicts the optical phenomenon, and “Fig. 2.” shows a vertical cross section where AB is the opaque surface, PF is the dense inferior atmosphere, and <span class="html-italic">gh</span> is the luminous superior atmosphere. The remaining letters serve to identify parts of the phenomenon (umbra, penumbra) with elements of the structural interpretation on the right.</p>
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17 pages, 15497 KiB  
Article
Novel Aluminum Alloy Tailored for Additive Manufacturing: Structural Characterization and Qualification Perspectives
by Maurizio Arena, Bharat Mehta, Tommaso Tirelli, Paolo Ambrogiani, Martina Castaldo, Sven Bengtsson and Lars Nyborg
Appl. Sci. 2024, 14(11), 4647; https://doi.org/10.3390/app14114647 - 28 May 2024
Viewed by 761
Abstract
The recent advances achieved in additive manufacturing (AM) technology demonstrate the potential to realize customized metal components, ensuring weight reduction opportunities. These benefits make AM attractive for high-cost aerospace applications, especially where high geometric complexity is required. In the context of an EU [...] Read more.
The recent advances achieved in additive manufacturing (AM) technology demonstrate the potential to realize customized metal components, ensuring weight reduction opportunities. These benefits make AM attractive for high-cost aerospace applications, especially where high geometric complexity is required. In the context of an EU research scenario, the H2020 MANUELA (Additive Manufacturing Using Metal Pilot Line) project promotes the development of new technologies for design optimization by enabling the application of novel materials in AM. This paper illustrates recent advances in a new aluminum alloy (Al-HS1) with high strength emphasizing all of the characterization steps at the coupon level. This material has been employed in the re-engineering of a conventional hydraulic manifold using a powder bed fusion-laser beam (PBF-LB) process. Both the simulations and structural tests allowed for proving its compliance and technological maturity with industrial standards and applicable airworthiness requirements. Full article
(This article belongs to the Special Issue Additive Manufacturing Technology and Applications for Aerospace)
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<p>AM building blocks: the main steps toward the certification of parts.</p>
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<p>Engineering end-to-end process addressed for Al-HS1 qualification.</p>
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<p>Bending fatigue sample after machining: (<b>a</b>) dog bone sample geometry; (<b>b</b>) test setup for the four-point bending test.</p>
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<p>(<b>a</b>) Optical microscopic image of a sample along the building direction (BD); (<b>b</b>) SEM images showing the microstructure with insets focusing on precipitates at melt pool boundaries (red) and grain boundaries (yellow) respectively.</p>
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<p>Bending fatigue data at R = −1.0 for the Al-HS1 printed along the building direction. Run-out samples (at 2 × 10<sup>6</sup> cycles) are spread along the X-axis for the visualization. The fatigue strength range is as reported for AlSi10Mg in the literature [<a href="#B69-applsci-14-04647" class="html-bibr">69</a>].</p>
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<p>Fractography tests on Al-HS1 after the bending fatigue tests: (<b>a</b>) low cycle fatigue sample; (<b>b</b>) high cycle fatigue sample.</p>
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<p>Details of the hydraulic manifold channels: (<b>a</b>) former geometry; (<b>b</b>) after the optimization.</p>
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<p>Manifold after printing: (<b>a</b>) before drilling; manifold after machining and postprocessing heat treatment; (<b>b</b>) thread detail (top); (<b>c</b>) plugs threads detail (front).</p>
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<p>Details of the three-dimensional FE model: (<b>a</b>) 3D model; (<b>b</b>) inner walls; (<b>c</b>) constraints; (<b>d</b>) internal pressure.</p>
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<p>Stress maps (limit pressure load, PP = 31.05 [MPa]): (<b>a</b>) Von Mises; (<b>b</b>) max principal; (<b>c</b>) Von Mises peak (inner flow channels); (<b>d</b>) max principal peak (inner flow channels).</p>
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<p>Fatigue life calculations of the manifold at a pulsating pressure for the Al-HS1 and AlSi10Mg alloys.</p>
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<p>Hydraulic manifold test articles: (<b>a</b>) AlSi10Mg [<a href="#B57-applsci-14-04647" class="html-bibr">57</a>]; (<b>b</b>) Al-HS1 type.</p>
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<p>Hydraulic manifold test stand: (<b>a</b>) hydraulic layout; (<b>b</b>) pressure load profiles.</p>
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<p>NDI of the hydraulic manifold: (<b>a</b>) disassembled test article; (<b>b</b>) UV images.</p>
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12 pages, 1913 KiB  
Article
Decreased Hepatic and Serum Levels of IL-10 Concur with Increased Lobular Inflammation in Morbidly Obese Patients
by Helena Solleiro-Villavicencio, Lucía Angélica Méndez-García, Nydia A. Ocampo-Aguilera, Itzel Baltazar-Pérez, José A. Arreola-Miranda, José A. Aguayo-Guerrero, Ana Alfaro-Cruz, Antonio González-Chávez, Miguel A. Fonseca-Sánchez, José Manuel Fragoso and Galileo Escobedo
Medicina 2024, 60(6), 862; https://doi.org/10.3390/medicina60060862 - 25 May 2024
Viewed by 758
Abstract
Background and Objectives: Non-alcoholic fatty liver disease (NAFLD) is associated with obesity and ranges from simple steatosis to non-alcoholic steatohepatitis (NASH), fibrosis, cirrhosis, and hepatocellular carcinoma. Accumulating evidence in animal models suggests that loss of interleukin-10 (IL-10) anti-inflammatory actions might contribute to [...] Read more.
Background and Objectives: Non-alcoholic fatty liver disease (NAFLD) is associated with obesity and ranges from simple steatosis to non-alcoholic steatohepatitis (NASH), fibrosis, cirrhosis, and hepatocellular carcinoma. Accumulating evidence in animal models suggests that loss of interleukin-10 (IL-10) anti-inflammatory actions might contribute to lobular inflammation, considered one of the first steps toward NASH development. However, the role of IL-10 in lobular inflammation remains poorly explored in humans. We examined mRNA and protein levels of IL-10 in liver biopsies and serum samples from morbidly obese patients, investigating the relationship between IL-10 and lobular inflammation degree. Materials and Methods: We prospectively enrolled morbidly obese patients of both sexes, assessing the lobular inflammation grade by the Brunt scoring system to categorize participants into mild (n = 7), moderate (n = 19), or severe (n = 13) lobular inflammation groups. We quantified the hepatic mRNA expression of IL-10 by quantitative polymerase chain reaction and protein IL-10 levels in liver and serum samples by Luminex Assay. We estimated statistical differences by one-way analysis of variance (ANOVA) and Tukey’s multiple comparison test. Results: The hepatic expression of IL-10 significantly diminished in patients with severe lobular inflammation compared with the moderate lobular inflammation group (p = 0.01). The hepatic IL-10 protein levels decreased in patients with moderate or severe lobular inflammation compared with the mild lobular inflammation group (p = 0.008 and p = 0.0008, respectively). In circulation, IL-10 also significantly decreased in subjects with moderate or severe lobular inflammation compared with the mild lobular inflammation group (p = 0.005 and p < 0.0001, respectively). Conclusions: In liver biopsies and serum samples of morbidly obese patients, the protein levels of IL-10 progressively decrease as lobular inflammation increases, supporting the hypothesis that lobular inflammation develops because of the loss of the IL-10-mediated anti-inflammatory counterbalance. Full article
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<p>Histologic examination and grading of liver specimens. We stained 4 μm thick slices of liver tissue with hematoxylin–eosin, examining the areas between the hepatic lobules to score lobular inflammation according to the Brunt scoring system as follows: (<b>A</b>) mild lobular inflammation, &lt;2 inflammatory foci/20× fields; (<b>B</b>) moderate lobular inflammation, 2–4 inflammatory foci/20× fields; (<b>C</b>) severe lobular inflammation, &gt;4 inflammatory foci/20× fields. Red arrows indicate the presence of inflammatory foci. Scale bars show the 200 μm magnification at which we acquired the microphotographs. (<b>D</b>) After quantifying the number of inflammatory foci, we compared data by one-way ANOVA followed by Tukey’s multiple comparison test, considering a <span class="html-italic">p</span> &lt; 0.05 significant.</p>
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<p>Quantification of IL-10 levels in liver tissue and serum. (<b>A</b>) IL-10 mRNA expression in liver specimens from morbidly obese patients with several degrees of lobular inflammation. (<b>B</b>) IL-10 protein levels in hepatic tissue from patients with different grades of lobular inflammation. (<b>C</b>) IL-10 serum values in liver samples from morbidly obese patients with several degrees of lobular inflammation. We compared data by one-way ANOVA followed by Tukey’s multiple comparison test, considering a <span class="html-italic">p</span> &lt; 0.05 significant. IL-10, interleukin 10.</p>
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