Journal Description
Astronomy
                    Astronomy 
                    is an international, peer-reviewed, open access journal on observational astronomy, theoretical astronomy and other specific subfields published quarterly online by MDPI.
                - Open Access— free for readers, with article processing charges (APC) paid by authors or their institutions.
- High Visibility: indexed within Scopus and other databases.
- Rapid Publication: manuscripts are peer-reviewed and a first decision is provided to authors approximately 27.6 days after submission; acceptance to publication is undertaken in 7.6 days (median values for papers published in this journal in the first half of 2025).
- Recognition of Reviewers: APC discount vouchers, optional signed peer review, and reviewer names published annually in the journal.
- Astronomy is a companion journal of Universe and Aerospace.
Latest Articles
        
        
                    
    
        
    
    A Census of Chemically Peculiar Stars in Stellar Associations
                        
    
                
            
                
        Astronomy 2025, 4(4), 20; https://doi.org/10.3390/astronomy4040020 - 22 Oct 2025
    
                            
    
                    
        
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            The pre-main-sequence evolution of the chemically peculiar (CP) stars on the upper main sequence is still a vast mystery and not well understood. Our analysis of young associations and open clusters aims to find (very) young CP stars to try to put a
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            The pre-main-sequence evolution of the chemically peculiar (CP) stars on the upper main sequence is still a vast mystery and not well understood. Our analysis of young associations and open clusters aims to find (very) young CP stars to try to put a lower boundary on the age of such objects. Using three catalogues of open clusters and associations, we determined membership probabilities using HDBSCAN. The hot stars from this selection were submitted to synthetic 
    Open AccessReview
    
    Time Markers for SETI in Binary Systems: History and Prospects
                        
            by
                    Jacob Haqq-Misra        
    
                
        
        Astronomy 2025, 4(4), 19; https://doi.org/10.3390/astronomy4040019 - 22 Oct 2025
    
                            
    
                    
        
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            Contemporary surveys in the search for extraterrestrial intelligence (SETI) typically make one-off “spot scans” across the sky to search planetary systems for narrow-band radio signals that would indicate the presence of intelligent life. Spot scans may span a duration of seconds to minutes
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            Contemporary surveys in the search for extraterrestrial intelligence (SETI) typically make one-off “spot scans” across the sky to search planetary systems for narrow-band radio signals that would indicate the presence of intelligent life. Spot scans may span a duration of seconds to minutes in order to observe a large number of targets with limited resources, but such a strategy does not necessarily consider the timing of exactly when to listen for extraterrestrial signals. Several ideas for possible time markers were suggested in the first few decades of SETI, such as the use of recurrent supernovae, gamma ray bursts, or pulsars as a way of establishing directionality and attracting attention toward an extraterrestrial beacon. Civilizations in binary systems might even choose the points of periastron and apastron in its host system to send transmissions to other single-star civilizations. However, all of these timing considerations were developed prior to the age of exoplanets, which enables a more detailed assessment of targets suitable for SETI. This paper suggests SETI strategies for circumbinary and circumprimary planets based upon the timing of orbital events in such systems. Events such as orbital extremes could represent a logical time marker for extraterrestrial civilizations to transmit, if they desire to be detected. Likewise, a transiting binary pair with inhabited planets around each star could yield maximum detectability of leakage radiation when both stars eclipse within our field of view. As planets in binary systems continue to be discovered, limited-duration SETI surveys should selectively target such systems based upon the occurrence of reasonable time markers.
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    Open AccessArticle
    
    On the Possible Nature of White Holes
                        
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                    Mikhail Pekker and Mikhail N. Shneider        
    
                
        
        Astronomy 2025, 4(4), 18; https://doi.org/10.3390/astronomy4040018 - 10 Oct 2025
    
                            
    
                    
        
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            This paper considers non-singular black holes. It discusses the observation of particles falling onto ordinary and non-singular black holes from the perspective of a distant observer. It is demonstrated that, during a stage in the evolution of non-singular black holes, powerful energy fluxes
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            This paper considers non-singular black holes. It discusses the observation of particles falling onto ordinary and non-singular black holes from the perspective of a distant observer. It is demonstrated that, during a stage in the evolution of non-singular black holes, powerful energy fluxes can be emitted. Distant observers may interpret these fluxes as white holes.
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Open AccessArticle
    
    Cosmic-Ray Boosted Diffuse Supernova Neutrinos
                        
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                    Alexander Sandrock        
    
                
        
        Astronomy 2025, 4(3), 17; https://doi.org/10.3390/astronomy4030017 - 12 Sep 2025
    
                            
    
                    
        
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            The subject of boosted fluxes of dark matter or cosmic relic neutrinos via scattering on cosmic rays has received considerable attention recently. This article investigates the boosted neutrino flux from the scattering of cosmic rays and the so-far undetected diffuse supernova neutrino background,
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            The subject of boosted fluxes of dark matter or cosmic relic neutrinos via scattering on cosmic rays has received considerable attention recently. This article investigates the boosted neutrino flux from the scattering of cosmic rays and the so-far undetected diffuse supernova neutrino background, taking into account both galactic and extragalactic cosmic rays. The calculated flux is many orders of magnitude smaller than either the galactic diffuse neutrino emission, the extragalactic astrophysical flux measured by IceCube, or the cosmogenic neutrino flux expected at the highest energies.
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Open AccessArticle
    
    Extending the Quantum Memory Matrix to Dark Energy: Residual Vacuum Imprint and Slow-Roll Entropy Fields
                        
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                    Florian Neukart, Eike Marx and Valerii Vinokur        
    
                
        
        Astronomy 2025, 4(3), 16; https://doi.org/10.3390/astronomy4030016 - 10 Sep 2025
    
                            
    
                    
        
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            We extend the Quantum Memory Matrix (QMM) framework—previously shown to unify gauge interactions and reproduce cold dark matter phenomenology—to account for the observed late-time cosmic acceleration. In QMM, each Planck-scale cell carries a finite-dimensional Hilbert space of quantum imprints. We show that (1)
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            We extend the Quantum Memory Matrix (QMM) framework—previously shown to unify gauge interactions and reproduce cold dark matter phenomenology—to account for the observed late-time cosmic acceleration. In QMM, each Planck-scale cell carries a finite-dimensional Hilbert space of quantum imprints. We show that (1) once local unitary evolution saturates the available micro-states, a uniform residual “vacuum-imprint energy” remains; its stress–energy tensor is of pure cosmological-constant form, with magnitude suppressed by the cell capacity, naturally yielding 
    
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Open AccessArticle
    
    The Status of the Astrophysical Parameters of Upper Main Sequence Stars
                        
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                    Lukas Kueß and Ernst Paunzen        
    
                
        
        Astronomy 2025, 4(3), 15; https://doi.org/10.3390/astronomy4030015 - 22 Aug 2025
    
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            Calibrating the ages, masses, and radii of stars on the upper main sequence depends heavily on accurate measurements of the effective temperature (
        
            Calibrating the ages, masses, and radii of stars on the upper main sequence depends heavily on accurate measurements of the effective temperature (
    
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Open AccessArticle
    
    Gravity Wave Phase Shift in a Cold Quark Star with a Nonconvex QCD BZT Shock Wave Van Der Waals Equation of State
                        
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                    Keith Andrew, Eric V. Steinfelds and Kristopher A. Andrew        
    
                
        
        Astronomy 2025, 4(3), 14; https://doi.org/10.3390/astronomy4030014 - 22 Aug 2025
    
                            
    
                    
        
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            We investigate BZT shocks and the QCD phase transition in the dense core of a cold quark star in beta equilibrium subject to the multicomponent van der Waals (MvdW) equation of state (EoS) as a model of internal structure. When this system is
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            We investigate BZT shocks and the QCD phase transition in the dense core of a cold quark star in beta equilibrium subject to the multicomponent van der Waals (MvdW) equation of state (EoS) as a model of internal structure. When this system is expressed in terms of multiple components, it can be used to explore the impact of a phase transition from a hadronic state to a quark plasma state with a complex clustering structure. The clustering can take the form of colored diquarks or triquarks and bound colorless meson, baryon, or hyperon states at the phase transition boundary. The resulting multicomponent EoS system is nonconvex, which can give rise to Bethe–Zel’dovich–Thompson (BZT) phase-changing shock waves. Using the BZT shock wave condition, we find constraints on the quark density and examine how this changes the tidal deformability of the compact core. These results are then combined with the TOV equations to find the resulting mass and radius relationship. These states are compared to recent astrophysical high-mass neutron star systems, which may provide evidence for a core that has undergone a quark gluon phase transition such as PSR 0943+10 or GW 190814.
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Open AccessArticle
    
    The Use of Conditional Variational Autoencoders in Generating Stellar Spectra
                        
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                    Marwan Gebran and Ian Bentley        
    
                
        
        Astronomy 2025, 4(3), 13; https://doi.org/10.3390/astronomy4030013 - 22 Aug 2025
    
                            
    
                    
        
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            We present a conditional variational autoencoder (CVAE) that generates stellar spectra covering 4000 ≤ 
        
            We present a conditional variational autoencoder (CVAE) that generates stellar spectra covering 4000 ≤ 
    
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Open AccessArticle
    
    Nonlinearity in Turbulent Diffusion as a Possible Cause of Stellar Flares
                        
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                    Elena Popova        
    
                
        
        Astronomy 2025, 4(3), 12; https://doi.org/10.3390/astronomy4030012 - 7 Jul 2025
    
                            
    
                    
        
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            Extremely powerful flares releasing energy well above 
        
            Extremely powerful flares releasing energy well above 
    
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Open AccessReview
    
    A Library of 77 Multibody Solar and Extrasolar Subsystems—A Review of Their Dynamical Properties, Global Mean-Motion Resonances, and the Landau-Damped Mean Tidal Fields
                        
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                    Dimitris M. Christodoulou, Silas G. T. Laycock and Demosthenes Kazanas        
    
                
        
        Astronomy 2025, 4(3), 11; https://doi.org/10.3390/astronomy4030011 - 23 Jun 2025
    
                            
    
                    
        
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            We revisit 77 relaxed (extra)solar multibody (sub)systems containing 2–9 bodies orbiting about gravitationally dominant central bodies. The listings are complete down to (sub)systems with 5 orbiting bodies and additionally contain 33 smaller systems with 2–4 orbiting bodies. Most of the multiplanet systems (68)
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            We revisit 77 relaxed (extra)solar multibody (sub)systems containing 2–9 bodies orbiting about gravitationally dominant central bodies. The listings are complete down to (sub)systems with 5 orbiting bodies and additionally contain 33 smaller systems with 2–4 orbiting bodies. Most of the multiplanet systems (68) have been observed outside of our solar system, and very few of them (5) exhibit classical Laplace resonances (LRs). The remaining 9 subsystems have been found in our solar system; they include 7 well-known satellite groups in addition to the four gaseous giant planets and the four terrestrial planets, and they exhibit only one classical Laplace resonant chain, the famous Galilean LR. The orbiting bodies (planets, dwarfs, or satellites) appear to be locked in/near global mean-motion resonances (MMRs), as these are determined in reference to the orbital period of the most massive (most inert) body in each (sub)system. We present a library of these 77 multibody subsystems for future use and reference. The library listings of dynamical properties also include regular spacings of the orbital semimajor axes. Regularities in the spatial configurations of the bodies were determined from patterns that had existed in the mean tidal field that drove multibody migrations toward MMRs, well before the tidal field was erased by the process of `gravitational Landau damping’ which concluded its work when all major bodies had finally settled in/near the global MMRs presently observed. Finally, detailed comparisons of results help us discern the longest commonly-occurring MMR chains, distinguish the most important groups of triple MMRs, and identify a new criterion for the absence of librations in triple MMRs.
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Open AccessArticle
    
    Core–Corona Decomposition of Very Compact (Neutron) Stars: Accounting for Current Data of XTE J1814-338
                        
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                    Rico Zöllner and Burkhard Kämpfer        
    
                
        
        Astronomy 2025, 4(2), 10; https://doi.org/10.3390/astronomy4020010 - 9 Jun 2025
    
                            
    
                    
        
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            A core–corona decomposition of compact (neutron) star models was compared with the current mass–radius data of the outlier XTE J1814-338. The corona (which may also be dubbed the envelope, halo or outer crust) is assumed to be of Standard Model matter, with an
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            A core–corona decomposition of compact (neutron) star models was compared with the current mass–radius data of the outlier XTE J1814-338. The corona (which may also be dubbed the envelope, halo or outer crust) is assumed to be of Standard Model matter, with an equation of state that is supposed to be faithfully known and accommodates nearly all other neutron star data. The core, solely parameterized by its mass, radius and transition pressure, presents a challenge regarding its composition. We derived a range of core parameters needed to describe the current data of XTE J1814-338.
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Open AccessArticle
    
    Analytic Investigation of the Imprints of Dark Energy and Charge on the Kerr–Newmann–De Sitter Black-Hole Photon Ring
                        
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                    James Mugambi, Eunice Omwoyo and Dismas Wamalwa        
    
                
        
        Astronomy 2025, 4(2), 9; https://doi.org/10.3390/astronomy4020009 - 21 May 2025
    
                            
    
                    
        
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            In 2019, the Event Horizon Telescope (EHT) released the first image of a black hole, sparking huge interest in the study of black-hole images. We present analytical solutions to the null geodesic equations for Kerr–Newman–de Sitter black holes derived using Jacobi elliptic functions.
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            In 2019, the Event Horizon Telescope (EHT) released the first image of a black hole, sparking huge interest in the study of black-hole images. We present analytical solutions to the null geodesic equations for Kerr–Newman–de Sitter black holes derived using Jacobi elliptic functions. Using these solutions, we have performed an analytic ray-tracing simulation to model direct images, lensing rings, and photon rings, considering standard observers and zero angular momentum observers (ZAMOs). Additionally, we have derived analytic expressions for the critical parameters governing the structure of the photon ring and analyzed them in detail. From the foregoing, an increase in charge leads to a decrease in both time delay and Lyapunov exponent, while the change in azimuthal angle is insignificant. These findings improve our understanding of the effects of charge on black-hole photon rings and provide a foundation for future studies.
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Open AccessArticle
    
    At the Edge of Uncertainty: Decoding the Cosmological Constant Value with the Bose–Einstein Distribution
                        
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                    Ahmed Farag Ali and Nader Inan        
    
                
        
        Astronomy 2025, 4(2), 8; https://doi.org/10.3390/astronomy4020008 - 13 May 2025
    
                            
    
                    
        
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            We propose that the observed value of the cosmological constant may be explained by a fundamental uncertainty in the spacetime metric, which arises when combining the principle that mass and energy curve spacetime with the quantum uncertainty associated with particle localization. Since the
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            We propose that the observed value of the cosmological constant may be explained by a fundamental uncertainty in the spacetime metric, which arises when combining the principle that mass and energy curve spacetime with the quantum uncertainty associated with particle localization. Since the position of a quantum particle cannot be sharply defined, the gravitational influence of such particles leads to intrinsic ambiguity in the formation of spacetime geometry. Recent experimental studies suggest that gravitational effects persist down to length scales of approximately 
    
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Open AccessArticle
    
    Hilbert Bundles and Holographic Space–Time Models
                        
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                    Tom Banks        
    
                
        
        Astronomy 2025, 4(2), 7; https://doi.org/10.3390/astronomy4020007 - 22 Apr 2025
    
                            
    
                    
        
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            We reformulate holographic space–time models in terms of Hilbert bundles over the space of the time-like geodesics in a Lorentzian manifold. This reformulation resolves the issue of the action of non-compact isometry groups on finite-dimensional Hilbert spaces. Following Jacobson, I view the background
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            We reformulate holographic space–time models in terms of Hilbert bundles over the space of the time-like geodesics in a Lorentzian manifold. This reformulation resolves the issue of the action of non-compact isometry groups on finite-dimensional Hilbert spaces. Following Jacobson, I view the background geometry as a hydrodynamic flow, whose connection to an underlying quantum system follows from the Bekenstein–Hawking relation between area and entropy, generalized to arbitrary causal diamonds. The time-like geodesics are equivalent to the nested sequences of causal diamonds, and the area of the holoscreen (The holoscreen is the maximal 
    
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Open AccessArticle
    
    Distance to M87 as the Mode of the Modulus Distribution
                        
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                    Mariusz Tarnopolski        
    
                
        
        Astronomy 2025, 4(2), 6; https://doi.org/10.3390/astronomy4020006 - 2 Apr 2025
    
                            
    
                    
        
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            de Grijs and Bono (ApJS 2020, 246, 3) compiled a list of distances to M87 from the literature published in the last 100 years. They reported the arithmetic mean of the three most stable tracers (Cepheids, tip of the red giant branch, and
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            de Grijs and Bono (ApJS 2020, 246, 3) compiled a list of distances to M87 from the literature published in the last 100 years. They reported the arithmetic mean of the three most stable tracers (Cepheids, tip of the red giant branch, and surface brightness fluctuations). The arithmetic mean is one of the measures of central tendency of a distribution; others are the median and mode. The three do not align for asymmetric distributions, which is the case for the distance moduli 
    
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Open AccessReview
    
    Solar Particle Acceleration
                        
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                    Donald V. Reames        
    
                
        
        Astronomy 2025, 4(1), 5; https://doi.org/10.3390/astronomy4010005 - 18 Mar 2025
    
                            
    
                    
        
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            High-energy particles may be accelerated widely in stellar coronae; probably by the same processes we find in the Sun. Here, we have learned of two physical mechanisms that dominate the acceleration of solar energetic particles (SEPs). The highest energies and intensities are produced
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            High-energy particles may be accelerated widely in stellar coronae; probably by the same processes we find in the Sun. Here, we have learned of two physical mechanisms that dominate the acceleration of solar energetic particles (SEPs). The highest energies and intensities are produced in “gradual” events where shock waves are driven from the Sun by fast and wide coronal mass ejections (CMEs). Smaller, but more numerous “impulsive” events with unusual particle compositions are produced during magnetic reconnection in solar jets and flares. Jets provide open magnetic field lines where SEPs can escape. Closed magnetic loops contain this energy to produce bright, hot flares; perhaps even contributing to heating the low corona in profuse nanoflares. Streaming protons amplify Alfvén waves upstream of the shocks. These waves scatter and trap SEPs and, in large events, modify the element abundances and flatten the low-energy spectra upstream. Shocks also re-accelerate the residual ions from earlier impulsive events, when available, that characteristically dominate the energetic heavy-ion abundances. The large CME-driven shock waves develop an extremely wide longitudinal span, filling much of the inner heliosphere with energetic particles.
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Open AccessArticle
    
    Deciphering the Electron Spectral Hardening in AMS-02
                        
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                    Carmelo Evoli        
    
                
        
        Astronomy 2025, 4(1), 4; https://doi.org/10.3390/astronomy4010004 - 28 Feb 2025
    
                            
    
                    
        
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            We analyze the electron cosmic-ray spectrum from AMS-02, focusing on the spectral hardening around 42 GeV. Our findings confirm that this feature is intrinsic to the primary electron component rather than a byproduct of contamination from primary positron sources. Even under conservative assumptions,
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            We analyze the electron cosmic-ray spectrum from AMS-02, focusing on the spectral hardening around 42 GeV. Our findings confirm that this feature is intrinsic to the primary electron component rather than a byproduct of contamination from primary positron sources. Even under conservative assumptions, its significance remains at about 
    
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Open AccessArticle
    
    Line Ratio in the C-like Ion Spectrum O III: Testing Atomic Theory Predictions Through the Observation of Galaxies
                        
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                    Julius Richard Dreisbach, Dominik J. Bomans and Elmar Träbert        
    
                
        
        Astronomy 2025, 4(1), 3; https://doi.org/10.3390/astronomy4010003 - 10 Feb 2025
    
                            
    
                    
        
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            The progress made in atomic structure computations has indicated that certain line ratios of forbidden transitions may be slightly different from earlier assumptions. In order to check this theory, we evaluate previous observations of dwarf galaxies by the UVES spectrograph at the VLT
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            The progress made in atomic structure computations has indicated that certain line ratios of forbidden transitions may be slightly different from earlier assumptions. In order to check this theory, we evaluate previous observations of dwarf galaxies by the UVES spectrograph at the VLT telescope on ESO Paranal for the line ratios of branched decays in C-like oxygen ions [O III] that are insensitive to the local environment. Our findings show that the observed line ratio for [O III] (
    
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Open AccessArticle
    
    Tracing the Evolution of the Emission Properties of Carbon-Rich AGB, Post-AGB, and PN Sources
                        
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                    Silvia Tosi and Ester Marini        
    
                
        
        Astronomy 2025, 4(1), 2; https://doi.org/10.3390/astronomy4010002 - 20 Jan 2025
    
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            Understanding the transition from the Asymptotic Giant Branch (AGB) to the Planetary Nebula (PN) phase is crucial for advancing our knowledge of galaxy evolution and the chemical enrichment of the universe. In this manuscript, we analyze 137 carbon-rich, evolved low- and intermediate-mass stars
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            Understanding the transition from the Asymptotic Giant Branch (AGB) to the Planetary Nebula (PN) phase is crucial for advancing our knowledge of galaxy evolution and the chemical enrichment of the universe. In this manuscript, we analyze 137 carbon-rich, evolved low- and intermediate-mass stars (LIMSs) from both the Magellanic Clouds (MCs) and the Milky Way (MW). We focus on AGB, post-AGB, and PN sources, tracing the evolution of their emission through spectral energy distribution (SED) modeling. Consistent with previous studies, we observe that more evolved LIMSs exhibit cooler dust temperatures and lower optical depths. Amorphous carbon (amC) is the dominant dust species in all the evolutionary stages examined in this work, while silicon carbide (SiC) accounts for 5–30% of the total dust content. Additionally, we analyze color–color diagrams (CCDs) in the infrared using data from IRAC, WISE, and 2MASS, uncovering significant evolutionary trends in LIMS emission. AGB stars evolve from bluer to redder colors as they produce increasing amounts of dust. Post-AGB and PN sources are clearly differentiated from AGB stars, reflecting shifts in both effective stellar and dust temperatures as the stars transition through these evolutionary phases.
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    An Investigation of the Entropy Associated with a Collapsing Molecular Cloud
                        
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                    Gemechu Muleta Kumssa        
    
                
        
        Astronomy 2025, 4(1), 1; https://doi.org/10.3390/astronomy4010001 - 17 Jan 2025
    
                            
    
                    
        
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            The investigation of entropy variation during the star formation process within collapsing molecular clouds represents a significant field of inquiry in astrophysics. As the cloud contracts, the presence of gaseous components contributes to an increase in entropy; however, the degree of this entropy
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            The investigation of entropy variation during the star formation process within collapsing molecular clouds represents a significant field of inquiry in astrophysics. As the cloud contracts, the presence of gaseous components contributes to an increase in entropy; however, the degree of this entropy change is contingent upon the spatial constraints imposed on the gases. In this research endeavor, I perform a comprehensive analysis of entropy dynamics on a microcosmic level within the contracting cloud, adhering to the tenets of the second law of thermodynamics. The initial focus centers on a turbulent cloud consisting of N particles, each with a mass of M, which succumbs to gravitational forces. It becomes evident that for the collapse to transpire, the gravitational energy must surpass the opposing pressure forces, resulting in the swift movement of particles throughout the cloud and ultimately facilitating a shift in entropy.
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