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Universe
Special Issues
Studying Astrophysics with High-Energy Cosmic Particles
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Studying Astrophysics with High-Energy Cosmic Particles

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Cosmology".

Deadline for manuscript submissions: 30 June 2025 | Viewed by 3538

Special Issue Editors

Prof. Dr. Kinwah Wu

E-Mail Website
Guest Editor
Mullard Space Science Laboratory, University College London, London, UK
Interests: general relativistic radiative transfer; gravitational waves from black hole; magnetic star systems; accreting systems; AGN; X-ray binaries; cataclysmic variables; dynamics of galaxy clusters; large-scale magnetic fields; multi-messanger astrophysics; interdisciplinary research: astrophysics, biomedical, non-linear systems, population biology
Dr. Ellis R. Owen

E-Mail Website
Guest Editor
Astrophysical Big Bang Laboratory, RIKEN Cluster for Pioneering Research, Saitama, Japan
Interests: particle astrophysics; gamma-ray astronomy; cosmic-ray astronomy; star formation; galaxy evolution; galaxies in the early Universe

Special Issue Information

Dear Colleagues,

Astronomy has traditionally relied on observations with photons (electromagnetic waves). In recent years, multi-wavelength observations have expanded our knowledge of the Universe far beyond approaches focussed on one particular waveband, e.g. solely radio, optical or X-ray. The development of new particle detectors and modern data analysis techniques have now opened-up a new domain, advancing our capability to probe physical processes and study astrophysical systems in great detail using non-photonic particles. Energetic non-photonic particles are often, but not exclusively, produced in violent astrophysical environments. They directly carry information about certain high-energy processes, such as subatomic interactions, that are not always within reach of photonic observations. It is therefore timely for us to gather together as researchers in high-energy astrophysics to explore and discuss the various emerging opportunities in the non-photonic particle domain, and the prospects with complimentary studies of photons, to probe astrophysical processes in new ways. 

We therefore propose a special issue in Universe, “Studying Astrophysics with High-Energy Cosmic-particles”. Our focus is the discussion of different aspects of studies of high-energy astrophysics, such as theory, phenomenological modelling, observation, data analysis and instrumentation using non-photonic and photonic means as an integral part studying the Universe. The scope of this special issue is not restrictive, and we welcome new ideas and approaches in addition to research conducted in a more canonical manner with proven techniques. Our goal is to bring together researchers with an interest in cosmo-particle astrophysics, to promote discussion towards the aim of advancing our understanding of the Universe.

Prof. Dr. Kinwah Wu
Dr. Ellis R. Owen
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

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Published Papers (3 papers)

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Research

21 pages, 881 KiB  
Article
A Study on the Evolution of Emission Altitude with Frequency Among 104 Normal Pulsars
by Chaoxin Luo, Xin Xu, Changrong Du and Qijun Zhi
Universe 2025, 11(1), 17; https://doi.org/10.3390/universe11010017 - 12 Jan 2025
Viewed by 412
Abstract
Utilizing the databases from the European Pulsar Network (EPN), the Australia Telescope National Facility (ATNF), and published literature data, a geometric method was used to investigate the multifrequency emission altitude of 104 pulsars. We found that the evolution of emission altitudes with frequency [...] Read more.
Utilizing the databases from the European Pulsar Network (EPN), the Australia Telescope National Facility (ATNF), and published literature data, a geometric method was used to investigate the multifrequency emission altitude of 104 pulsars. We found that the evolution of emission altitudes with frequency for the majority of pulsars can be fitted using a power-law function with a normalization constant. In this work, it is found that the frequency evolution of pulsar emission altitude can be divided into three groups according to their different frequency dependencies of emission altitude (emission altitude decreases with frequency (Group A, η≤−0.1), keeps relatively constant with frequency (Group B, −0.1<η≤0.1), and increases with frequency (Group C, η≥0.1)), where η is the emission altitude variation rate. We also computed the emission altitudes across multiple frequency bands for these pulsars, thereby estimating the approximate range of the pulsar emission regions. We found that most pulsar emissions occur at altitudes of tens to hundreds of kilometers above the polar cap, with differences in emission altitude between the three groups becoming more clear at lower frequencies. Full article
(This article belongs to the Special Issue Studying Astrophysics with High-Energy Cosmic Particles)
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30 pages, 11511 KiB  
Article
Sources and Radiations of the Fermi Bubbles
by Vladimir A. Dogiel and Chung-Ming Ko
Universe 2024, 10(11), 424; https://doi.org/10.3390/universe10110424 - 12 Nov 2024
Viewed by 993
Abstract
Two enigmatic gamma-ray features in the galactic central region, known as Fermi Bubbles (FBs), were found from Fermi-LAT data. An energy release, (e.g., by tidal disruption events in the Galactic Center, GC), generates a cavity with a shock that expands into the local [...] Read more.
Two enigmatic gamma-ray features in the galactic central region, known as Fermi Bubbles (FBs), were found from Fermi-LAT data. An energy release, (e.g., by tidal disruption events in the Galactic Center, GC), generates a cavity with a shock that expands into the local ambient medium of the galactic halo. A decade or so ago, a phenomenological model of the FBs was suggested as a result of routine star disruptions by the supermassive black hole in the GC which might provide enough energy for large-scale structures, like the FBs. In 2020, analytical and numerical models of the FBs as a process of routine tidal disruption of stars near the GC were developed; these disruption events can provide enough cumulative energy to form and maintain large-scale structures like the FBs. The disruption events are expected to be 10−4∼10−5yr−1, providing an average power of energy release from the GC into the halo of E˙∼3×1041 erg s−1, which is needed to support the FBs. Analysis of the evolution of superbubbles in exponentially stratified disks concluded that the FB envelope would be destroyed by the Rayleigh–Taylor (RT) instabilities at late stages. The shell is composed of swept-up gas of the bubble, whose thickness is much thinner in comparison to the size of the envelope. We assume that hydrodynamic turbulence is excited in the FB envelope by the RT instability. In this case, the universal energy spectrum of turbulence may be developed in the inertial range of wavenumbers of fluctuations (the Kolmogorov–Obukhov spectrum). From our model we suppose the power of the FBs is transformed partly into the energy of hydrodynamic turbulence in the envelope. If so, hydrodynamic turbulence may generate MHD fluctuations, which accelerate cosmic rays there and generate gamma-ray and radio emission from the FBs. We hope that this model may interpret the observed nonthermal emission from the bubbles. Full article
(This article belongs to the Special Issue Studying Astrophysics with High-Energy Cosmic Particles)
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13 pages, 417 KiB  
Article
Low-Energy Cosmic Rays and Associated MeV Gamma-Ray Emissions in the Protoplanetary System
by Xulei Sun, Shuying Zheng, Zhaodong Shi, Bing Liu and Ruizhi Yang
Universe 2024, 10(8), 310; https://doi.org/10.3390/universe10080310 - 27 Jul 2024
Viewed by 1101
Abstract
Low-energy cosmic rays (LECRs) play a crucial role in the formation of planetary systems, and detecting and reconstructing the properties of early LECRs is essential for understanding the mechanisms of planetary system formation. Given that LECRs interact with the surrounding medium to produce [...] Read more.
Low-energy cosmic rays (LECRs) play a crucial role in the formation of planetary systems, and detecting and reconstructing the properties of early LECRs is essential for understanding the mechanisms of planetary system formation. Given that LECRs interact with the surrounding medium to produce nuclear de-excitation line emissions, which are gamma-ray emissions with energy mainly within 0.1–10 MeV and are unaffected by stellar wind modulation, these emissions can accurately reflect the properties of LECRs. This study introduces an innovative method for using gamma-ray emissions to infer LECR properties. We employed the Parker transport equation to simulate the propagation and spectral evolution of LECRs in a protoplanetary disk and calculated the characteristic gamma-ray emissions resulting from interactions between LECRs and disk material. These gamma-ray emissions encapsulate the spectral information of LECRs, providing a powerful tool to reconstruct the cosmic ray environment at that time. This method, supported by further theoretical developments and observations, will fundamentally enhance our understanding of the impact of CRs on the origin and evolution of planetary systems and address significant scientific questions regarding the cosmic ray environment at the origin of life. Full article
(This article belongs to the Special Issue Studying Astrophysics with High-Energy Cosmic Particles)
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