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Universe
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A Multiwavelength View of Supernovae
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A Multiwavelength View of Supernovae

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Solar and Stellar Physics".

Deadline for manuscript submissions: closed (31 May 2025) | Viewed by 7333

Special Issue Editor

Prof. Dr. Vikram Dwarkadas

E-Mail Website
Guest Editor
Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave., ERC 569, Chicago, IL 60637, USA
Interests: supernovae; supernova remnants; massive stars; stellar winds; wind-blown bubbles; interstellar medium; shock waves; particle acceleration; gamma-ray and X-ray emission; formation of the solar system

Special Issue Information

Dear Colleagues,

Supernovae (SNe) are one of the few objects that are visible over the entire wavelength range. They have been imaged at radio, infra-red, optical, ultraviolet, and X-ray wavelengths, with candidates at gamma-ray wavelengths. The increasing sensitivity of ground-based and space-based telescopes in the last half century has led to a vast increase in both the number of objects detected and our knowledge of these objects. More classes and subclasses of SNe appear to have arisen. Type Ia SNe have acquired a prominent role in cosmology, but their progenitors are still debated. The role of binary stars in SN formation and evolution is being investigated. Improvements in X-ray and radio telescopes have allowed for an investigation of various emission processes that was not possible a few decades ago. Our understanding of their radiation signatures at all wavelengths has significantly increased.

The goal of this Special Issue is to summarize recent multiwavelength results for supernovae. We aim to have papers describing results for individual SNe at various wavelengths, as well as review papers summarizing results at specific wavelengths. We also aim to include a description of theoretical processes, analysis of various emission signatures, and investigations of SN evolution and interactions with the circumstellar medium. Overall, we hope that this Special Issue will encapsulate the current state of SN research, summarize the observational results, and outline the physics necessary to understand the observations.

Prof. Dr. Vikram Dwarkadas
Guest Editor

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 250 words) can be sent to the Editorial Office for assessment.

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.

Keywords

  • supernovae
  • core collapse
  • type Ia
  • binaries
  • evolution
  • circumstellar interactions
  • emission processes
  • thermal and non-thermal emission

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Published Papers (5 papers)

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Research

Jump to: Review

13 pages, 419 KB  
Article
The Two Alternative Explosion Mechanisms of Core-Collapse Supernovae: 2024 Status Report
by Noam Soker
Universe 2024, 10(12), 458; https://doi.org/10.3390/universe10120458 - 16 Dec 2024
Cited by 18 | Viewed by 3142
Abstract
In comparing the two alternative explosion mechanisms of core-collapse supernovae (CCSNe), I examine recent three-dimensional (3D) hydrodynamical simulations of CCSNe in the frame of the delayed neutrino explosion mechanism (neutrino mechanism) and argue that these valuable simulations show that neutrino heating can supply [...] Read more.
In comparing the two alternative explosion mechanisms of core-collapse supernovae (CCSNe), I examine recent three-dimensional (3D) hydrodynamical simulations of CCSNe in the frame of the delayed neutrino explosion mechanism (neutrino mechanism) and argue that these valuable simulations show that neutrino heating can supply a non-negligible fraction of the explosion energy but not the observed energies, and hence cannot be the primary explosion mechanism. In addition to the energy crisis, the neutrino mechanism predicts many failed supernovae that are not observed. The most challenging issue of the neutrino mechanism is that it cannot account for point-symmetric morphologies of CCSN remnants, many of which were identified in 2024. These contradictions with observations imply that the neutrino mechanism cannot be the primary explosion mechanism of CCSNe. The alternative jittering jets explosion mechanism (JJEM) seems to be the primary explosion mechanism of CCSNe; neutrino heating boosts the energy of the jittering jets. Even if some simulations show explosions of stellar models (but usually with energies below that observed), it does not mean that the neutrino mechanism is the explosion mechanism. Jittering jets, which simulations do not include, can explode the core before the neutrino heating process does. Morphological signatures of jets in many CCSN remnants suggest that jittering jets are the primary driving mechanism, as expected by the JJEM. Full article
(This article belongs to the Special Issue A Multiwavelength View of Supernovae)
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Review

Jump to: Research

45 pages, 4592 KB  
Review
Multiwavelength View of Circumstellar Interaction in Supernovae
by Poonam Chandra
Universe 2025, 11(11), 363; https://doi.org/10.3390/universe11110363 - 3 Nov 2025
Viewed by 484
Abstract
The interaction of post-explosion supernova ejecta with the surrounding circumstellar medium creates emissions across the electromagnetic spectrum. Since the circumstellar medium is created by the mass lost from the progenitor star, it carries tell-tale signatures of the progenitor. Consequently, observations and modeling of [...] Read more.
The interaction of post-explosion supernova ejecta with the surrounding circumstellar medium creates emissions across the electromagnetic spectrum. Since the circumstellar medium is created by the mass lost from the progenitor star, it carries tell-tale signatures of the progenitor. Consequently, observations and modeling of radiation produced by the interaction in various types of supernovae have provided valuable insights into their progenitors. Detailed studies have shown that the interaction in supernovae begins and sustains over various timescales and lengthscales, with differing mass-loss rates in distinct sub-classes. This reveals diverse progenitor histories for these stellar explosions. This review paper summarizes various supernova subtypes, linking them to stellar death pathways, and presents an updated supernova classification diagram. We then present a multi-wavelength study of circumstellar interaction in different supernova classes. We also present unpublished X-ray as well as radio observations of a type IIn supernova, SN 2010jl, which allow us to extend its circumstellar interaction studies to about 7 years post-explosion. The new data indicates that the extreme mass-loss rate (∼0.1 M⊙ yr−1) in SN 2010jl, reported by Chandra et al. commenced within the last 300 years before the explosion. We summarize the current status of the field and argue that via detailed studies of the circumstellar interaction, a.k.a. “Time Machine” technique, one of the big mysteries of stellar evolution, i.e., mapping supernovae progenitors to their explosive outcomes can be solved. Full article
(This article belongs to the Special Issue A Multiwavelength View of Supernovae)
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35 pages, 2170 KB  
Review
Probing Supernova Diversity Through High-Cadence Optical Observations
by Kuntal Misra, Bhavya Ailawadhi, Raya Dastidar, Monalisa Dubey, Naveen Dukiya, Anjasha Gangopadhyay, Divyanshu Janghel, Kumar Pranshu and Mridweeka Singh
Universe 2025, 11(11), 361; https://doi.org/10.3390/universe11110361 - 31 Oct 2025
Viewed by 427
Abstract
Supernovae (SNe) are among the most energetic and transient events in the universe, offering crucial insights into stellar evolution, nucleosynthesis, and cosmic expansion. Optical observations have historically played a central role in the discovery, classification, and physical interpretation of SNe. In this review, [...] Read more.
Supernovae (SNe) are among the most energetic and transient events in the universe, offering crucial insights into stellar evolution, nucleosynthesis, and cosmic expansion. Optical observations have historically played a central role in the discovery, classification, and physical interpretation of SNe. In this review, we summarize recent progress in the optical study of SNe, with a focus on advancements in time-domain surveys and photometric and spectroscopic follow-up strategies. High-cadence optical monitoring is pivotal in capturing the diverse behaviors of SNe, from early-time emission to late-phase decline. Leveraging data from ARIES telescopes and national/international collaborations, we systematically investigate various SN types, including Type Iax, IIP/L, IIb, IIn/Ibn and Ib/c events. Our analysis includes light curve evolution and spectral diagnostics, providing insights into early emission signatures (e.g., shock breakout), progenitor systems, explosion mechanisms, and circumstellar medium (CSM) interactions. Through detailed case studies, we demonstrate the importance of both early-time and nebular-phase observations in constraining progenitor and CSM properties. This comprehensive approach underscores the importance of coordinated global efforts in time-domain astronomy to deepen our understanding of SN diversity. We conclude by discussing the challenges and opportunities for future optical studies in the era of wide-field observatories such as the Vera C. Rubin Observatory (hereafter Rubin), with an emphasis on detection strategies, automation, and rapid-response capabilities. Full article
(This article belongs to the Special Issue A Multiwavelength View of Supernovae)
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16 pages, 4520 KB  
Review
SN 2023ixf: The Closest Supernova of the Decade
by Wynn Jacobson-Galán
Universe 2025, 11(7), 231; https://doi.org/10.3390/universe11070231 - 15 Jul 2025
Cited by 3 | Viewed by 1276
Abstract
Supernova 2023ixf occurred on 18 May 2023 in the nearby galaxy Messier 101 (D≈6.85 Mpc), making it the closest supernova in the last decade. Following its discovery, astronomers around the world rushed to observe the explosion across the electromagnetic spectrum [...] Read more.
Supernova 2023ixf occurred on 18 May 2023 in the nearby galaxy Messier 101 (D≈6.85 Mpc), making it the closest supernova in the last decade. Following its discovery, astronomers around the world rushed to observe the explosion across the electromagnetic spectrum in order to uncover its early-time properties. Based on multi-wavelength analysis during its first year after explosion, Supernova 2023ixf is a type II supernova that interacted with dense, confined circumstellar material in its local environment—this material being lost from its red supergiant progenitor in the final years before explosion. In this article, we will review the findings of >80 studies already published on this incredible event and explore how the synthesis of SN 2023ixf observations across the electromagnetic spectrum can be used to constrain type II supernova explosion physics in addition to the uncertain mass loss histories of red supergiant stars in their final years. Full article
(This article belongs to the Special Issue A Multiwavelength View of Supernovae)
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32 pages, 1368 KB  
Review
On the X-Ray Emission from Supernovae, and Implications for the Mass-Loss Rates of Their Progenitor Stars
by Vikram V. Dwarkadas
Universe 2025, 11(5), 161; https://doi.org/10.3390/universe11050161 - 15 May 2025
Cited by 8 | Viewed by 1067
Abstract
We summarize the X-ray emission from young SNe. Having accumulated data on most observed X-ray SNe, we display the X-ray lightcurves of young SNe. We also explore the X-ray spectra of various SN types. The X-ray emission from Type Ib/c SNe is non-thermal. [...] Read more.
We summarize the X-ray emission from young SNe. Having accumulated data on most observed X-ray SNe, we display the X-ray lightcurves of young SNe. We also explore the X-ray spectra of various SN types. The X-ray emission from Type Ib/c SNe is non-thermal. It is also likely that the emission from Type IIP SNe with low mass-loss rates (around 10−7 M⊙ yr−1) is non-thermal. As the mass-loss rate increases, thermal emission begins to dominate. Type IIn SNe have the highest X-ray luminosities, and are clearly thermal. We do not find evidence of non-thermal emission from Type IIb SNe. The aggregated data are used to obtain approximate mass-loss rates of the progenitor stars of these SNe. Type IIP have progenitors with mass-loss rates <10−5M⊙ yr−1, while Type IIn progenitors generally have mass-loss rates >10−3M⊙ yr−1. However, we emphasize that the density of the ambient medium is the important parameter, and if it is due to a non-steady outflow solution, it cannot be translated into a mass-loss rate. Full article
(This article belongs to the Special Issue A Multiwavelength View of Supernovae)
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