Tag: SNR

Filaments in Cas A probe the processes occurred inside the progenitor during the explosion. The paper: “Filamentary ejecta network in Cassiopeia A reveals fingerprints of the supernova explosion mechanism” of S. Orlando (INAF-OAPA) appeared on A&A

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A new theoretical study shows that the filamentary structure observed in the supernova remnant Cassiopeia A (Cas A) is a direct consequence of the processes that occurred in the progenitor star immediately after core collapse.   Supernovae are among the most energetic explosive events in the Universe. Yet, despite their immense brightness, they convert only about 1% of their energy

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A green monster inside Cas A unveils the secrets of its violent phenomena. The study: “The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions” of I. de Looze (Ghent University) recently appeared on ApJL

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There are many lessons about the physics of supernova remnants and progenitor stars that the Cassiopeia A (Cas A) supernova remnant teaches us. For example, we have learned that both the supernova explosion and the mass-loss episodes that characterize the final evolutionary stages of the progenitor star can be highly asymmetric. We have come to understand that supernovae can play

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Non thermal emission and cosmic rays in the supernova remnants SN1006. The paper: “”Hadronic particle acceleration in the supernova remnant SN 1006 as traced by Fermi-LAT observations” of M. Lemoine-Goumard (University of Bordeaux) appeared on A&A

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Supernova remnants serve as unique laboratories to understand the complex processes occurring during a supernova explosion and to investigate the internal structure of massive stars just before their explosive demise. Additionally, the study of these remnants is driven by their crucial role in accelerating cosmic rays, which are particles with extremely high energies. In 1949, Enrico Fermi laid the groundwork for

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Chronology of a Supernova. The article: “Constraining the CSM structure and progenitor mass-loss history of interacting supernovae through 3D hydrodynamic modeling: The case of SN 2014C” by S. Orlando (INAF-OAPA), published in The Astrophysical Journal

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The properties and morphology of supernova remnants result from complex physical processes in the progenitor star, both in the stages preceding the explosion and during the event itself. This involves the rapid collapse of the core, occurring in seconds, up to the shock wave reaching the star’s surface. Additionally, the supernova’s evolution is shaped by interactions between the star’s expelled

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The acceleration of cosmic rays in supernova remnants depends on the interaction with the surrounding medium. The study: “Time evolution of the synchrotron X-ray emission in Kepler’s SNR: the effects of turbulence and shock velocity” of V. Sapienza (UNIPA/INAF-OAPA) appeared on ApJ

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The role of supernova remnants (expanding clouds produced by supernovae) in the acceleration of cosmic rays (high-energy particles present in various astrophysical environments) has been known since 1995. The discovery, made by astronomers from Kyoto University, was made possible by identifying the presence of non-thermal X-ray emission in the supernova remnant SN 1006. X-rays are a type of high-energy radiation

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Predictions on the observability of the neutron star in SN1987A. The study: “Investigating the Time Evolution of the Thermal Emission from the Putative Neutron Star in SN 1987A for 50+ Years” of A. Dohi (Kyushu University) appeared on ApJ

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SN1987A, located in the Large Magellanic Cloud, is an object of great importance for the study of supernovae and supernova remnants. In fact, it is the only supernova that has occurred recently and is close enough to allow us to obtain detailed observations across the entire electromagnetic spectrum. SN1987A was a core-collapse supernova, resulting from the collapse of the core

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The magnetic field in SN1987A revealed from radio observations. The study: “Polarized radio emission unveils the structure of the pre-supernova circumstellar magnetic field and the radio emission in SN1987A” of O. Petruk (INAF-OAPA) appeared on A&A

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Without any doubts, the supernova remnants SN1987A is the one that taught us more about this class of objects and supernova exposions. Produced by a supernova exploded in the Large Magellanic Cloud on February 23rd 1987, this is the only case in which we have observations of the progenitor, of the supernova explosion, and in which we follow the development

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The properties of the reverse shock in Cas A reveal properties of the progenitor. The paper: “Evidence for past interaction with an asymmetric circumstellar shell in the young SNR Cassiopeia A” of S. Orlando (INAF – OAPA) recently appeared on A&A

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Supernova remnants (expanding clouds produced by the explosion of massive stars) are fascinating objects. Their study, in fact, can unveil the physical processes working during supernova explosions and even the properties of the stellar progenitors. To these aims, of particular importance is the analysis of the physical and chemical properties of the ejecta (which are the fragments of the dying

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Confirmed the existence of a neutron star in the center of SN1987A. The paper: “Additional Evidence for a Pulsar Wind Nebula in the Heart of SN 1987A from Multiepoch X-Ray Data and MHD Modeling” of E. Greco (University of Amsterdam; INAF-OAPA) recently appeared on Apj

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SN1987A, the supernova exploded in the Large Magellanic Cloud (at about 170000 light years of distance) on February 23rd 1987, was an iconic event for the study of supernovae and supernova remnants. In fact, it is the only case where it was possible to observe (with telescopes) the explosion and to follow with periodic observations the evolution of the supernova

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Supernova explosions produced by LBV stars. The study: “Modeling the remnants of core-collapse supernovae from luminous blue variable stars” of S. Ustamujic (INAF-OAPA) recently appeared on Astronomy & Astrophysics

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LBV (Luminous Blue Variable) stars are massive and unstable stars characterized by large mass-lost due to intense stellar winds and aperiodic bursts. Due to their instability, LBV stars are also variable, with quasi-periodic oscillations of their luminosity of the order of 0.5-2 magnitudes. Typical examples of this class of stars are: the supergiant S Doradus in the Large Magellanic Clouds,

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