Tag: SNR

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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A laboratory experiment to test particle acceleration in astrophysical environments. The study: “Laboratory evidence for proton energization by collisionless shock surfing” of W. Yao and J. Fuchs (École Polytechnique, Sorbonne Université) recently appeared on Nature Physics

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Energetic particles, called “cosmic rays”, constantly rain down on our planet. Thanks to several years of theoretical studies and observations, we know that these particles can be accelerated by shocks propagating in certain astrophysical environments. The classical example of such environment are the supernovae remnants, which are expanding clouds created by supernova explosions, which are often interacting with surrounding material.

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The role of the magnetic field during the evolution of supernova remnants i. The study: “Magneto-hydrodynamic simulations of young supernova remnants and their energy-conversion phase” of O. Petruk (IAPMM NASU) recently appeared on MNRAS

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Supernova explosions are sorted into two categories: The thermonuclear explosions triggered by white dwarfs in close binary systems (type Ia) and those triggered by the gravitational collapse of the core of massive stars (type Ib/c and II). Because of the paucity of known supernova remnants younger than 1000 years, astronomers developed several models describing the evolution of supernova remnants to

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A new diagnostic tool to identify metal-rich ejects in supernova remnants. The study: “Unveiling pure-metal ejecta X-ray emission in supernova remnants through their radiative recombination continuum” of E. Greco (UNIPA/INAF-OAPA/API) recently appeared on A&A

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Supernova remnants are nebulae created by supernova explosions. These expanding clouds are formed by the interstellar medium shocked and heated up by the expanding shock produced by the explosion, and the knots of material launched by the exploding star, called ejecta. These ejecta are located behind the expanding shock, traveling with lower velocity, and they are heated up by the reverse shock:

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The morphology of the oxygen-rich supernova remnant N132D. The study: “Three-dimensional Kinematic Reconstruction of the Optically Emitting, High-velocity, Oxygen-rich Ejecta of Supernova Remnant N132D” of C. J. Law (CfA) recently appeared on ApJ

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Supernove explosions are repeatedly observed in distant galaxies, which lie at such large distances that it is impossible for us to resolve the geometry of the ejected material and its interaction with the surrounding interstellar and circumstellar clouds. With the only exception of SN 1978A, in the Milky Way and in the nearby galaxies (namely the Magellanic Clouds), we did

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The mechanism responsible for the formation of magnetars? The study: “Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin” of P. Zhou (University of Amsterdam/Nanjing University) recently appeared on A&A

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At the end of their evolution, stars with a final mass larger than 8 solar masses (“final mass” because massive stars lose a large fraction of their mass as stellar winds during their evolution) explode as Core-Collapse Supernovae, e.g. triggered by the collapse of their nucleus. Two objects are produced by such explosions: the supernova remnant formed by the ejected

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