Supernova, such as iron, silicon and argon, are heated they emit lightĪt certain wavelengths. Previously known phenomenon - the Doppler effect - and a new technology
To create this visualization, scientists took advantage of both a The blue region is composed of gas surrounding the explosion that was heated when it was struck by the outgoing blast wave, as clearly seen in Chandra images. These unshocked debris were known to exist because they absorb background radio light, but they were only recently discovered in infrared emission with Spitzer. The red material interior to the yellow/orange ring has not yet encountered the inward moving shock and so has not yet been heated. Most of the material shown in this visualization, which begins with an artist's rendition of the neutron star previously detected by Chandra, is debris from the explosion that has been heated by a shock moving inwards. The red region is cold debris seen in the infrared.įinally, the blue reveals the outer blast wave, most prominently
#Cassiopeia a plus#
Optical, and infrared - including jets of silicon - plus outer debris Yellow region is a combination of argon and silicon seen in X-rays, This visualization, the green region is mostly iron observed in X-rays. Visualization of Cassiopeia A (Cas A), the result of an explosionĪpproximately 330 years ago, uses X-ray data from Chandra, infrared dataįrom Spitzer and pre-existing optical data from NOAO's 4-meter telescopeĪt Kitt Peak and the Michigan-Dartmouth-MIT 2.4-meter telescope. Reconstruction of a supernova remnant has been created. Results.For the first time, a multiwavelength three-dimensional (3-D) The simulations cover ≈2000 yr of expansion and include all physical processes relevant to describe the complexities in the SN evolution and the subsequent interaction of the stellar debris with the wind of the progenitor star.
We coupled a three-dimensional (3D) hydrodynamic model of a neutrino-driven SN explosion, which has the potential to reproduce the observed morphology of the Cassiopeia A (Cas A) remnant, with 3D (magneto)-hydrodynamic simulations of the remnant formation. Here we aim to explore to which extent the remnant keeps memory of the asymmetries that develop stochastically in the neutrino-heating layer due to hydrodynamic instabilities (e.g., convective overturn and the standing accretion shock instability SASI) during the first second after core bounce. The remnants of core-collapse supernovae (SNe) are probes of the physical processes associated with their parent SNe.Īims. Our results are useful to limit the power of the jet-structure formation process, and a weak jet mechanism with low temperature may be needed to explain it.Ĭontext. Thus, we conclude that the energy source that formed the jet structure was not the primary engine for the supernova explosion. Three-dimensional velocities of Fe- and Si/O-rich ejecta are obtained as $>$4,500 km s$^$ K at most). We investigate the kinematic and nucleosynthetic properties of the inverted ejecta layers in detail to understand its formation process using the data taken by the Chandra X-ray Observatory. X-ray observations of the supernova remnant Cassiopeia A have indicated that the Fe-rich ejecta lies outside the Si-rich materials in the southeastern region, which is consistent with the hypothesis on the inversion of the ejecta. The central strong activities in core-collapse supernovae expect to produce the overturning of the Fe- and Si/O-rich ejecta during the supernova explosion based on multi-dimensional simulations.