Explosion

Summary

An explosion is a rapid expansion in volume of a given amount of matter associated with an extreme outward release of energy, usually with the generation of high temperatures and release of high-pressure gases. Explosions may also be generated by a slower expansion that would normally not be forceful, but is not allowed to expand, so that when whatever is containing the expansion is broken by the pressure that builds as the matter inside tries to expand, the matter expands forcefully. An example of this is a volcanic eruption created by the expansion of magma in a magma chamber as it rises to the surface. Supersonic explosions created by high explosives are known as detonations and travel through shock waves. Subsonic explosions are created by low explosives through a slower combustion process known as deflagration. Causes Explosions can occur in nature due to large influxes of energy. There are numerous ways explosions can occur naturally, such as volcanic or stellar pr

Official source

https://en.wikipedia.org/wiki/Explosion

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Beyrouth, déjà lourdement impactée par des crises économiques et sociales, subit une explosion en 2020, qui impacte le logement de 300 000 personnes. Les instances humanitaires deviennent alors vitales afin de subvenir aux besoins de la population. Le projet est au cœur de cette problématique du logement d’urgence et de sa temporalité. Il propose une réponse alternative au système de planification des camps humanitaires organisés à distance des centres urbains et construits à titre provisoire. A contrario, le projet investit une tour de haut standing, dégradée par l’explosion et abandonnée, en plein centre de Beyrouth dont l’organisation interne et externe permet la planification d’un camp d’urgence à la verticale. Cette tour se réinventera et se transformera progressivement en refuge pour 800 habitants. Elle dialoguera directement avec le contexte en se mettant au service de son quartier afin de lui offrir de nouveaux espaces publics. Elle se développera progressivement de l’intérieur grâce à ses habitants et aux premières interventions de professionnel.le.s, telle que la planification des réseaux, la sécurité structurelle ainsi que le confort interne. Ses espaces intérieurs et sa matérialité seront élaborés pour une dynamique communautaire et participative. Leurs degrés de privacité ainsi que leur potentiels évolutifs et modulaires offriront aux habitant.e.s une grande capacité d’appropriation. L’urgence est organisée temporairement mais est elle vécue de façon permanente.

2022

The Cas A-Like Snr 1E 0102.2-7219 In The Small Magellanic Cloud: An Asymmetric Bipolar Explosion

Frédéric Vogt

We have used the Wide Field Spectrograph on the 2.3 m telescope at Siding Spring Observatory to map the [O III] lambda 5007 dynamics of the young oxygen-rich supernova remnant 1E 0102.2-7219 in the Small Magellanic Cloud. From the resultant data cube, we have been able to reconstruct the full three-dimensional structure of the system of [O III] filaments. From this we are able to deduce that the ejecta trace an asymmetric bipolar structure. The redshifted gas contains fainter clumps but with higher velocities than the blueshifted gas. The major axis of the explosion is inclined at similar to 40 degrees to the line of sight. This structure shows that the supernova explosion has been influenced both by the rotation of the progenitor star and, presumably, by a global rotational instability following core collapse.

2010

Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected on January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. Aims. We aim to probe the possibility of very-high-energy (VHE; E >= 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions. Methods. We performed follow-up observations after this supernova (SN) explosion for five days, between January 27 and February 2 2014. We searched for gamma-ray signals in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of similar to 5.5 h of observations. Prospects for observing gamma rays of hadronic origin from SN 2014J in the near future are also being addressed. Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE proportional to E-Gamma, with a spectral index of Gamma = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 x 10(-12) and 4.1 x 10-(13) photons cm(-2) s(-1), respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first similar to 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10(-6) of the total available energy budget (similar to 10(51) erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.

Edp Sciences S A2017