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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Barlow, Mj
University College London
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (8/8 displayed)
- 2021The impact of metallicity-dependent dust destruction on the dust-to-metals ratio in galaxies
- 2019The dust content of the Crab Nebula
- 2015A stubbornly large mass of cold dust in the ejecta of Supernova 1987Acitations
- 2015The dust and gas content of the Crab Nebulacitations
- 2012A Cool Dust Factory in the Crab Nebula: A Herschel Study of the Filamentscitations
- 2007Dust yields in clumpy supernova shells: SN 1987A revisitedcitations
- 2006The Spatial Distribution of Grains Around the Dual Chemistry Post-AGB Star Roberts 22
- 2003Three-dimensional photoionization modelling of the hydrogen-deficient knots in the planetary nebula Abell 30citations
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article
The dust and gas content of the Crab Nebula
Abstract
We have constructed mocassin photoionization plus dust radiative transfer models for the Crab Nebula core-collapse supernova (CCSN) remnant, using either smooth or clumped mass distributions, in order to determine the chemical composition and masses of the nebular gas and dust. We computed models for several different geometries suggested for the nebular matter distribution but found that the observed gas and dust spectra are relatively insensitive to these geometries, being determined mainly by the spectrum of the pulsar wind nebula which ionizes and heats the nebula. Smooth distribution models are ruled out since they require 16-49 M <SUB>☉ </SUB> of gas to fit the integrated optical nebular line fluxes, whereas our clumped models require 7.0 M <SUB>☉ </SUB> of gas. A global gas-phase C/O ratio of 1.65 by number is derived, along with a He/H number ratio of 1.85, neither of which can be matched by current CCSN yield predictions. A carbonaceous dust composition is favored by the observed gas-phase C/O ratio: amorphous carbon clumped model fits to the Crab’s Herschel and Spitzer infrared spectral energy distribution imply the presence of 0.18-0.27 M <SUB>☉ </SUB> of dust, corresponding to a gas to dust mass ratio of 26-39. Mixed dust chemistry models can also be accommodated, comprising 0.11-0.13 M <SUB>☉ </SUB> of amorphous carbon and 0.39-0.47 M <SUB>☉ </SUB> of silicates. Power-law grain size distributions with mass distributions that are weighted toward the largest grain radii are derived, favoring their longer-term survival when they eventually interact with the interstellar medium. The total mass of gas plus dust in the Crab Nebula is 7.2 ± 0.5 M <SUB>☉ </SUB>, consistent with a progenitor star mass of ̃9 M <SUB>☉ </SUB>.