| People | Locations | Statistics |
|---|---|---|
| Naji, M. |
| |
| Motta, Antonella |
| |
| Aletan, Dirar |
| |
| Mohamed, Tarek |
| |
| Ertürk, Emre |
| |
| Taccardi, Nicola |
| |
| Kononenko, Denys |
| |
| Petrov, R. H. | Madrid |
|
| Alshaaer, Mazen | Brussels |
|
| Bih, L. |
| |
| Casati, R. |
| |
| Muller, Hermance |
| |
| Kočí, Jan | Prague |
|
| Šuljagić, Marija |
| |
| Kalteremidou, Kalliopi-Artemi | Brussels |
|
| Azam, Siraj |
| |
| Ospanova, Alyiya |
| |
| Blanpain, Bart |
| |
| Ali, M. A. |
| |
| Popa, V. |
| |
| Rančić, M. |
| |
| Ollier, Nadège |
| |
| Azevedo, Nuno Monteiro |
| |
| Landes, Michael |
| |
| Rignanese, Gian-Marco |
|
Dwek, Eli
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (10/10 displayed)
- 2021The infrared echo of SN2010jl and its implications for shock breakout characteristics
- 2016Dust destruction by the reverse shock in the Cassiopeia A supernova remnantcitations
- 2015The Evolution of Dust Mass in the Ejecta of SN1987Acitations
- 2013The Importance of Physical Models for Deriving Dust Masses and Grain Size Distributions in Supernova Ejecta. I. Radiatively Heated Dust in the Crab Nebulacitations
- 2012Properties and Spatial Distribution of Dust Emission in the Crab Nebulacitations
- 2010The Chemistry of Population III Supernova Ejecta. II. The Nucleation of Molecular Clusters as a Diagnostic for Dust in the Early Universecitations
- 2004The Detection of Cold Dust in Cassiopeia A: Evidence for the Formation of Metallic Needles in the Ejectacitations
- 2004Interstellar Dust Models Consistent with Extinction, Emission, and Abundance Constraintscitations
- 2003Interstellar Dust Models Consistent with Extinction, Emission, and Abundance Constraints
- 2002The Zodiacal Emission Spectrum as Determined by COBE and Its Implicationscitations
Places of action
| Organizations | Location | People |
|---|
article
The Chemistry of Population III Supernova Ejecta. II. The Nucleation of Molecular Clusters as a Diagnostic for Dust in the Early Universe
Abstract
We study the formation of molecular precursors to dust in the ejecta of Population III supernovae (Pop. III SNe) using a chemical kinetic approach to follow the evolution of small dust cluster abundances from day 100 to day 1000 after explosion. Our work focuses on zero-metallicity 20 M <SUB>sun</SUB> and 170 M <SUB>sun</SUB> progenitors, and we consider fully macroscopically mixed and unmixed ejecta. The dust precursors comprise molecular chains, rings, and small clusters of chemical composition relevant to the initial elemental composition of the ejecta under study. The nucleation stage for small silica, metal oxides and sulfides, pure metal, and carbon clusters is described with a new chemical reaction network highly relevant to the kinetic description of dust formation in hot circumstellar environments. We consider the effect of the pressure dependence of critical nucleation rates and test the impact of microscopically mixed He<SUP>+</SUP> on carbon dust formation. Two cases of metal depletion on silica clusters (full and no depletion) are considered to derive upper limits to the amounts of dust produced in SN ejecta at 1000 days, while the chemical composition of clusters gives a prescription for the type of dust formed in Pop. III SNe. We show that the cluster mass produced in the fully mixed ejecta of a 170 M <SUB>sun</SUB> progenitor is ~ 25 M <SUB>sun</SUB> whereas its 20 M <SUB>sun</SUB> counterpart forms ~ 0.16 M <SUB>sun</SUB> of clusters. The unmixed ejecta of a 170 M <SUB>sun</SUB> progenitor SN synthesize ~5.6 M <SUB>sun</SUB> of small clusters, while its 20 M <SUB>sun</SUB> counterpart produces ~0.103 M <SUB>sun</SUB>. Our results point to smaller amounts of dust formed in the ejecta of Pop. III SNe by a factor of ~ 5 compared to values derived by previous studies, and to different dust chemical compositions. Such deviations result from some erroneous assumptions made, the inappropriate use of classical nucleation theory to model dust formation, and the omission of the synthesis of molecules in SN ejecta. We also find that the unmixed ejecta of massive Pop. III SNe chiefly form silica and/or silicates, and pure silicon grains whereas their lower mass counterparts form a dust mixture dominated by silica and/or silicates, pure silicon, and iron sulfides. Amorphous carbon can only condense via the nucleation of carbon chains and rings characteristic of the synthesis of fullerenes when the ejecta carbon-rich zone is deprived of He<SUP>+</SUP>. The first dust enrichment to the primordial gas in the early universe from Pop. III massive SN comprises primarily pure silicon, silica, and silicates. If carbon dust is present at redshift z > 6, alternative dust sources must be considered.