| People | Locations | Statistics |
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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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Matsuura, Mikako
Cardiff University
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (9/9 displayed)
- 2023Quantifying the dust in SN 2012aw and iPTF14hls with ORBYTScitations
- 2023Evidence for late-time dust formation in the ejecta of supernova SN 1995N from emission-line asymmetriescitations
- 2021JWST Survey of the Prototypical Core-collapse Supernova Remnant Cassiopeia A
- 2015A stubbornly large mass of cold dust in the ejecta of Supernova 1987Acitations
- 2015From flux to dust mass: Does the grain-temperature distribution matter for estimates of cold dust masses in supernova remnants?citations
- 2010The mass-loss return from evolved stars to the Large Magellanic Cloud. III. Dust properties for carbon-rich asymptotic giant branch starscitations
- 2006Mid-Infrared Spectroscopy of Carbon Stars in the Small Magellanic Cloudcitations
- 2006A Spitzer mid-infrared spectral survey of mass-losing carbon stars in the Large Magellanic Cloudcitations
- 2006A Spitzer mid-infrared spectral survey of mass-losing carbon stars in the Large Magellanic Cloudcitations
Places of action
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article
Quantifying the dust in SN 2012aw and iPTF14hls with ORBYTS
Abstract
Core-collapse supernovae (CCSNe) are capable of producing large quantities of dust, with strong evidence that ejecta dust masses can grow significantly over extended periods of time. Red-blue asymmetries in the broad emission lines of CCSNe can be modelled using the Monte Carlo radiative transfer code DAMOCLES, to determine ejecta dust masses. To facilitate easier use of DAMOCLES, we present a Tkinter graphical user interface (GUI) running DAMOCLES. The GUI was tested by high school students through the Original Research By Young Twinkle Students programme, who used it to measure the dust masses formed at two epochs in Type IIP CCSNe, SN 2012aw and iPTF14hls, demonstrating that a wide range of people can contribute to scientific advancement. Bayesian methods quantified uncertainties on our model parameters. From the red scattering wing in the day 1863 Hα profile of SN 2012aw, we constrained the dust composition to large (radius >0.1 μm) silicate grains, with a dust mass of $6.0^{+21.9}_{-3.6} 10^{-4}~{ M}_$. From the day 1158 Hα profile of SN 2012aw, we found a dust mass of $3.0^{+14}_{-2.5} 10^{-4}$ M<SUB>⊙</SUB>. For iPTF14hls, we found a day 1170 dust mass of 8.1$^{+81}_{-7.6} 10^{-5}$ M<SUB>⊙</SUB> for a dust composition consisting of 50 per cent amorphous carbon and 50 per cent astronomical silicate. At 1000 d post-explosion, SN 2012aw and iPTF14hls have formed less dust than the peculiar Type II SN 1987A, suggesting that SN 1987A may have formed a larger dust mass than typical Type IIP's....