Chapter 10. Enhancing School Students’ Engagement in Chemistry Through a University-led Enrichment Programme

Simon, Shirley; Mallaburn, Andrea; Seton, Linda

doi:10.1039/9781788016087-00192

Cited by 1 publication

(1 citation statement)

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“…One of the core aims of the programme is to address the underrepresentation of people from socially deprived backgrounds in higher education. Longitudinal schemes are the most ef fecti ve way to increase pupil interest in taking Science, Technology, Engineering, and Mathematics (STEM) subjects at university (Simon, Mallaburn & Seton 2020 ). The ORBYTS programme achieves this goal by improving pupils' confidence in their abilities through regular interaction with their tutor, which changes the narrative on what it means to be a scientist.…”

Section: O R I G I Na L R E S E a R C H B Y Yo U N G T W I N K L E S ...mentioning

confidence: 99%

Quantifying the dust in SN 2012aw and iPTF14hls with ORBYTS

Niculescu-Duvaz

Barlow

Dunn

et al. 2022

Monthly Notices of the Royal Astronomical Society

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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 (ORBYTS) 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 $6.0^{+21.9}_{-3.6}\times 10^{-4}~M_\odot$. From the day 1158 Hα profile of SN 2012aw, we found a dust mass of $3.0^{+14}_{-2.5}\times 10^{-4}$ M⊙. For iPTF14hls, we found a day 1170 dust mass of 8.1 $^{+81}_{-7.6}\times 10^{-5}$ M⊙ for a dust composition consisting of 50 per cent amorphous carbon and 50 per cent astronomical silicate. At 1000 days 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.

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Section: O R I G I Na L R E S E a R C H B Y Yo U N G T W I N K L E S ...mentioning

confidence: 99%