English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present 1-D non-Local-Thermodynamic-Equilibrium time-dependentradiative-transfer simulations for supernovae (SNe) of type IIb, Ib, and Icthat result from the terminal explosion of the mass donor in a close-binarysystem. Here, we select three ejecta with a total kinetic energy of ~1.2e51erg,but characterised by different ejecta masses (2-5Msun), composition, andchemical mixing. The type IIb/Ib models correspond to the progenitors that haveretained their He-rich shell at the time of explosion. The type Ic model arisesfrom a progenitor that has lost its helium shell, but retains 0.32Msun ofhelium in a CO-rich core of 5.11Msun. We discuss their photometric andspectroscopic properties during the first 2-3 months after explosion, andconnect these to their progenitor and ejecta properties including chemicalstratification. For these three models, Arnett's rule overestimates the 56Nimass by ~50% while the procedure of Katz et al., based on an energy argument,yields a more reliable estimate. The presence of strong CI lines around 9000Aprior to maximum is an indicator that the pre-SN star was under-abundant inhelium. As noted by others, the 1.08micron feature is a complex blend of CI,MgII, and HeI lines, which makes the identification of He uncertain in SNe Ibcunless other HeI lines can be identified. Our models show little scatter in(V-R) colour 10d after R-band maximum. We also address a number of radiativetransfer properties of SNe Ibc, including the notion of a photosphere, theinference of a representative ejecta expansion rate, spectrum formation,blackbody fits and "correction factors".

Radiative-transfer models for supernovae IIb/Ib/Ic from binary-star progenitors