Broad-lined type Ic supernova iPTF16asu: A challenge to all popular models

DOI: 
10.1093/mnras/stz2184
Publication date: 
01/08/2019
Main author: 
Wang, L. J.
IAA authors: 
Cano, Z.
Authors: 
Wang, L. J.;Wang, X. F.;Cano, Z.;Wang, S. Q.;Liu, L. D.;Dai, Z. G.;Deng, J. S.;Yu, H.;Li, B.;Song, L. M.;Qiu, Y. L.;Wei, J. Y.
Journal: 
Monthly Notices of the Royal Astronomical Society
Refereed: 
Yes
Publication type: 
Article
Pages: 
1110-1119
Abstract: 
It is well-known that ordinary supernovae (SNe) are powered by <SUP>56</SUP>Ni cascade decay. Broad-lined type Ic SNe (SNe Ic-BL) are a subclass of SNe that are not all exclusively powered by <SUP>56</SUP>Ni decay. It was suggested that some SNe Ic-BL are powered by magnetar spin-down. iPTF16asu is a peculiar broad-lined type Ic supernova discovered by the intermediate Palomar Transient Factory. With a rest-frame rise time of only 4 days, iPTF16asu challenges the existing popular models, for example, the radioactive heating (<SUP>56</SUP>Ni-only) and the magnetar+<SUP>56</SUP>Ni models. Here we show that this rapid rise could be attributed to interaction between the SN ejecta and a pre-existing circumstellar medium ejected by the progenitor during its final stages of evolution, while the late-time light curve can be better explained by energy input from a rapidly spinning magnetar. This model is a natural extension to the previous magnetar model. The mass-loss rate of the progenitor and ejecta mass are consistent with a progenitor that experienced a common envelope evolution in a binary. An alternative model for the early rapid rise of the light curve is the cooling of a shock propagating into an extended envelope of the progenitor. It is difficult at this stage to tell which model (interaction+magnetar+<SUP>56</SUP>Ni or cooling+magnetar+<SUP>56</SUP>Ni) is better for iPTF16asu. However, it is worth noting that the inferred envelope mass in the cooling+magnetar+<SUP>56</SUP>Ni is very high.
Database: 
ADS
SCOPUS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85077613902&doi=10.1093%2fmnras%2fstz2184&partnerID=40&md5=84cc866a5edb38f1e5fee24bb3237277
ADS Bibcode: 
2019MNRAS.489.1110W
Keywords: 
stars: mass-loss;stars: neutron;supernovae: general;supernovae: individual (iPTF16asu)