English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/192246
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:


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

AuthorsWang, 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.
KeywordsStars: mass-loss
Stars: neutron
Supernovae: general
Supernovae: individual: iPTF16asu
Issue Date2019
PublisherOxford University Press
CitationMonthly Notices of the Royal Astronomical Society 489(1): 1110-1119 (2019)
AbstractIt is well known that ordinary supernovae (SNe) are powered by 56Ni cascade decay. Broad-lined type Ic SNe (SNe Ic-BL) are a subclass of SNe that are not all exclusively powered by 56Ni 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 d, iPTF16asu challenges the existing popular models, for example, the radioactive heating (56Ni-only) and the magnetar +56Ni 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 + 56Ni or cooling+magnetar + 56Ni) is better for iPTF16asu. However, it is worth noting that the inferred envelope mass in the cooling+magnetar + 56Ni is very high.© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Publisher version (URL)http://dx.doi.org/ 10.1093/mnras/stz2184
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2019_stz2184.pdf1,41 MBAdobe PDFThumbnail
Show full item record
Review this work

Related articles:

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.