A Caltech Library Service

Rapidly fading supernovae from massive star explosions

Kleiser, Io K. W. and Kasen, Daniel (2014) Rapidly fading supernovae from massive star explosions. Monthly Notices of the Royal Astronomical Society, 438 (1). pp. 318-328. ISSN 0035-8711. doi:10.1093/mnras/stt2191.

PDF - Published Version
See Usage Policy.

PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


Transient surveys have recently discovered a class of supernovae (SNe) with extremely rapidly declining light curves. These events are also often relatively faint, especially compared to Type Ia SNe. The common explanation for these events involves a weak explosion, producing a radioactive outflow with small ejected mass and kinetic energy (M ∼ 0.1 M_⊙ and E ∼ 0.1 B, respectively), perhaps from the detonation of a helium shell on a white dwarf. We argue, in contrast, that these events may be Type Ib/c SNe with typical masses and energies (M ∼ 3 M_⊙, E ∼ 1 B), but which ejected very little radioactive material. In our picture, the light curve is powered by the diffusion of thermal energy deposited by the explosion shock wave, and the rapid evolution is due to recombination, which reduces the opacity and results in an ‘oxygen-plateau’ light curve. Using a radiative transfer code and simple 1D ejecta profiles, we generate synthetic spectra and light curves and demonstrate that this model can reasonably fit the observations of one event, SN 2010X. Similar models may explain the features of other rapidly evolving SNe such as SN 2002bj and SN 2005ek. SNe such as these may require stripped-envelope progenitors with rather large radii (R ∼ 20 R_⊙), which may originate from a mass-loss episode occurring just prior to explosion.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 November 7. Received 2013 November 6; in original form 2013 September 11. First published online: December 13, 2013. We would like to thank Maria Drout, Alex Heger, Mansi Kasliwal, Ehud Nakar, Christian Ott, Tony Piro, Dovi Poznanski, Josh Shiode, Alicia Soderberg and Eliot Quataert for useful discussion. This work was supported by an NSF Astronomy and Astrophysics Grant (AST-1109896) and by an NSF Division of Astronomical Sciences collaborative research grant AST-1206097. IK is supported by the Department of Energy National Nuclear Security Administration Stewardship Science Graduate Fellowship. DK is supported in part by a Department of Energy Office of Nuclear Physics Early Career Award and by the Director, Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the US Department of Energy under Contract no. DE-AC02-05CH11231.We are grateful for computing time made available by the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract no. DE-AC02-05CH11231.
Funding AgencyGrant Number
Department of Energy (DOE) National Nuclear Security AdministrationUNSPECIFIED
Department of EnergyDE-AC02-05CH11231
Subject Keywords:radiative transfer, supernovae: general, supernovae: individual: SN 2010X, supernovae: individual: SN 2002bj, supernovae: individual: SN 2005ek, supernovae: individual: SN 1994I.
Issue or Number:1
Record Number:CaltechAUTHORS:20140227-140801135
Persistent URL:
Official Citation:Io K. W. Kleiser and Daniel Kasen Rapidly fading supernovae from massive star explosions MNRAS (February 11, 2014) Vol. 438 318-328 first published online December 13, 2013 doi:10.1093/mnras/stt2191
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:44041
Deposited By: Ruth Sustaita
Deposited On:28 Feb 2014 17:13
Last Modified:10 Nov 2021 16:46

Repository Staff Only: item control page