How do the most massive stars explode? A new model of massive stars predicts new observational evidence.
How does a massive star’s rotation affect the properties of its eventual explosion?
Some GRB-SNe pairs show interesting correlations across their light curves.
Spectra from the light echoes of distant supernovae can be used to probe the three dimensional structure of these massive and poorly-understood explosions.
Archival data are able to place constraints on the origin of supernova 2011fe.
By examining their expansion rate over time, Type II supernovae provide a way to measure extragalactic distances.
There might be more information in the Hubble diagram of supernovae than we first thought. Far away supernovae are subject to gravitational lensing and in the upcoming decades, they could be used to determine how much matter there is in the Universe and how it clusters.
This month’s undergraduate research post features pulsars as a probe of our galaxy’s magnetic field, and the possibility of asymmetries in supernovae associated with gamma-ray bursts.
Supernovae happen in the Milky Way at a rate of two or three per century. But, will we be able to see it when it happens next, or will dusty galactic center prevent us from studying it?
In this paper the authors present simulations of a model to explain rapidly-fading supernovae, a class of transients whose lightcurves decline quickly without substantial radioactive tails. They posits a standard core-collapse explosion of a standard Type Ib/Ic supernova progenitor, but one that produces very little radioactivity and instead exhibits a light curve governed by oxygen recombination.