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.
Recent computer simulations are shedding light on the brightest and most energetic phenomena in the Universe – supernova explosions. A team of researchers at the Max Planck Institute for Astrophysics modeled the formation of neutron stars in three dimensions with unprecedented accuracy, showing that as matter is drawn inward, it sloshes both asymmetrically and in spiral motions. It’s a bold, new look into the center of the supernova explosion and the birth of a neutron star.
When the supernova impostor SN2009ip brightened to a V-band absolute magnitude of -17.7 near the end of 2012, the outburst was classified as a Type IIn supernova and many observers thought the star had finally exploded for good. In this paper, however, the authors present several months of multiband imaging of transient 2012b and argue that the low limit on the nickel mass and lack of most heavy elements in the ejecta suggest the progenitor is still around, and that transient 2012b was produced instead by the collision of two massive shells, possibly ejected by the pulsational pair instability.