Search

Type Ia supernovae are thought to be the result of a thermonuclear runaway in carbon/oxygen white dwarfs, but it is uncertain whether the explosion is triggered by accretion from a non-degenerate companion star or by a merger with another white dwarf. Observations of a supernova immediately following the explosion provide unique information on the distribution of ejected material and the progenitor system. Models predict that the interaction of supernova ejecta with a companion star or circumstellar debris lead to a sudden brightening lasting from hours to days. Here we present data for three supernovae that are likely to be type Ia observed during the Kepler mission with a time resolution of 30 minutes. We find no signatures of the supernova ejecta interacting with nearby companions. The lack of observable interaction signatures is consistent with the idea that these three supernovae resulted from the merger of binary white dwarfs or other compact stars such as helium stars. [ABSTRACT FROM AUTHOR]

A correction is presented to the article "No signature of ejecta interaction with a stellar companion in three type Ia supernovae," by Rob P. Olling, Richard Mushotzky, Edward J. Shaya, Armin Rest, Peter M. Garnavich, Brad E. Tucker, Daniel Kasen, Steve Margheim, and Alexei V. Filippenko, which was published in a previous issue.