Constraints on Shallow 56Ni from the Early Lightcurves of Type Ia Supernovae

TL;DR

This study uses early supernova lightcurve data and semi-analytic models to constrain the distribution of radioactive nickel on white dwarf surfaces, improving explosion timing estimates and progenitor radius constraints.

Contribution

It introduces a method to better determine explosion times using velocity evolution, enabling more accurate surface nickel distribution analysis in early Type Ia supernovae.

Findings

Nickel is located within ~0.01 solar masses from the surface in studied supernovae.

The explosion time can be constrained with improved velocity models despite systematic uncertainties.

Early lightcurve analysis refines progenitor radius estimates and supports a t^2 rise law.

Abstract

Ongoing transient surveys are presenting an unprecedented account of the rising lightcurves of Type Ia supernovae (SNe Ia). This early emission probes the shallowest layers of the exploding white dwarf, which can provide constraints on the progenitor star and the properties of the explosive burning. We use semi-analytic models of radioactively-powered rising lightcurves to analyze these observations. As we have summarized in previous work, the main limiting factor in determining the surface distribution of 56Ni is the lack of an unambiguously identified time of explosion, as would be provided by detection of shock breakout or shock-heated cooling. Without this the SN may in principle exhibit a "dark phase" for a few hours to days, where the only emission is from shock-heated cooling that is too dim to be detected. We show that by assuming a theoretically-motivated time-dependent velocity evolution, the explosion time can be better constrained, albeit with potential systematic uncertainties. This technique is used to infer the surface 56Ni distributions of three recent SNe Ia that were caught especially early in their rise. In all three we find fairly similar 56Ni distributions. Observations of SN 2011fe and SN 2012cg probe shallower depths than SN 2009ig, and in these two cases 56Ni is present merely ~0.01Msun from the WDs' surfaces. The uncertainty in this result is up to an order of magnitude given the difficulty of precisely constraining the explosion time. We also use our conclusions about the explosion times to reassess radius constraints for the progenitor of SN 2011fe, as well as discuss the roughly t^2 power law that is inferred for many observed rising lightcurves.