Model Light Curves for Type Ib and Ic Supernovae

Using the Monte Carlo code SEDONA, multiband photometry and spectra are calculated for supernovae derived from stripped helium stars with presupernova masses of 2.2 to 10.0 M (circle dot). The models are representative of evolution in close binaries and have previously been exploded using a parameterized one-dimensional model for neutrino transport. A subset, those with presupernova masses in the range of 2.2-5.6 M (circle dot), have many properties in common with observed Type Ib and Ic supernovae, including a median ejected mass near 2 M (circle dot), explosion energies near 1 x 10(51) erg, typical Ni-56 masses of 0.07-0.09 M (circle dot), peak times of about 20 days, and a narrow range for the V - R color index 10 days post-V-maximum near 0.3 mag. The median peak bolometric luminosity, near 10(42.3) erg s(-1), is fainter, however, than several observational tabulations, and the brightest explosion has a bolometric luminosity of only 10(42.50) erg s(-1). The brightest absolute B, V, and R magnitudes at peak are -17.2, -17.8, and -18.0. These limits are fainter than some allegedly typical Type Ib and Ic supernovae and could reflect problems in our models or in the observational analysis. Helium stars with lower and higher masses also produce interesting transients that may have been observed, including fast, faint, blue transients and long, red, faint Type Ic supernovae. New models are specifically presented for SN 2007Y, SN 2007gr, SN 2009jf, LSQ 13abf, SN 2008D, and SN 2010X.

Automated summary

Using the Monte Carlo code SEDONA, multiband photometry and spectra were calculated for supernovae originating from stripped helium stars. Some of the models exhibit similarities with observed Type Ib and Ic supernovae, but also show differences in certain aspects. Helium stars of varying masses produce interesting transients that have been observed.