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 _⊙. 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 _⊙, have many properties in common with observed Type Ib and Ic supernovae, including a median ejected mass near 2 M _⊙, explosion energies near 1 10⁵¹ erg, typical ⁵⁶Ni masses of 0.07–0.09 M _⊙, 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.

使用蒙特卡洛代码 SEDONA，可以计算超新星前超新星质量为 2.2 至 10.0 M _{⊙ 的}剥离氦星产生的超新星的多波段光度测量和光谱。这些模型代表了近距离双星的演化，并且之前已经使用参数化的一维中微子传输模型进行了分解。一个子集，即超新星前质量在 2.2-5.6 M _⊙范围内的那些，与观测到的 Ib 型和 Ic 型超新星有许多共同的特性，包括中值喷射质量接近 2 M _⊙，爆炸能量接近 1 10 ⁵¹ erg，典型的⁵⁶的0.07-0.09倪群众中号 _⊙，峰值时间约为 20 天，V - R颜色指数在V最大值后 10 天的范围很窄，接近 0.3 mag。然而，在 10 ^42.3 erg s ^-1附近的中值峰值热光度比几个观测表要暗，而且最亮的爆炸的热光度仅为 10 ^42.50 erg s ^-1。最亮的绝对B、V和R峰值的震级为 -17.2、-17.8 和 -18.0。这些限制比一些所谓的典型 Ib 型和 Ic 型超新星要暗，可能反映了我们的模型或观测分析中的问题。具有较低和较高质量的氦星也会产生可能已经观察到的有趣瞬变，包括快速、微弱、蓝色瞬变和长、红色、微弱的 Ic 型超新星。新型号专门用于 SN 2007Y、SN 2007gr、SN 2009jf、LSQ 13abf、SN 2008D 和 SN 2010X。