论文标题
IB型和IC超新星的模型光曲线
Model Light Curves for Type Ib and Ic Supernovae
论文作者
论文摘要
使用Monte Carlo Code，Sedona，Multiband Photmogetry和Spectra是针对从2.2到10.0 $ M_ \ ODOT $的超新星衍生而来的超新星。这些模型代表了近距离二进制文件的进化，并以前使用用于中微子传输的参数化的一维模型爆炸。 A subset, those with presupernova masses in the range 2.2 - 5.6 $M_\odot$, have many properties in common with observed Type Ib and Ic supernovae, including a median ejected mass near 2 $M_\odot$, explosion energies near $1 \times 10^{51}$ erg, typical $^{56}$Ni masses 0.07 - 0.09 $ m_ \ odot $，大约20天的高峰时间，$ v $ - $ r $ $ $ $颜色指数的狭窄范围10天$ v $ -mmaximim接近0.3 mag。然而，比起几个观察性爆炸的峰值荧光量仅为10 $^{42.50} $ erg s $^{ - 1} $，比几个观测爆炸的峰值均值相比，中位峰值侧侧光度光度近10 $^{42.3} $ erg s $^{ - 1} $比几个观察爆炸均具有10 $^{42.50} $^{ - 1} $。最明亮的绝对$ b $，$ v $和$ r $ $ $ $ $ $ $，$ -17.2 $，$ -17.8 $和$ -18.0 $。这些限制比某些典型的IB和IC超新星相比，这些限制较为卑鄙，并且可以反映我们的模型或观察性分析中的问题。具有较低肿块和较高质量的氦星还会产生有趣的瞬变，这些瞬变可能已被观察到，包括快速，微弱，蓝色瞬变和长，红色，淡淡的IC超新星。专门为SN 2007Y，SN 2007GR，SN 2009JF，LSQ13ABF，SN 2008D和SN 2010x提供了新模型。
Using the Monte Carlo code, SEDONA, multiband photometry and spectra are calculated for supernovae derived from stripped helium stars with presupernova masses from 2.2 to 10.0 $M_\odot$. The models are representative of evolution in close binaries and have previously been exploded using a parametrized one-dimensional model for neutrino-transport. A subset, those with presupernova masses in the range 2.2 - 5.6 $M_\odot$, have many properties in common with observed Type Ib and Ic supernovae, including a median ejected mass near 2 $M_\odot$, explosion energies near $1 \times 10^{51}$ erg, typical $^{56}$Ni masses 0.07 - 0.09 $M_\odot$, 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 for 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 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, LSQ13abf, SN 2008D, and SN 2010X.
