超新星2012 aw-原型类型IIP SN 1999 em的高能克隆
Supernova 2012aw - a high-energy clone of archetypal type IIP SN 1999em
摘要：
我们提出了密集采样的UBVRI/griz光度和低分辨率（6-10A）光学光谱观测4至270天后，新发现的II型SN 2012 aw在附近（~9.9 Mpc）星系M95的爆炸。光变曲线的视星等、颜色、辐射热光度以及显著光谱特征的存在和演化与原型IIP SNe 1999 em、1999 gi和2004 et具有惊人的相似性。SN 2012 aw的早期观测清楚地发现了爆发后37天左右V、R和I带光变曲线的极小值，这可能是复合相出现的一个观测证据。中坪MV星等（-16.67 $\pm$ 0.04）位于亮（~ -18）和亚亮（~ -15）IIP SNe之间。镍的质量为0.06 $\pm$ 0.01 M_sun。光谱的SYNOW模拟结果表明，在相当的历元上，SN 2004 et的光球速度值和演化与SN 2004 et相似，但比SN 1999 em和1999 gi的光球速度高约600 km/s。这种趋势在H α和H β的线速度中更为明显。喷出物的速度特性与现有的辐射流体动力学模拟结果的比较表明，爆炸能量在1- 2 × 10^51尔格之间;星云相位[Oi]双重态光度与SNe 2004 et和1987 A的进一步比较表明，祖星的质量约为14-15 M_sun。高速吸收功能的存在下，在中期到晚期的高原，并可能在早期阶段的光谱显示出喷出物和拱星物质之间的相互作用的迹象，与其早期的X射线和无线电波段的检测是一致的。
英文摘要：
We present densely-sampled UBVRI/griz photometric and low-resolution (6-10A) optical spectroscopic observations from 4 to 270 days after explosion of a newly discovered type II SN 2012aw in a nearby (~9.9 Mpc) galaxy M95. The light-curve characteristics of apparent magnitudes, colors, bolometric luminosity and the presence and evolution of prominent spectral features are found to have striking similarity with the archetypal IIP SNe 1999em, 1999gi and 2004et. The early time observations of SN 2012aw clearly detect minima in the light-curve of V, R and I bands near 37 days after explosion and this we suggest to be an observational evidence for emergence of recombination phase. The mid-plateau MV magnitude (-16.67 $\pm$ 0.04) lies in between the bright (~ -18) and subluminous (~ -15) IIP SNe. The mass of nickel is 0.06$\pm$0.01 M_sun. The SYNOW modelling of spectra indicate that the value and evolution of photospheric velocity is similar to SN 2004et, but about ~600 km/s higher than that of SNe 1999em and 1999gi at comparable epochs. This trend is more apparent in the line velocities of H alpha and H beta. A comparison of ejecta velocity properties with that of existing radiation-hydrodynamical simulations indicate that the energy of explosion lies in the range 1-2x10^51 ergs; a further comparison of nebular phase [Oi] doublet luminosity with SNe 2004et and 1987A indicate that the mass of progenitor star is about 14-15 M_sun. The presence of high-velocity absorption features in the mid-to-late plateau and possibly in early phase spectra show signs of interaction between ejecta and the circumstellar matter; being consistent with its early-time detection at X-ray and radio wavebands.
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