Broadband Polarimetry of Supernovae: SN 1994D, SN 1994Y, SN 1994ae, SN 1995D, and SN 1995H
Broadband Polarimetry of Supernovae: SN 1994D, SN 1994Y, SN 1994ae, SN 1995D, and SN 1995H
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超新星宽带偏振测量：SN 1994D、SN 1994Y、SN 1994ae、SN 1995D 和 SN 1995H
DOI：
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发表时间：
1996
期刊：
影响因子：
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通讯作者：
A. Clocchiatti
中科院分区：
文献类型：
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作者：
Lifan Wang;J. C. Wheeler;Zong;A. Clocchiatti
我们对三颗Ia型超新星（SN Ia）和两颗II型超新星（SN II）进行了偏振观测。没有明显的极化被检测到的任何一个SN Ia下降到0.2\%的水平，而1.0\%$的顺序极化被检测到的两个SN II 1994 Y和1995 H。所有的SNe与极化数据的目录编译，显示了一个明显的趋势，所有5个SN II与足够的极化数据显示在1%左右的极化，而没有9个SN Ia样品中显示出内在的极化。这种超新星极化的系统性差异，如果得到证实，将引发许多关于超新星爆炸机制的有趣问题。我们的观察增强了Ia型超新星作为通过各种技术确定距离尺度的工具的使用，但建议在使用II型超新星进行距离测定时必须非常谨慎。然而，我们要提醒的是，超新星的非球面性和测量的"内在“偏振之间的联系是复杂的反射光从拱星物质和干预星际物质，所谓的光回波。这种效应对超新星II的贡献可能比对超新星Ia的贡献更大。Ia型超新星偏振的严格限制可能会限制具有广泛散射星云的祖先模型，如共生星和其他大量质量损失的系统。
We have made polarimetric observations of three Type Ia supernovae (SN Ia) and two type II supernovae (SN II). No significant polarization was detected for any of the SN Ia down to the level of 0.2\%, while polarization of order $1.0\%$ was detected for the two SN II 1994Y and 1995H. A catalog of all the SNe with polarization data is compiled that shows a distinct trend that all the 5 SN II with sufficient polarimetric data show polarizations at about 1\%, while none of the 9 SN Ia in the sample show intrinsic polarization. This systematic difference in polarization of supernovae, if confirmed, raises many interesting questions concerning the mechanisms leading to supernova explosions. Our observations enhance the use of SN Ia as tools for determining the distance scale through various techniques, but suggest that one must be very cautious in utilizing Type II for distance determinations. However, we caution that the link between the asphericity of a supernova and the measured ``intrinsic' polarization is complicated by reflected light from the circumstellar material and the intervening interstellar material, the so-called light echo. This effect may contribute more substantially to SN II than to SN Ia. The tight limits on polarization of SN Ia may constrain progenitor models with extensive scattering nebulae such as symbiotic stars and other systems of extensive mass loss.