论文标题
要理解星际介质中2175Å灭绝凹凸的物理起源
Toward understanding physical origin of 2175Å extinction bump in interstellar medium
论文作者
论文摘要
1965年发现了银河系中星际培养基（ISM）的2175Å紫外线（UV）灭绝肿块。但是，在对半个多世纪以上的深入探索之后，其确切的起源仍然是一个正在辩论的大问题。在这里，我们提出了一个混合模型，通过该模型，ISM中的灭绝凸起可能与氢化的T-碳（HTC）分子（C40H16）的簇有关，该簇在波长2175Å的波长上本质上具有锐利的吸收峰。通过线性结合HTC混合物，石墨，MGSIO3和FE2SIO4的计算出的吸收光谱，我们表明可以很好地拟合可选的六颗恒星的UV灭绝曲线。本工作为理解银河系ISM的2175Å灭绝凹凸的物理起源提供了另一种解释。
The 2175 Å ultraviolet (UV) extinction bump in interstellar medium (ISM) of the Milky Way was discovered in 1965. After intensive exploration of more than a half century, however, its exact origin still remains a big conundrum that is being debated. Here we propose a mixture model by which the extinction bump in ISM is argued possibly relevant to the clusters of hydrogenated T-carbon (HTC) molecules (C40H16) that have intrinsically a sharp absorption peak at the wavelength 2175 Å. By linearly combining the calculated absorption spectra of HTC mixtures, graphite, MgSiO3 and Fe2SiO4, we show that the UV extinction curves of optional six stars can be nicely fitted. This present work poses an alternative explanation toward understanding the physical origin of the 2175 Å extinction bump in ISM of the Milky Way.
