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arXiv 1601.02506astro-ph.SRastro-ph.GAastro-ph.HE
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SN 1987 A赤道环的红外连续谱和谱线演化

Infrared Continuum and Line Evolution of the Equatorial Ring around SN 1987A

Richard G. Arendt, Eli Dwek, Patrice Bouchet, I. John Danziger, Kari A. Frank, Robert D. Gehrz, Sangwook Park, Charles E. Woodward

备注：
Accepted for publication in AJ. 22 pages, 18 figures
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摘要：

斯皮策对SN 1987 A的观测已经持续了十多年。从第4,000天开始，赤道环（ER）中的中红外（中红外）辐射主要来自激波加热的尘埃。从爆炸后的6,000到8,000天，斯皮策的观测包括3.6 - 24微米的宽带测光，以及5 - 35微米的中低分辨率光谱。在这里，我们提出了后来斯皮策观测，直到10,377天，其中只包括在3.6和4.5微米的宽带测量。这些数据表明，3.6和4.5微米的亮度在8,500天后明显开始减弱，不再像早期那样跟踪X射线发射。这可以解释为在时间尺度上比冲击气体的冷却时间短的ER中的灰尘的破坏。我们发现，后期的红外辐射的演变也类似于现在衰落的光发射。我们提供了斯皮策在第8000天之前看到的红外发射线的完整记录。过去的演变的气体所看到的红外线发射线似乎在很大程度上与光发射一致，虽然红外线[Fe II]和[Si II]线显示不同的，奇特的速度结构。

英文摘要：

Spitzer observations of SN 1987A have now spanned more than a decade. Since day ~4,000, mid-infrared (mid-IR) emission has been dominated by that from shock-heated dust in the equatorial ring (ER). From 6,000 to 8,000 days after the explosion, Spitzer observations included broadband photometry at 3.6 - 24 micron, and low and moderate resolution spectroscopy at 5 - 35 micron. Here we present later Spitzer observations, through day 10,377, which include only the broadband measurements at 3.6 and 4.5 micron. These data show that the 3.6 and 4.5 micron brightness has clearly begun to fade after day ~8,500, and no longer tracks the X-ray emission as well as it did at earlier epochs. This can be explained by the destruction of the dust in the ER on time scales shorter than the cooling time for the shocked gas. We find that the evolution of the late time IR emission is also similar to the now fading optical emission. We provide the complete record of the IR emission lines, as seen by Spitzer prior to day 8,000. The past evolution of the gas as seen by the IR emission lines seems largely consistent with the optical emission, although the IR [Fe II] and [Si II] lines show different, peculiar velocity structures.

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