Silicate Emission Feature in the Spectrum of Comet Mueller 1993a
Silicate Emission Feature in the Spectrum of Comet Mueller 1993a
复制标题
米勒彗星 1993a 光谱中的硅酸盐发射特征
DOI：
10.1006/icar.1994.1200
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发表时间：
1994
期刊：
影响因子：
--
通讯作者：
D. Lynch
中科院分区：
文献类型：
--
作者：
M. Hanner;J. Hackwell;R. Russell;D. Lynch
Mueller 1993 a彗星是一颗动力学上的新彗星，在R = 2 Au时获得了8 ~ 13 μm的光谱。强烈的，结构化的硅酸盐发射存在，非常类似于彗星P/哈雷在较小的R。这是首次在新彗星中探测到11.2 μm的结晶橄榄石峰，表明结晶橄榄石颗粒在太阳星云中广泛存在。结晶橄榄石粒子可能在温度高于1200 K的原太阳星云内部形成;将这些颗粒运送到彗星形成区域需要广泛的径向混合。要么是太阳星云中的径向混合比目前一些理论预测的要多，要么是橄榄石颗粒起源于太阳系前。
Abstract An 8- to 13-μm spectrum of comet Mueller 1993a, a dynamically new comet, was acquired when the comet was at R = 2 AU. Strong, structured silicate emission is present, closely resembling that seen in Comet P/Halley at smaller R. For the first time in a new comet, the 11.2-μm peak of crystalline olivine was detected, demonstrating that crystalline olivine particles were widespread in the solar nebula. Crystalline olivine particles could have formed in the inner protosolar nebula at temperatures greater than 1200 K; extensive radial mixing would have been required to transport these grains to the region of comet formation. Either there was more radial mixing in the solar nebula than some current theories predict or the olivine grains have a presolar origin.