概括
大多数C,G,B和F类小行星的表面可能已经发生了热变形. 加热的碳状石,特别是CM2石,与小行星反射频谱密切匹配,暗示了类似的表面组成和历史.
科学领域:
- 行星科学 行星科学
- 频谱学是一种光谱学.
- 矿物学是什么?矿物学是什么?
背景情况:
- 小行星的分类依赖于光谱特性.
- 碳状石是起源于小行星的石.
- 了解小行星表面成分是太阳系形成研究的关键.
研究的目的:
- 为了比较小行星和碳酸的反射光谱.
- 为了确定小行星表面构成的潜在类似物.
- 为了研究小行星表面的热处理.
主要方法:
- 获得和分析反射频谱 (0.32.6微米).
- 来自14颗C,G,B和F小行星的光谱与21颗碳酸粉的比较.
- 实验加热默奇森CM2混石以模拟热变形.
主要成果:
- 三个经过热变异的CM-Cl混凝土显示出弱紫外线吸收,与一些小行星相匹配.
- 经过加热的默奇森CM2混石 (6001000°C) 与平均C和G类小行星光谱非常相匹配.
- 紫外线吸收分析表明大多数研究小行星的热变形 (6001000°C).
结论:
- 一些碳酸,特别是热变化的,是某些C,G,B和F类小行星的可行类型.
- 小行星表面矿物可能经历了显著的热转化.
- 光谱比较提供了关于小行星表面热史和组成的见解.
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