从石的Hf-W计时法对陆地行星形成的短时间尺度
Qingzhu Yin1, S B Jacobsen, K Yamashita
1Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, Massachusetts 02138, USA. yin@fas.harvard.edu
Nature
|August 29, 2002
概括
我们太阳系中的行星形成速度很快,大多数金属酸盐分离发生在3000万年内. 这一发现支持了恒星形成后不久的快速行星组装模型.
科学领域:
- 太空进化的宇宙进化
- 行星科学 行星科学
- 地质化学 地质化学
背景情况:
- 确定早期太阳系天体组装的时间表对于理解恒星和行星形成至关重要.
- 以前使用放射性核酸计时器的研究表明,像维斯塔这样的天体在300万年内迅速形成.
- 矛盾的哈夫-烯同位素数据表明后期形成 (大约. 16亿年) 和更长的陆地行星积累 (62亿年).
研究的目的:
- 解决早期太阳系天体形成时间上的差异.
- 提供关于石组成的新同位素数据.
- 改进行星积累时间尺度的模型.
主要方法:
- 在石中分析的同位素组成.
- 在石中测量哈夫-的比率.
- 将新的同位素数据与现有的计时数据进行比较.
主要成果:
- 对于几个石,获得了新的同位素和与的比率测量.
- 与之前的一些发现相反,大部分金属酸盐分离发生在3000万年内.
- 结果与快速行星形成场景一致.
结论:
- 早期太阳系的物体形成,包括金属酸盐的分离,是一个快速的过程.
- 这些发现支持对年轻恒星物体和动态积累模型的天文观测.
- 一个简短的时间范围 (大约. 10 Myr) 是用于陆地行星形成的主要生长阶段.
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