The Imprint of Nova Nucleosynthesis in Presolar Grains
The Imprint of Nova Nucleosynthesis in Presolar Grains
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DOI：
10.1086/422569
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发表时间：
2002-10
期刊：
影响因子：
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通讯作者：
J. José;M. Hernanz;S. Amari;K. Lodders;E. Zinner
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文献类型：
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作者：
J. José;M. Hernanz;S. Amari;K. Lodders;E. Zinner
新星光曲线的红外和紫外观测证实了它们膨胀的壳层中颗粒的形成，这些壳层是由热核失控抛射到星际介质中的。本文基于20个新星爆炸流体动力学模型，给出了CO和一颗新星喷出物中质量元素直至硅的同位素比率。这些理论估计将有助于正确识别原始陨石中的新星颗粒。此外，平衡冷凝计算用于预测新星喷出物中可能存在的颗粒类型，为在O b> C环境中令人困惑的富C尘埃的形成提供了一些线索。这些结果表明，SiC颗粒可以在一个新星中凝聚，这与推断出的几个太阳前SiC颗粒的（一个）新星起源一致。
Infrared and ultraviolet observations of nova light curves have confirmed grain formation in their expanding shells that are ejected into the interstellar medium by a thermonuclear runaway. In this paper we present isotopic ratios of intermediate-mass elements up to silicon for the ejecta of CO and ONe novae, based on 20 hydrodynamic models of nova explosions. These theoretical estimates will help to properly identify nova grains in primitive meteorites. In addition, equilibrium condensation calculations are used to predict the types of grains that can be expected in the nova ejecta, providing some hints on the puzzling formation of C-rich dust in O > C environments. These results show that SiC grains can condense in ONe novae, in concert with an inferred (ONe) nova origin for several presolar SiC grains.