“尘埃粒子的分布”的版本间差异
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Ref. http://arxiv.org/abs/astro-ph/0603833 |
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of dust grains in the MilkWay |
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<math> N(a)\propto a^{−3.5}, </math> |
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:grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy. |
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:Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure; |
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*BF model: Bianchi & Ferrara (2005) |
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:assuming an initial flat size abundance |
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:the post-processed distribution remains nearly flat |
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:the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering |
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2015年3月20日 (五) 04:25的最新版本
Ref. http://arxiv.org/abs/astro-ph/0603833
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay 解析失败 (带SVG或PNG备选的MathML（建议用于现代的浏览器和辅助工具）：从服务器“https://wikimedia.org/api/rest_v1/”返回无效的响应（“Math extension cannot connect to Restbase.”）：): {\displaystyle N(a)\propto a^{−3.5}}
- grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy.
- Smaller grains (a<0.05μm) are either destroyed by sputtering or unable to travel far from formation sites as they are inefficiently pushed away by radiation pressure;
- BF model: Bianchi & Ferrara (2005)
- assuming an initial flat size abundance
- the post-processed distribution remains nearly flat
- the size range is slightly shifted towards smaller radii, 0.02−0.15 μm due to erosion sputtering