“尘埃粒子的分布”的版本间差异
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＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution |
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay |
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of dust grains in the MilkWay |
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:*grains larger than ∼ 0.2μm are too heavy and remain trapped in the gravitational field of the host galaxy. |
:*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; |
:*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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2015年3月20日 (五) 04:23的版本
＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay 解析失败 (语法错误): {\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;