“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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＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay

<math>N(a)\propto a^{−3.5}</math>
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＊MRN model(Mathis, Rumpl & Nordsiek 1977) ,describes the size distribution of dust grains in the MilkWay <math>N(a)\propto a^{−3.5}</math>
:*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.
:*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;

*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

2015年3月20日 (五) 04:25的版本

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 (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;
  • 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
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