“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

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<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
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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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<math> N(a) \propto a^{-3.5}</math>
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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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: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;

*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

*尘埃到行星，粒子分布的gap？arXiv:2511.01957

2025年11月5日 (三) 11:45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

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
  • 尘埃到行星，粒子分布的gap？arXiv:2511.01957
取自“http://202.127.29.3/~shen/wiki/index.php?title=尘埃粒子的分布&oldid=4253”