尘埃粒子的分布

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