“消光曲线”的版本间差异
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无编辑摘要 |
无编辑摘要 |
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* simple power-law <math>\propto \lambda^{-1}</math> |
* simple power-law <math>\propto \lambda^{-1}</math> |
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*在0.9mu到5mu可以近似为<math>\propto \lambda^{-1.7}</math> |
*在0.9mu到5mu可以近似为<math>\propto \lambda^{-1.7}</math> |
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*9.7,18mu有硅吸收，3.4mu有烃吸收，6.2mu有PAH吸收 |
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* the Milky Way (MW) extinction curve (with a prominent bump at 2175)理论解释 [https:// |
* the Milky Way (MW) extinction curve (with a prominent bump at 2175)理论解释 [https://arxiorg/abs/1507.03327] |
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:尺度小于0.02目的carbonaceous grains |
:尺度小于0.02目的carbonaceous grains |
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* the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV |
* the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV |
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2017年6月1日 (四) 13:53的版本
常用消光曲线
- simple power-law
- 在0.9mu到5mu可以近似为
- 9.7,18mu有硅吸收，3.4mu有烃吸收，6.2mu有PAH吸收
- the Milky Way (MW) extinction curve (with a prominent bump at 2175)理论解释 [1]
- 尺度小于0.02目的carbonaceous grains
- the featureless Small Magellanic Cloud (SMC) extinction curve which steeply rises with inverse wavelength from near-IR to far-UV
- the LargeMagellanic Cloud (LMC) curve being intermediate between that of the MW and the SMC;
- the featureless “Calzetti” attenuation law for the dust in local starburst galaxies (Calzetti et al. 1994);
- the relatively flat “Maiolino” extinction law for the dust in the dense circumnuclear region of AGNs (Maiolino et al. 2001) where the dust size distribution is skewed toward large grains
以上参见图1 [2]
类星体中的尘埃
- 一种认为和SMC差不多 Hopkins et al. (2004)
- 一种认为比较平 (Czerny et al. 2004; Gaskell et al. 2004).
see also 尘埃粒子的分布'
ARA&A文献：[3]