“尘埃”的版本间差异
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*发射线的消光可能和连续谱的消光不同 |
*发射线的消光可能和连续谱的消光不同 |
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*Halpha/Hbeta 线比 |
*Halpha/Hbeta 线比 |
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:e.g. If the two Si II transitions at 1260 and 1527A are optically thin, then the ratio of their equivalent widths will be W1260/W1527 > 6. The observed ratio is W1260/W1527 ~ 1, implying that the lines are saturated and hence their depths are sensitive to the covering fraction of Si II-enriched material. |
:e.g. If the two Si II transitions at 1260 and 1527A are optically thin, then the ratio of their equivalent widths will be W1260/W1527 > 6. The observed ratio is W1260/W1527 ~ 1, implying that the lines are saturated and hence their depths are sensitive to the covering fraction of Si II-enriched material. |
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:对于比912A更短的波长来说，气体的吸收消光是最主要的而不是dust，但是气体和尘埃是相关的，参见[http://arxiv.org/abs/1606.00434] |
:对于比912A更短的波长来说，气体的吸收消光是最主要的而不是dust，但是气体和尘埃是相关的，参见[http://arxiv.org/abs/1606.00434] |
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*分子云中的turblence导致尘埃粒子按照颗粒大小分层分布，可以解释分子云中的消光曲线和其它地方不同[https://arxiv.org/abs/1706.05055] |
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:可以延展到2R25，[http://arxiv.org/abs/1607.01020]: |
:可以延展到2R25，[http://arxiv.org/abs/1607.01020]: |
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:密度轮廓比较follow恒星，而不是恒星形成（气体？） |
:密度轮廓比较follow恒星，而不是恒星形成（气体？） |
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:有温度梯度，从中心25K到边缘15K |
:有温度梯度，从中心25K到边缘15K |
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:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象？ |
:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象？ |
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:多波段结果进行对比[https://arxiv.org/abs/1706.05351] |
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*分子云中的turblence导致尘埃粒子按照颗粒大小分层分布[https://arxiv.org/abs/1706.05055] however we find evidence for 'size-sorting' of grains, where turbulence preferentially concentrates larger grains into dense regions. Size-sorting may help to explain observations of 'coreshine' from dark clouds, and why extinction laws differ along lines of sight through molecular clouds in the Milky Way compared to the diffuse interstellar medium. |
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2017年6月19日 (一) 13:31的版本
- 发射线的消光可能和连续谱的消光不同
- Halpha/Hbeta 线比
- 内禀数值：2.86（恒星形成），3.1（AGN） 参见Osterbrock & Ferland 2006
- 尘埃在8000A左右有一个Extended Red Emission(ERE)的连续谱发射
- 尘埃的红外发射: dustEM
- 尘埃与气体有关，气体的光深可以从low-ionization interstellar (IS) absorption lines(e.g., Si II, O I, Fe II)获得 (Shapley et al. 2003)
- e.g. If the two Si II transitions at 1260 and 1527A are optically thin, then the ratio of their equivalent widths will be W1260/W1527 > 6. The observed ratio is W1260/W1527 ~ 1, implying that the lines are saturated and hence their depths are sensitive to the covering fraction of Si II-enriched material.
- 对于比912A更短的波长来说，气体的吸收消光是最主要的而不是dust，但是气体和尘埃是相关的，参见[1]
- 模型THEMIS The Heterogeneous dust Evolution Model for Interstellar Solids) [2]
消光曲线
- 分子云中的turblence导致尘埃粒子按照颗粒大小分层分布，可以解释分子云中的消光曲线和其它地方不同[3]