“尘埃”的版本间差异

来自Shiyin's note
跳到导航 跳到搜索
无编辑摘要
无编辑摘要
第7行: 第7行:
: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.
: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]
*盘星系的尘埃分布,Herschel的结果
:可以延展到2R25,[http://arxiv.org/abs/1607.01020]:
密度轮廓比较follow恒星,而不是恒星形成(气体?)
:有温度梯度,从中心25K到边缘15K
:盘上的尘埃可以解释类星体的受到的intergalactic的红化现象?

2016年7月6日 (三) 01:37的版本

  • 消光曲线
  • 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]
  • 盘星系的尘埃分布,Herschel的结果
可以延展到2R25,[2]:

密度轮廓比较follow恒星,而不是恒星形成(气体?)

有温度梯度,从中心25K到边缘15K
盘上的尘埃可以解释类星体的受到的intergalactic的红化现象?