复杂赤道尘埃结构的近红外，光学和紫外偏振和定时研究
A near-infrared, optical and ultraviolet polarimetric and timing investigation of complex equatorial dusty structures
摘要：
上下文从恒星到活动星系核，许多天体物理系统都被赤道分布的尘埃物质所包围，在许多情况下，即使使用最先进的设施，空间也无法解析。目的。在本文中，我们调查，如果以及如何可以确定未解决的和不均匀的形态尘埃分布的中央明亮的来源，使用时间分辨偏振观测。方法.我们使用偏振辐射转移模拟研究样品的环核尘埃形态。我们探索了一个网格的均匀，碎片化，密度分层，几何可变模型在近红外，光学和紫外波段，并提出其独特的时间依赖性偏振签名。结果正如预期的那样，改变遮蔽赤道盘的结构对我们观察到的与倾角相关的通量、偏振度和角度以及时滞有着深刻的影响。我们发现，分层介质是可区分的时间分辨的偏振观测，预期的偏振是在红外波段比在紫外线高得多。然而，由于尘埃升华所施加的物理尺度，总通量和偏振通量之间的平均时滞是重要的（数月至数年），延长了打破更复杂（因此也更退化）模型所需的观测活动。在紫外波段，时间滞后比红外或光学波段稍短，加上稀释星光通量较低，紫外波段的时间分辨偏振法似乎更有希望用于未来的活动。
英文摘要：
Context. From stars to active galactic nuclei, many astrophysical systems are surrounded by an equatorial distribution of dusty material that are, in a number of cases, spatially unresolved even with cutting edge facilities. Aims. In this paper, we investigate if and how one can determine the unresolved and heterogeneous morphology of dust distribution around a central bright source using time-resolved polarimetric observations. Methods. We use polarized radiative transfer simulations to study a sample of circumnuclear dusty morphologies. We explore a grid of uniform, fragmented, density-stratified, geometrically-variable models in the near-infrared, optical and ultraviolet bands, and present their distinctive time-dependent polarimetric signatures. Results. As expected, varying the structure of the obscuring equatorial disk has a deep impact on the inclination-dependent flux, polarization degree and angle, and time-lags we observe. We find that stratified media are distinguishable by time-resolved polarimetric observations, and that the expected polarization is much higher in the infrared band than in the ultraviolet. However, due to the physical scales imposed by dust sublimation, the average time-lags between the total and polarized fluxes are important (months to years), lengthening the observational campaigns necessary to break more sophisticated (and therefore also more degenerated) models. In the ultraviolet band, time-lags are slightly shorter than in the infrared or optical bands, and, coupled to lower diluting starlight fluxes, time-resolved polarimetry in the UV appears more promising for future campaigns.
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