纺纱粉尘排放：不规则颗粒形状、瞬时加热的影响以及与WMAP结果的比较
Spinning Dust Emission: Effects of irregular grain shape, transient heating and comparison with WMAP results
摘要：
普朗克有望回答早期宇宙的关键问题，但它也提供了对异常微波发射的进一步理解。自旋尘埃粒子的电偶极辐射仍然是异常微波辐射的有利解释。本文提出了一种计算具有转动惯量的不规则小颗粒转动辐射的方法$I_{1}> I_{2}> I_{3}$。我们表明，一个转矩自由旋转的不规则颗粒与一个给定的角动量辐射在多个频率模式。所得旋转粉尘光谱具有峰值频率和发射率随颗粒形状不规则程度而增加，其由$I_{1}:I_{2}:I_{3}$定义。我们讨论了如何在体坐标系中的偶极矩$\bmu$的取向影响旋转尘埃光谱的不同制度的内部热波动。我们表明，自旋尘埃发射率的情况下，强的热波动是不太敏感的$\bmu$的取向比在弱的热波动的情况下。我们计算自旋尘埃光谱的气体密度和偶极矩的范围。研究了可压缩湍流对旋转粉尘排放强度的影响。我们表明，在湍流介质中的发射强度增加的一个因素，从1.2-1.4相对于在均匀介质中，作为音速马赫数$M_{s}$从2-7增加。最后，旋转尘埃参数的约束，通过拟合我们的改进模型，五年{ \it威尔金森微波各向异性探针}互相关前景光谱，H $α$相关和100 $μ$ m相关的发射光谱。
英文摘要：
Planck is expected to answer crucial questions on the early Universe, but it also provides further understanding on anomalous microwave emission. Electric dipole emission from spinning dust grains continues to be the favored interpretation of anomalous microwave emission. In this paper, we present a method to calculate the rotational emission from small grains of irregular shape with moments of inertia $I_{1}> I_{2}> I_{3}$. We show that a torque-free rotating irregular grain with a given angular momentum radiates at multiple frequency modes. The resulting spinning dust spectrum has peak frequency and emissivity increasing with the degree of grain shape irregularity, which is defined by $I_{1}:I_{2}:I_{3}$. We discuss how the orientation of dipole moment $\bmu$ in body coordinates affects the spinning dust spectrum for different regimes of internal thermal fluctuations. We show that the spinning dust emissivity for the case of strong thermal fluctuations is less sensitive to the orientation of $\bmu$ than in the case of weak thermal fluctuations. We calculate spinning dust spectra for a range of gas density and dipole moment. The effect of compressible turbulence on spinning dust emission intensity is investigated. We show that the emission intensity in a turbulent medium increases by a factor from 1.2-1.4 relative to that in a uniform medium, as sonic Mach number $M_{s}$ increases from 2-7. Finally, spinning dust parameters are constrained by fitting our improved model to five-year {\it Wilkinson Microwave Anisotropy Probe} cross-correlation foreground spectra, for both the H$α$-correlated and 100 $μ$m-correlated emission spectra.
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