论文标题
潜在的双重性小行星的明智/新型多上观察成像：（3200）Phaethon，2005年UD和1999年YC
WISE/NEOWISE Multi-Epoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD and 1999 YC
论文作者
论文摘要
我们介绍了可能是双子化相关的小行星的空间热红外观测：（3200）Phaethon，2005 UD和1999 YC使用Wise/Neowise。这些图像是在四个波长频段（W1），4.6 $ $ m（W2），12 $μ$ m（W3）和22 $μ$ m（W4）的四个波长频段中拍摄的。我们没有发现在十年多上述数据集中小行星中持久质量损失的证据。我们为Phaethon设定了Q <2kg S $^{ - 1} $的质量损失率，对于2005 UD和1999 YC的<0.1kg S $^{ - 1} $，几乎没有观察到的HeliePentric距离的依赖性。对于Phaethon来说，即使最大质量损失在双子座流的1000年动态时代持续下去，它也超过两个数量级，而无法提供报道的流质量（1E13 $ - $ 14公斤）。未在r = 2.3au下检测到与phaethon相关的尘埃径（GEMINID流），对应于$τ$ <7e-9的光学深度的上限。此外，未发现与半径<650m的小行星共同移动的小行星。命运+灰尘分析仪将能够检测到距Phaethon远距离（> 50,000公里）的10美元$ M大小的星际尘埃颗粒中的几个。从2005年开始，如果质量损失率持续了白天的六二烷六体族流的10,000元动力学年龄，则该流的质量将为〜1e10kg。 1999年的YC图像既没有显示相关的灰尘步道（$τ$ <2e-8），也没有在r = 1.6au时与Radii r <1.70亿的对象共同移动。这些限制的估计物理参数不能解释双子聚体流的生产机制。最后，为了探索双子座的起源，我们讨论了与phaethon的可能是钠（NA）驱动的围场活动有关的数据的含义。
We present space-based thermal infrared observations of the presumably Geminid-associated asteroids: (3200)Phaethon, 2005 UD and 1999 YC using WISE/NEOWISE. The images were taken at the four wavelength bands 3.4$μ$m(W1),4.6$μ$m(W2),12$μ$m(W3),and 22$μ$m(W4). We find no evidence of lasting mass-loss in the asteroids over the decadal multi-epoch datasets. We set an upper limit to the mass-loss rate in dust of Q<2kg s$^{-1}$ for Phaethon and <0.1kg s$^{-1}$ for both 2005 UD and 1999 YC, respectively, with little dependency over the observed heliocentric distances of R=1.0$-$2.3au. For Phaethon, even if the maximum mass-loss was sustained over the 1000(s)yr dynamical age of the Geminid stream, it is more than two orders of magnitude too small to supply the reported stream mass (1e13$-$14kg). The Phaethon-associated dust trail (Geminid stream) is not detected at R=2.3au, corresponding an upper limit on the optical depth of $τ$<7e-9. Additionally, no co-moving asteroids with radii r<650m were found. The DESTINY+ dust analyzer would be capable of detecting several of the 10$μ$m-sized interplanetary dust particles when at far distances(>50,000km) from Phaethon. From 2005 UD, if the mass-loss rate lasted over the 10,000yr dynamical age of the Daytime Sextantid meteoroid stream, the mass of the stream would be ~1e10kg. The 1999 YC images showed neither the related dust trail ($τ$<2e-8) nor co-moving objects with radii r<170m at R=1.6au. Estimated physical parameters from these limits do not explain the production mechanism of the Geminid meteoroid stream. Lastly, to explore the origin of the Geminids, we discuss the implications for our data in relation to the possibly sodium (Na)-driven perihelion activity of Phaethon.
