138175 (2000 EE104) and the Source of Interplanetary Field Enhancements
138175 (2000 EE104) and the Source of Interplanetary Field Enhancements
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138175 (2000 EE104) 和行星际场增强的来源
DOI：
10.3847/psj/aba68f
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发表时间：
2020
影响因子：
--
通讯作者：
D. Jewitt
中科院分区：
文献类型：
--
作者：
D. Jewitt
我们提出了首次光学观测来表征近地天体 138175 (2000 EE104)。该天体与行星际场增强（IFE）有关，被认为是由太阳风磁场和母体轨道上尾随的固体物质之间的相互作用引起的。根据光学测光法，等积球体的半径（以米为单位）和质量（以千克为单位）分别为 和 ，其中 pR 是红色几何反照率，假设密度为 ρ = 1500 kg m−3。测量到的颜色介于 C 型（原始）和 S 型（变质）小行星的颜色之间，但经过对阶段红化可能影响的校正，与 C 型分类比与 S 型更一致。没有发现半径大于 ∼40(0.1/pR) m 的共同移动伴星的证据，也没有检测到尘埃粒子尾迹，将尾迹光学深度限制为 τ ≤ 2 × 10−9。考虑到冲击粉碎产生的粒度分布，很难产生解释 IFE 所需的纳米尘埃质量（至少 105-106 千克），除非粒度分布异常陡峭。此外，所需尺寸的源物体的撞击粉碎时间尺度比动态时间尺度长得多。虽然新的光学数据并没有明确反驳巨石粉碎是 IFE 来源的假设，但也没有为其提供任何支持。
We present the first optical observations taken to characterize the near-Earth object 138175 (2000 EE104). This body is associated with interplanetary field enhancements (IFEs), thought to be caused by interactions between the solar wind magnetic field and solid material trailing in the orbit of the parent body. Based on optical photometry, the radius (in meters) and mass (in kilograms) of an equal-area sphere are found to be and , respectively, where pR is the red geometric albedo and a density of ρ = 1500 kg m−3 is assumed. The measured colors are intermediate between those of C-type (primitive) and S-type (metamorphosed) asteroids but, with correction for the likely effects of phase reddening, are more consistent with a C-type classification than with S-type. No evidence for co-moving companions larger than ∼40(0.1/pR) m in radius is found, and no dust particle trail is detected, setting a limit to the trail optical depth of τ ≤ 2 × 10−9. Consideration of the size distribution produced by impact pulverization makes it difficult to generate the mass of nanodust (minimum 105–106 kg) required to account for IFEs, unless the size distribution is unusually steep. Furthermore, impact pulverization timescales for source objects of the required size are much longer than the dynamical timescale. While the new optical data do not definitively refute the hypothesis that boulder pulverization is the source of IFEs, neither do they provide any support for it.
影响因子：
5.3
作者：
Blanton, Michael R.;Bershady, Matthew A.;Zou, Hu
通讯作者：
Zou, Hu