An improved model of the Edgeworth-Kuiper debris disk
An improved model of the Edgeworth-Kuiper debris disk
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埃奇沃斯-柯伊伯碎片盘的改进模型
DOI：
10.1051/0004-6361/201118551
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发表时间：
2012
影响因子：
6.5
通讯作者：
T. Löhne
中科院分区：
文献类型：
--
作者：
Ch. Vitense;A.V. Krivov;H. Kobayashi;T. Löhne
与所有其他碎片盘不同的是，通过恒星光球层上的红外过量可以看到尘埃，埃奇奥尔-柯伊伯带（EKB）的尘埃发射由于黄道云的强烈前景发射而无法进行远程探测。我们通过建模获得了预期的EKB尘埃盘属性。我们把已知的海王星外天体（TNOs）作为母体，用我们的碰撞代码产生尘埃。由此产生的尘埃分布进行了修改，以考虑到引力散射和共振捕获的行星上迁移的尘埃颗粒的影响，以及升华的效果。建模的一个困难是，尘埃的数量和分布在很大程度上取决于亚公里大小的物体。这些是直接不可观察的，并且它们的属性不能通过碰撞建模来访问，因为大于（10. 60) m in the present-day EKB are not in a collisional equilibrium.为了施加额外的限制，我们在20分钟内对新视野号航天器进行了现场测量。 Au。我们表明，为了维持与这些测量结果一致的尘埃盘，TNO粒子数必须在70 ° C处有一个粒度分布的中断 公里.然而，即使这样，我们仍然有几个模型，都正确地再现了几乎恒定的尘埃撞击率在该地区的巨行星轨道，并没有违反的限制，从非检测的EKB尘埃热辐射的COBE航天器。模型化的EKB尘埃盘，符合观测约束，可以是运输为主或运输为主和碰撞为主的制度之间的中间。这种盘的面内光学厚度为τ π（r> 10 Au）~ 10- 6，分光度为fd ~ 10-7。行星和升华被发现对尘埃撞击通量和尘埃热发射的影响很小。如从10可见的EKB类似物的光谱能量分布 pc距离在波长为（40. 50）μm atF ≤ 0.5 mJy，这是不到1%的光球通量在这些波长。因此，EKB类似物不能用当今的仪器如Herschel/PACS检测。
In contrast to all other debris disks, where the dust can be seen via an infrared excess over the stellar photosphere, the dust emission of the Edgeworth-Kuiper belt (EKB) eludes remote detection because of the strong foreground emission of the zodiacal cloud. We accessed the expected EKB dust disk properties by modeling. We treated the debiased population of the known trans-Neptunian objects (TNOs) as parent bodies and generated the dust with our collisional code. The resulting dust distributions were modified to take into account the influence of gravitational scattering and resonance trapping by planets on migrating dust grains as well as the effect of sublimation. A difficulty with the modeling is that the amount and distribution of dust are largely determined by sub-kilometer-sized bodies. These are directly unobservable, and their properties cannot be accessed by collisional modeling, because objects larger than (10...60) m in the present-day EKB are not in a collisional equilibrium. To place additional constraints, we used in-situ measurements of the New Horizons spacecraft within 20 AU. We show that to sustain a dust disk consistent with these measurements, the TNO populationhasto have a break in the size distribution ats≲ 70 km. However, even this still leaves us with several models that all correctly reproduce nearly constant dust impact rates in the region of giant planet orbits and do not violate the constraints from the non-detection of the EKB dust thermal emission by the COBE spacecraft. The modeled EKB dust disks, which conform to the observational constraints, can either be transport-dominated or intermediate between the transport-dominated and collision-dominated regime. The in-plane optical depth of such disks isτ∥(r> 10 AU) ~ 10-6and their fractional luminosity isfd~ 10-7. Planets and sublimation are found to have little effect on dust impact fluxes and dust thermal emission. The spectral energy distribution of an EKB analog as seen from 10 pc distance peaks at wavelengths of (40...50)μm atF≈ 0.5 mJy, which is less than 1% of the photospheric flux at those wavelengths. Therefore, EKB analogs cannot be detected with present-day instruments such asHerschel/PACS.
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