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Escape of asteroids from the main belt

机译:从主带逸出小行星

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Aims. We locate escape routes from the main asteroid belt, particularly into the near-Earth-object (NEO) region, and estimate the relative fluxes for different escape routes as a function of object size under the influence of the Yarkovsky semimajor-axis drift. Methods. We integrated the orbits of 78?355 known and 14?094 cloned main-belt objects and Cybele and Hilda asteroids (hereafter collectively called MBOs) for 100 Myr and recorded the characteristics of the escaping objects. The selected sample of MBOs with perihelion distance q & 1.3 au and semimajor axis a & 4.1 au is essentially complete, with an absolute magnitude limit ranging from H _( V ) & 15.9 in the inner belt ( a & 2.5 au ) to H _( V ) & 14.4 in the outer belt ( 2.5 au & a & 4.1 au ). We modeled the semimajor-axis drift caused by the Yarkovsky force and assigned four different sizes (diameters of 0.1, 0.3, 1.0, and 3.0 km) and random spin obliquities (either 0 deg or 180 deg) for each test asteroid. Results. We find more than ten obvious escape routes from the asteroid belt to the NEO region, and they typically coincide with low-order mean-motion resonances with Jupiter and secular resonances. The locations of the escape routes are independent of the semimajor-axis drift rate and thus are also independent of the asteroid diameter. The locations of the escape routes are likewise unaffected when we added a model for Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) cycles coupled with secular evolution of the rotation pole as a result of the solar gravitational torque. A Yarkovsky-only model predicts a flux of asteroids entering the NEO region that is too high compared to the observationally constrained flux, and the discrepancy grows larger for smaller asteroids. A combined Yarkovsky and YORP model predicts a flux of small NEOs that is approximately a factor of 5 too low compared to an observationally constrained estimate. This suggests that the characteristic timescale of the YORP cycle is longer than our canonical YORP model predicts.
机译:目标。我们从主要的小行星带定位逃生路线,特别是进入近地 - 物体(Neo)区域,并估计不同逃生路线的相对助条,因为yarkovsky半草轴漂移的影响下的物体大小的函数。方法。我们综合了78个?355的轨道,已知和14克隆的主带对象和Cybele和Hilda小行星(以下以后称为MBO),以100 myR并记录逃逸物体的特征。具有截瘫距离Q&GT的MBO所选择的MBO样品。 1.3 AU和半轴A轴A& 4.1 AU基本上是完整的,绝对限制从H _(v)& 15.9在内带(a <2.5 au)中至h _(v)& 14.4在外带中(2.5 Au& 4.1 au)。我们建模了由Yarkovsky Force引起的半臂轴漂移,并为每个测试小行星分配了四种不同尺寸(直径为0.1,0.3,1.0和3.0 km)和随机旋转倒数(0°或180°)。结果。我们发现从小行星带到Neo区域的十个以上明显的逃生路线,并且它们通常与具有木星和世俗共振的低阶平均运动共振。逃逸路径的位置与半约轴漂移率无关,因此也与小行星直径无关。当我们为太阳重力扭矩加上旋转杆的世俗演变时,逃生路线的位置同样不受影响。只有yarkovsky的模型预测,与观察到约束的通量相比,进入太高的新区域的小行星通量,并且对于较小的小行星而差异变大。与观察到约束的估计相比,亚马夫斯基和YorP模型预测了大约5倍的小型Neos的助焊剂。这表明Yorp循环的特征时间尺度比我们的规范Yorp模型预测更长。

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