旋转不对称天体周围环的世俗演化和稳定性。问题的修正

IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS
B. P. Kondratyev, V. S. Kornoukhov
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引用次数: 0

摘要

本文提出了一种研究没有牧夫卫星的小天体的环形状的世俗演变和稳定的方法。构建了一个复合环模型,该模型由两个接近的、一般为非共面的椭圆形高斯环组成。通过边界环的相互引力能量 Wmut 考虑了环的自引力。函数 Wmut 以数列形式表示,精确度可达小偏心率和环的相互倾角的 4 次幂。复合环的世俗演化由特殊(集合)变量微分方程描述。对于没有中心体的环(问题 1),利用互能函数可以得到由八个微分方程组成的封闭系统。此外,还研究了旋转三轴体方位角平均电势中环的演变(问题 2),并得出了第二个八微分方程系统。在这两个问题中,除了一般情况外,还考虑了两个特殊情况:(i) 共面椭圆环的情况和 (ii) 带倾斜的圆环的情况。该理论被用于研究最近发现的矮行星妊神星的星环。结果表明,在不考虑自重力的情况下,妊神星环的节点前摄动时间等于 TΩ = 12.9 ± 0.7d,但考虑星环的自重力可以缩短这一周期。研究证实,自重力确实有助于保持环的形状,而无需援引牧夫卫星的假说。获得了保持星环形状的标准,从而可以估算出星环质量与 Haumea 质量之比 10-4 < m/M < 10-3 的区间。考虑到星环的光学厚度τ ≈ 0.5,可以证明质量为m/M ≈ (1-2) × 10-4的妊神星环可以由大小为({{d}_{0}} \大约 0.7{-} 1\) m)的冰粒组成。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

Secular Evolution and Stability of Rings Around Rotationally Asymmetrical Bodies. Revision of the Problem

Secular Evolution and Stability of Rings Around Rotationally Asymmetrical Bodies. Revision of the Problem

A method for studying the secular evolution and stabilization of the shape of rings in small celestial bodies that do not have shepherd satellites is developed. A model of a compound ring consisting of two close, generally non-coplanar elliptical Gaussian rings is constructed. The self-gravitation of the ring is taken into account through the mutual gravitational energy of the boundary rings Wmut. The function Wmut is presented as a series with an accuracy of up to the 4th power of small eccentricities and mutual inclination of the rings. The secular evolution of a compound ring is described by differential equations in special (collective) variables. For rings without a central body (problem 1), a closed system of eight differential equations is obtained using the mutual energy function. The evolution of rings in the azimuthally averaged potential of a rotating triaxial body is also studied (problem 2), for which a second system of eight differential equations is derived. In both problems, besides the general case, two particular ones are considered: (i) the case of coplanar elliptical rings, and (ii) the case of circular rings with a tilt. The theory is applied to study the recently discovered ring of dwarf planet Haumea. It is shown that without taking into account self-gravity, the nodal precession time of the Haumea ring is equal to TΩ = 12.9 ± 0.7d but taking into account the self-gravity of the ring can reduce this period. It is established that self-gravity does indeed contribute to the preservation of the ring shape without invoking the hypothesis of shepherd satellites. Criteria for the preservation of the ring shape are obtained, which made it possible to estimate the interval for the ratio of the ring mass to the mass of Haumea 10–4 < m/M < 10–3. Taking into account the optical thickness of the ring τ ≈ 0.5, it is shown that the Haumea ring with a mass m/M ≈ (1–2) × 10–4 can consist of ice particles with a size of \({{d}_{0}} \approx 0.7{-} 1\) m.

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来源期刊
Astronomy Reports
Astronomy Reports 地学天文-天文与天体物理
CiteScore
1.40
自引率
20.00%
发文量
57
审稿时长
6-12 weeks
期刊介绍: Astronomy Reports is an international peer reviewed journal that publishes original papers on astronomical topics, including theoretical and observational astrophysics, physics of the Sun, planetary astrophysics, radio astronomy, stellar astronomy, celestial mechanics, and astronomy methods and instrumentation.
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