搜索结果: 61-75 共查到“知识库 行星物理学”相关记录322条 . 查询时间(3 秒)
Planetesimal clusters in a Keplerian disk I. gravitational evolution
planetary systems formation protoplanetary disks gravitation
2015/12/25
It was recently demonstrated by numerical simulations that a turbulent flow in a rotating system is capable of efficiently concentrating passively advected particles – having a density larger thanthe ...
N-Body Simulations of Planetesimal Evolution:Effect of Varying Impactor Mass Ratio
planetesimals asteroids planetary formation collisional physics
2015/12/25
We present results from direct N-body simulations of collisions between gravitational aggregates of varying size as part of a study to parameterize planetesimal growth in the Solar System. We find tha...
Collisions and Gravitational Reaccumulation:Forming Asteroid Families and Satellites
Collisions and Gravitational Asteroid Families Satellites
2015/12/25
Numerical simulations of the collisional disruption of large asteroids show that although the parent body is totally shattered, subsequent gravitational reaccumulation leads to the formation of an ent...
Direct N-body Simulations of Rubble Pile Collisions
asteroids collisional physics impact processes planetary formation planetesimals
2015/12/25
There is increasing evidence that many kilometer-sized bodies in the Solar System are piles of rubble bound together by gravity. We present results from a project to map the parameter space of collisi...
Formation of Asteroid Families by Catastrophic Disruption:Simulations with Fragmentation and Gravitational Reaccumulation
asteroids dynamics planetesimals resonances surfaces asteroids
2015/12/25
This paper builds on preliminary work in which numerical simulations of the collisional disruption of large asteroids (represented by the Eunomia and Koronis family parent bodies) were performed and w...
Direct Large-Scale N-Body Simulations of Planetesimal Dynamics
N-body simulation planetesimals planetary formation planetary dynamics resonances
2015/12/25
We describe a new direct numerical method for simulating planetesimal dynamics in which N ～ 106 or more bodies can be evolved simultaneously in three spatial dimensions over hundreds ofdynamical times...
We have re-measured control points and re-computed a control point network for Saturn’s satellite Dione. Our network
is based on16 images (obtained by the narrow-angle cameras of Voyager I and II), 1...
用推迟引力求解GP-B轨道进动
GP-B轨道进动 推迟引力 角向加速度 引力辐射
2015/5/28
水星进动被认为是对广义相对论及其它引力理论的最重要检验。但由于Le Verrier/Newcomb等所用的行星摄动模型(质量均匀分布的圆环)太粗略，有关论证缺乏说服力。相比而言，GP-B陀螺的轨道数据是清晰的、准确的,是检验广义相对论及其它引力理论的可靠判据。考虑到GP-B轨道的偏心率极小，本文改用圆轨道的角向加速度公式计算角向附加引力是合理的, 也简化了我以前用推迟引力求解GP-B进动的方法。两...
金星对水星的牛顿轨道之摄动
太阳起潮力 地球固体潮 行星摄动 水星轨道进动
2015/5/28
行星对水星的摄动作用类似于日、月对地球上海水或地壳的潮汐作用。本文以金星对水星的摄动为例，考虑了金星在每一瞬间的摄动作用，计算了金星摄动力对水星轨道的影响。与Le Verrier和Newcomb将所有的行星轨道都看成质量均匀分布的同心圆环模型相比，本文的论证和计算方法更接近太阳系的实际情况。
哥白尼日心说推翻了托勒密地心说。开普勒椭圆理论推翻了托勒密摆线方法论。1687年，牛顿在《自然哲学的数学原理》里提出了质心说，揭露了物质运动的本质。通过逻辑推理，摆线与质心说是不同参考系的同一个理论。以公共质心（简称质心）为参考系，两个天体都绕质心运动。变换参考系，用实体为参考系，太阳绕质心运动，换成质心绕太阳运动。这样，行星绕太阳运动轨道就是摆线。摆线是天体的本质轨道。这是质心说和摆线327年的...
现在我们的理解还在于物质理论，认为物质是组成我们星球的根本。但也有很多的现象无法解释，比如地球的自转，
火山的喷发还有地壳运动等，地球中心是什么，我们探测不到，更看不到，那么地球的中心和我们的地心吸力有什么联系。
THE SINGLE-DEGENERATE BINARY ORIGIN OF TYCHO'S SUPERNOVA AS TRACED BY THE STRIPPED ENVELOPE OF THE COMPANION
X-ray arc Tycho's supernova
2014/12/20
We propose that a nonthermal X-ray arc inside the remnant of Tycho's supernova (SN) represents the interaction between the SN ejecta and the companion star's envelope lost in the impact of the explosi...
水星在太阳引力的作用下沿椭圆轨道运动，GP-B陀螺在地球引力的作用下也沿椭圆轨道运动，属于同类的物理过程; 如果史瓦西轨道方程可以正确地解释水星轨道异常，当然也应可正确地解释GP-B陀螺进动。但是，相对论物理学家们都未使用熟悉的史瓦西轨道方程去解释GP-B陀螺进动，而改用冷僻的Thomas进动公式，原因何在？我们发现，由一般史瓦西轨道方程（前提）导出的轨道近日点进动一般表达式（结论）居然不适用于一...
牛顿引力定律以极高精度解释了太阳系行星的运动轨道。对水星轨道作100年的观测，仅有微小的43角秒无法用牛顿理论去解释，偏差率只有0.000,008%。 爱因斯坦等认为，用史瓦西轨道方程可以圆满解释水星轨道的43角秒偏差；但是，近年来，部分广义相对论专家开始意识到，史瓦西轨道方程不包括其他行星对水星轨道的摄动，无法解释水星的轨道异常，试图改用后牛顿近似去解释水星轨道异常。 本文发现：在用后牛顿近似解...