関連する実験動画
Updated: Mar 29, 2026

06:48
Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
Published on: May 10, 2020
4.0K
低質量の火星は,木星の初期のガス駆動の移住から来ている
Kevin J Walsh1, Alessandro Morbidelli, Sean N Raymond
11] Université de Nice - Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France. kwalsh@boulder.swri.edu
Nature
|June 7, 2011
まとめ
巨大な惑星の移住は,初期の太陽系形成に影響を与えた. 木星,木星,木星,木星,木星,木星,木星,木星,木星,木星,木星,木星,木星,木星,木星
科学分野:
- 惑星科学は惑星科学である.
- 太陽系形成 太陽系形成について
- 比較惑星学とは
背景:
- 巨大な惑星である木星と土星は,ガスに支配された円盤の中で早期に形成されました.
- 彼らの軌道は,急速な,ガス駆動の移住に敏感でした.
- 陸上の惑星の形成は後になって起こったが,火星の質量は以前のモデルに挑戦をもたらした.
研究 の 目的:
- 巨大惑星の移住が地球上の惑星形成に与える影響を調査する.
- 火星の質量を含む地質惑星の観測された特徴を説明するために.
- 小惑星帯の組成の違いの起源を理解するために.
主な方法:
- 初期の太陽系の水力力学シミュレーション.
- 木星の内向と外向の移動をモデル化する.
- 惑星小円盤の進化と地上の惑星の増殖をシミュレートする.
主要な成果:
- 木星の1.5天文単位 (au) への内側への移動と,その後の外側への移動は,1 au.でプラネテシマルディスクを切り裂いた.
- 地上の惑星は,この断片化された円盤から3千万~5千万年にわたって形成され,観測された地球/火星の質量比が得られました.
- 木星の散乱は,小惑星帯の組成の二分法を説明し,内部の体は1~3 AUから,外部の体は巨大惑星の向こうから来ている.
結論:
- 巨大惑星の移住は,地上の惑星の形成を理解するために重要である.
- このモデルは,地質惑星の形成のタイムラインと特徴を調和させています.
- 木星と土星のダイナミックな振る舞いは,太陽系外の大惑星の推論を反映しています.
関連する概念動画
Kepler's First Law of Planetary Motion
6.1K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
6.1K
Acceleration due to Gravity on Other Planets
5.2K
The gravitational acceleration of an object near the Earth's surface is called the acceleration due to gravity. It can be measured by conducting simple experiments on Earth. However, such an experiment is impossible to conduct on the surface of other planets.
Astronomical observations are thus used to measure the acceleration due to gravity on other planets. This can be determined by observing the effect of a planet's gravity on objects close to it. The crucial factor that helps in this...
Astronomical observations are thus used to measure the acceleration due to gravity on other planets. This can be determined by observing the effect of a planet's gravity on objects close to it. The crucial factor that helps in this...
5.2K
Kepler's Second Law of Planetary Motion
5.8K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
5.8K
Kepler's Third Law of Planetary Motion
4.6K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
4.6K
Torque Free Motion
909
The torque-free motion refers to the movement of a rigid body in space when no external torques are acting upon it. This type of motion can be observed in environments where there are no external forces or frictions, like in outer space. For example, a rotation of Mars in space is a torque-free motion. Mars is an axisymmetric object, meaning it has an axis of symmetry along which it rotates, designated as the z-axis. The rotating frame of reference is defined such that the center of mass of...
909
Reduced Mass Coordinates: Isolated Two-body Problem
2.6K
In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
2.6K

