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Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

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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.
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Kepler's Third Law of Planetary Motion01:18

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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...
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Kepler's First Law of Planetary Motion01:10

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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.
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Schwarzschild Radius and Event Horizon01:21

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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
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Reduced Mass Coordinates: Isolated Two-body Problem01:12

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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...
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Circular Orbits and Critical Velocity for Satellites01:16

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The Moon orbits around the Earth. In turn, the Earth (and other planets) orbit the Sun. The space directly above our atmosphere is filled with artificial satellites in orbit. One can examine the circular orbit, the simplest kind of orbit, to understand the relationship between the speed and the period of planets and satellites with respect to their positions and the bodies that they orbit.
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高質量 b センタウリ 二重星系 の 広い 軌道 の 巨大 惑星

Markus Janson1, Raffaele Gratton2, Laetitia Rodet3

  • 1Department of Astronomy, Stockholm University, Stockholm, Sweden. markus.janson@astro.su.se.

Nature
|December 9, 2021
PubMed
まとめ

巨大な恒星の周りに 巨大惑星が形成されることもあり これまでの仮説に 異議を唱えます この研究では 巨大な二重星系を周回する 広い軌道に惑星が発見され 惑星形成の極端を 解明することができました

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科学分野:

  • 外惑星科学
  • 恒星 と 銀河 の 天文学
  • 惑星 形成 と 進化

背景:

  • 惑星の形成は,多様な恒星質量とシステム構造で観察される.
  • 以前の研究では,太陽質量 (M) を超える恒星の周りの巨大惑星の頻度が低下していることが示され,形成障害が示唆されている.
  • 近い惑星の検出方法は 広い軌道の伴星には敏感ではありません

研究 の 目的:

  • 恒星質量パラメータ空間全体で,特に高質量で惑星の形成を調査する.
  • 巨大惑星は珍しい あるいは存在しない という仮説を検証する
  • 巨大な恒星を周回する 広い軌道に惑星が存在する可能性を 探求するためです

主な方法:

  • エクソプラネットを検出するために 直接画像技術を使用した.
  • 6から10Mのバイナリ系bセンタウリに注目した観測.
  • 惑星と星の質量比と軌道分離を分析した

主要な成果:

  • 太陽と地球の560倍の距離で 惑星の存在を確認しました
  • 惑星の質量比 (0.10-0.17%) は木星と太陽の比率に匹敵する.
  • この発見は,惑星が,これまで考えられていたよりも 遥かに大きな恒星系に 存在しうることを示しています

結論:

  • 巨大な二重星の周りの 広い軌道を持つこの惑星の形成は 核増殖モデルの限界に挑戦しています
  • 異なる形成場所からの重力不安定や移動などの代替形成メカニズムは妥当である.
  • この発見は惑星形成の 既知のパラメータ空間を拡大し 特に巨大な恒星の周りに広がります