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Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

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,...
Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

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...
Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

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...
Eccentricity of an Ellipse01:27

Eccentricity of an Ellipse

An ellipse is a fundamental conic section defined by the constant sum of distances from any point on its curve to two fixed points, known as the foci. This geometric property can be physically demonstrated using a pencil, string, and two pins. By anchoring the string at both ends and maintaining it taut with a pencil, one can trace the outline of an ellipse.The shape and extent of the ellipse are determined by its eccentricity, e, defined as the ratio of the distance between the center and a...
Trigonometric Substitution01:23

Trigonometric Substitution

Trigonometric substitution is a technique used to simplify integrals that contain square root expressions involving quadratic forms. It is particularly effective when the integrand includes terms resembling those found in standard geometric equations, such as circles or ellipses.Molniya satellites follow highly elliptical orbits, repeatedly sweeping out the same regions of space as they revolve around Earth. To estimate the area enclosed by such an orbit, the path is modeled as an ellipse...
Variability: Analysis01:11

Variability: Analysis

Measures of variability are statistical metrics that reveal the dispersion pattern within a dataset. They are pivotal in biostatistics, providing insights into the heterogeneity within health and biological data. Variability signifies the degree to which data points diverge from one another, helping researchers understand the potential range of values and associated uncertainty within the data.
The range is a simple measure of variability, indicating the difference between the highest and...

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Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
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Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

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精密な太陽の形とその変動性

J R Kuhn1, R Bush, M Emilio

  • 1Institute for Astronomy, University of Hawaii, Pukalani, Maui, HI 96790, USA. kuhn@ifa.hawaii.edu

Science (New York, N.Y.)
|August 21, 2012
PubMed
まとめ
この要約は機械生成です。

太陽の正確な形状は未だに捉え難いままです. この研究は,表面活動に影響を受けない恒常的な太陽の平らさを明らかにし,太陽の外層の自転が遅くなることを示唆しています.

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Scattering And Absorption of Light in Planetary Regoliths
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Last Updated: May 19, 2026

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
06:48

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

Scattering And Absorption of Light in Planetary Regoliths
11:34

Scattering And Absorption of Light in Planetary Regoliths

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Indoor Experimental Assessment of the Efficiency and Irradiance Spot of the Achromatic Doublet on Glass (ADG) Fresnel Lens for Concentrating Photovoltaics
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Published on: October 27, 2017

科学分野:

  • ソーラー物理学 ソーラー物理学
  • 星の天体物理学 星の天体物理学
  • ヘリオフィジックス ヘリオフィジックス

背景:

  • 太陽の正確な形状を決定することは,広範な光電気観測にもかかわらず,挑戦的でした.
  • 完璧な球体 (非球体性) から太陽の偏差は,太陽の内部状態と太陽大気の敏感な指標です.

研究 の 目的:

  • 長期にわたる宇宙実験による高解像度データを使用して,太陽の形状を正確に決定する.
  • 太陽周期の変動が太陽の形状に及ぼす影響を調査し,理論的な予測と結果を比較する.

主な方法:

  • 長年にわたる宇宙での実験から得られたデータの分析.
  • 高空間解像度技術の適用により,太陽四肢の形状を測定する.
  • 観測された太陽のぼろぼろさと理論モデルを比較する.

主要な成果:

  • 太陽の平らな形状は,はっきりと恒定であり,太陽周期の表面の変動によって著しく影響を受けないことがわかりました.
  • 測定された太陽のぼろぼろさは,現在の理論モデルによって予測されるよりも著しく低い.
  • この不一致は,太陽の大気圏の外層の微分回転が遅いことを示唆している.

結論:

  • 太陽の形状は安定しており,表面活動から大きく独立しています.
  • 現在のモデルでは,太陽の外部地域における微分回転速度に関する精細化が必要になる可能性があります.
  • この発見は,太陽の内部ダイナミクスと大気の振る舞いを理解するための新しい制約を提供します.