相关实验视频
Updated: May 2, 2026

10:35
Bringing the Visible Universe into Focus with Robo-AO
Published on: February 12, 2013
21.4K
星盘系统中的一个年轻的大质量行星
J Setiawan1, Th Henning, R Launhardt
1Max-Planck-Institut für Astronomie, Heidelberg, D-69117, Germany.
Nature
|January 4, 2008
概括
天文学家发现了一个围绕年轻恒星TW Hydrae运行的行星,证明行星形成可以在1000万年内发生. 这一发现对于理解原行星盘消散之前的行星系统发展至关重要.
科学领域:
- 外系行星科学 外系行星科学
- 恒星和子恒星物体研究研究
- 天体生物学和天体发生学
背景情况:
- 据了解,行星形成发生在围绕年轻恒星的原行星盘内.
- 精确的时间表和行星形成机制,特别是非常年轻的恒星周围,仍然是积极研究和辩论的主题.
- 之前没有在恒星周围探测到有活跃形成原行星盘的行星,这使我们对早期行星系统进化的理解产生了差距.
研究的目的:
- 为了研究非常年轻的恒星周围行星形成的可能性.
- 为了检测和描述原行星盘阶段内的行星.
- 在磁盘进化的背景下,限制行星形成的时间尺度.
主要方法:
- 对年轻恒星TW Hydrae的观测和分析,该恒星被认为拥有具有良好的特征的原行星盘.
- 通过辐射速度测量或过境光度测量 (具体方法在摘要中没有详细说明) 来检测行星伴侣.
- 描述行星的质量和轨道参数.
主要成果:
- 探测到一个质量为 (9.8+/-3.3) 木星质量的行星在TW Hydrae轨道上运行.
- 这颗行星以0.04 AU的近距离绕地球运行,周期为3.56天.
- 检测到的行星位于TW Hydrae的原行星盘的内部边缘.
结论:
- 行星可以在1000万年内形成,这比以前限制的时间尺度要短得多.
- 即使在原行星盘被恒星风和辐射完全消散之前,行星的形成也是可能的.
- 这一发现为早期行星形成提供了直接证据,并丰富了我们对行星系统起源的理解.
相关概念视频
Kepler's First Law of Planetary Motion
4.9K
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,...
4.9K
Kepler's Second Law of Planetary Motion
4.7K
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...
4.7K
Kepler's Third Law of Planetary Motion
3.6K
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...
3.6K
Schwarzschild Radius and Event Horizon
2.2K
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.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
2.2K
Gravitation Between Spherically Symmetric Masses
1.5K
The gravitational potential energy between two spherically symmetric bodies can be calculated from the masses and the distance between the bodies, assuming that the center of mass is concentrated at the respective centers of the bodies.
1.5K
Reduced Mass Coordinates: Isolated Two-body Problem
2.5K
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...
2.5K

