ブラックホールの伴侶であるBe型恒星
J Casares1, I Negueruela2, M Ribó3
11] Instituto de Astrofísica de Canarias, E-38205 La Laguna, Santa Cruz de Tenerife, Spain [2] Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Santa Cruz de Tenerife, Spain.
Nature
|January 17, 2014
まとめ
天文学者は,軌道の円盤線の観測を用いて,ビー星,MWC 656のブラックホールの仲間を発見しました. この発見は,ブラックホール-Be 星のバイナリがX線調査で検出するのが難しいことを示唆しています.
科学分野:
- 天体物理学 天体物理学
- 恒星の進化について
- X線天文学 X線天文学
背景:
- 恒星質量のブラックホールは,通常,二重星系におけるガス蓄積からのX線放射によって発見される.
- バイナリ進化モデルでは,ブラックホールがBe星から形成されると予測しているが,同伴星として観測されたのは中性子星のみである.
- Be star MWC 656のブラックホールの同伴者が存在するという以前の主張は,限られたデータに基づいていた.
研究 の 目的:
- ベー星MWC 656.6のブラックホールの存在と質量を確認するためです.
- ブラックホール-ビー・スター・バイナリの増積特性と検出可能性を調査する.
主な方法:
- MWC 656.6の軌道を反映した蓄積円盤線が観測されました.
- Fe II プロファイルを装着することによって,ベスターの改善された半径速度曲線を取得しました.
- ベ星のスペクトル分類を精進した.
主要な成果:
- 3.8~6.9太陽質量のブラックホールの仲間がMWC 656.6の周りを回っていることが確認されました.
- ブラックホールはX線静止状態で,放射的に非効率な流れを通じて増加しています.
- システムの低X線光度により,標準的な調査では検出が困難です.
結論:
- この研究は,ビー星系MWC 656のブラックホールの同伴存在の強力な証拠を提供します.
- ブラックホール・ビー・スター・バイナリは,これまで考えられていたよりも一般的だが,検出は困難である.
- 将来の調査は,X線調査以外の代替検出方法を検討する必要があります.
関連する概念動画
01:10Detection of Black Holes
1.7K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
1.7K
01:21Schwarzschild 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
01:12Reduced 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
01:14Gravitation 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
01:18Kepler'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
01:10Kepler'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