関連する実験動画

Updated: Mar 31, 2026

Super-Resolution Microscopy of the Synaptonemal Complex Within the Caenorhabditis elegans Germline
09:14

Super-Resolution Microscopy of the Synaptonemal Complex Within the Caenorhabditis elegans Germline

Published on: September 13, 2022

3.2K

超コンパクトな矮星銀河の中の超大質量ブラックホール

Anil C Seth1, Remco van den Bosch2, Steffen Mieske3

  • 1Department of Physics and Astronomy, University of Utah, 115 South 1400 East, Salt Lake City, Utah 84112, USA.

Nature
|September 19, 2014
PubMed
まとめ

超コンパクトの矮星銀河は,超大質量ブラックホールを宿している可能性があります. M60-UCD1を研究したところ,巨大なブラックホールが発見され,これらの密集したシステムには銀河の核が剥がれている可能性があることを示唆した.

さらに関連する動画

Setting Limits on Supersymmetry Using Simplified Models07:46

Setting Limits on Supersymmetry Using Simplified Models

Published on: November 16, 2013

9.0K
Bringing the Visible Universe into Focus with Robo-AO10:35

Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

20.3K

関連する概念動画

Detection of Black Holes01:10

Detection of Black Holes

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...
2.6K
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

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...
3.0K
Gravitation Between Spherically Symmetric Masses01:14

Gravitation Between Spherically Symmetric Masses

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 Problem01:12

Reduced Mass Coordinates: Isolated Two-body Problem

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
Conservation of Angular Momentum: Application01:18

Conservation of Angular Momentum: Application

A system's total angular momentum remains constant if the net external torque acting on the system is zero. Examples of such systems include a freely spinning bicycle tire that slows over time due to torque arising from friction, or the slowing of Earth's rotation over millions of years due to frictional forces exerted on tidal deformations. However in the absence of a net external torque, the angular momentum remains conserved. The conservation of angular momentum principle requires a...
12.5K
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...
4.6K