Video Experimental Relacionado
Updated: Mar 31, 2026
09:14
Super-Resolution Microscopy of the Synaptonemal Complex Within the Caenorhabditis elegans Germline
Published on: September 13, 2022
3.2K
Un agujero negro supermasivo en una galaxia enana ultracompacta
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
Resumen
Las galaxias enanas ultracompactas pueden albergar agujeros negros supermasivos. El estudio de M60-UCD1 reveló un agujero negro masivo, lo que sugiere que estos sistemas densos podrían estar despojados de núcleos galácticos.
Área de la Ciencia:
- La astrofísica es la astrofísica.
- Evolución de la galaxia Evolución de la galaxia.
- La dinámica estelar es la dinámica estelar.
Sus antecedentes:
- Las galaxias enanas ultracompactas (UCD) son sistemas estelares extremadamente densos.
- Las estimaciones de masa dinámica a menudo exceden las masas basadas en la luminosidad en los UCD.
- Se debate el origen de esta discrepancia de masa: los agujeros negros supermasivos (SMBH) o las funciones de masa inicial estelar no estándar (IMF).
Objetivo del estudio:
- Para investigar la causa de la discrepancia de masa en los UCD.
- Para determinar la presencia y la masa de un agujero negro central en M60-UCD1.1.
- Comprender las vías de formación de los UCD.
Principales métodos:
- Adquisición de datos cinemáticos de óptica adaptativa para el M60-UCD1.1.
- Análisis de la dispersión y rotación de la velocidad central.
- Modelado dinámico para estimar la masa del agujero negro.
Principales resultados:
- M60-UCD1 exhibe un pico de dispersión de velocidad central >100 km/s y una rotación modesta.
- El modelado dinámico indica una SMBH de 2,1 × 10 ^ 7 masas solares.
- Este SMBH constituye el 15% de la masa total de M60-UCD1.
Conclusiones:
- La alta fracción de masa del agujero negro sugiere que M60-UCD1 es un núcleo galáctico despojado.
- La masa estelar de M60-UCD1 es consistente con su luminosidad.
- Esto implica una población significativa de pequeñas y medianas empresas no reconocidas en otros UCD.
Videos de Conceptos Relacionados
01:10Detection of Black Holes
2.6K
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...
2.6K
01:21Schwarzschild Radius and Event Horizon
3.0K
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...
3.0K
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
01:12Reduced Mass Coordinates: Isolated Two-body Problem
2.6K
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
01:18Conservation of Angular Momentum: Application
12.5K
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
01:18Kepler's Third Law of Planetary Motion
4.6K
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...
4.6K