Video Experimental Relacionado
Updated: Mar 13, 2026
09:44
Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
Published on: June 5, 2014
13.5K
Un sistema triple de protoestrellas formado por la fragmentación de un disco gravitatoriamente inestable
John J Tobin1,2, Kaitlin M Kratter3, Magnus V Persson2,4
1Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman, Oklahoma 73019, USA.
Nature
|October 28, 2016
Resumen
Las observaciones del sistema triple de protoestrellas L1448 IRS3B revelan una estructura de disco en espiral. Esto sugiere inestabilidad gravitacional en el disco protostellar, consistente con los modelos de formación de estrellas binarias y múltiples.
Área de la Ciencia:
- Astronomía y astrofísica
- Formación y evolución de las estrellas
Sus antecedentes:
- Los sistemas binarios y múltiples son comunes, formándose a través de la fragmentación turbulenta o la fragmentación del disco.
- La evidencia observacional de la fragmentación turbulenta existe, pero la evidencia de la fragmentación del disco se infería previamente de los sistemas evolucionados.
- El sistema triple de protoestrellas L1448 IRS3B ofrece un entorno compacto de fase temprana para estudiar la fragmentación del disco.
Objetivo del estudio:
- Para investigar la evidencia de la fragmentación del disco en las primeras etapas de la formación estelar.
- Para analizar la estructura y la dinámica del disco protostellar en el sistema L1448 IRS3B.
Principales métodos:
- Observaciones de la emisión de polvo y de gases moleculares.
- Análisis de la estructura espiral dentro del disco protostellar.
- Determinación de las separaciones y masas de las protoestrellas.
Principales resultados:
- Se observó una estructura de disco en espiral alrededor de las tres protoestrellas en L1448 IRS3B.
- Dos protoestrellas centrales están separadas por 61 UA; una protoestrella terciaria está a 183 UA dentro de un brazo espiral.
- El disco muestra susceptibilidad a la fragmentación entre 150 y 320 UA, coincidiendo con la ubicación de la protoestrella terciaria.
Conclusiones:
- Los hallazgos apoyan la teoría de la fragmentación del disco protostellar a través de la inestabilidad gravitacional.
- Esto proporciona evidencia observacional directa para la fragmentación del disco como un mecanismo para la formación de múltiples sistemas estelares.
- El sistema L1448 IRS3B sirve como un estudio de caso clave para comprender la formación temprana de estrellas binarias / múltiples.
Videos de Conceptos Relacionados
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
2.5K
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
01:20Mass Spectrometry: Molecular Fragmentation Overview
6.1K
The ionization of a molecule into a molecular ion inside the mass spectrometer causes instability in the molecule's structure due to the loss of an electron. This eventually leads to the fragmentation or breaking of some bonds in the molecule. The fragmentation occurs predominantly at specific bonds to yield relatively stable fragments.
One type of fragmentation pattern is the cleavage of a single bond in the molecular ion. The cleavage leads to a radical and a cation. The cleavage can occur at...
One type of fragmentation pattern is the cleavage of a single bond in the molecular ion. The cleavage leads to a radical and a cation. The cleavage can occur at...
6.1K
01:10Kepler's First Law of Planetary Motion
5.9K
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,...
5.9K
01:18Kepler's Third Law of Planetary Motion
4.5K
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...
4.5K
01:21Schwarzschild Radius and Event Horizon
2.9K
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...
2.9K