Video Experimental Relacionado
Updated: May 9, 2026
06:04
Simulation of the Planetary Interior Differentiation Processes in the Laboratory
Published on: November 16, 2013
El desarrollo de un disco protoplanetario desde su envoltura natal.
Dan M Watson1, C J Bohac, C Hull
1Department of Physics and Astronomy, University of Rochester, Rochester, New York 14627-0171, USA. dmw@pas.rochester.edu
Nature
|August 31, 2007
Resumen
Los astrónomos observaron la emisión de agua de la joven protoestrella NGC 1333-IRAS 4B, revelando detalles de un disco protoplanetario en formación. Este hallazgo ofrece información sobre las primeras etapas de la formación de planetas alrededor de objetos estelares jóvenes.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Formación estelar y evolución de las estrellas.
- Ciencia exoplanetaria Ciencia de los exoplanetas.
Sus antecedentes:
- Las protoestrellas de clase 0 son la etapa más temprana de los objetos estelares jóvenes, cruciales para comprender la formación del disco protoplanetario.
- Estudios anteriores indicaron regiones más cálidas y densas dentro de protoestrellas como NGC 1333-IRAS 4, pero carecían de observaciones detalladas.
- Las observaciones en longitudes de onda milimétricas han mostrado firmas cinemáticas de colapso en envolturas protostellares.
Objetivo del estudio:
- Para investigar la estructura central del sistema proto-múltiple NGC 1333-IRAS 4 en las escalas del Sistema Solar.
- Para detectar y analizar la composición del gas dentro de la región incrustada de una protoestrella de Clase 0.
- Para observar el desarrollo temprano de un disco protoplanetario.
Principales métodos:
- Observaciones en el infrarrojo medio (20-37 micrómetros) de NGC 1333-IRAS 4B.
- Análisis de la emisión de la línea molecular, específicamente agua (H2O).
- Modelado de la emisión observada para inferir las propiedades del gas y la dinámica de caída.
Principales resultados:
- Detección de un rico espectro de emisión de H2O de NGC 1333-IRAS 4B.
- La emisión se origina en un gas extremadamente denso y caliente.
- Los datos apoyan un modelo de caída en un disco denso y profundamente incrustado, lo que indica el desarrollo del disco protoplanetario.
- Este es el único objeto de Clase 0 en una muestra de 30 que muestra tal emisión de agua en el infrarrojo medio.
Conclusiones:
- Las observaciones proporcionan evidencia directa de la formación de un disco protoplanetario alrededor de una protoestrella de Clase 0.
- La detección única puede deberse a una orientación favorable o representar una fase evolutiva transitoria.
- Este estudio ofrece una rara visión de las primeras etapas críticas de la formación de planetas.
Videos de Conceptos Relacionados
02:06Conditions on Early Earth
Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
02:06Conditions on Early Earth
Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
01:10Kepler's First 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. 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,...
01:29Kepler's Second 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. 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...
01:18Kepler'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...
01:17Design Example: Calculating Safe Diameter for Wind-Exposed Disc
Assessing safety in wind-exposed installations is crucial to preventing potential failures. This example explores the calculation and design adjustments needed to mount a circular disc on a building facade, where wind forces are a primary concern. A 4-meter diameter disc was initially designed as an aesthetic feature facing winds at a velocity of 25 meters per second, with an air density of 1.25 kilograms per cubic meter. Given these conditions, the drag force on the disc was determined using...