Video Experimental Relacionado

Updated: Apr 28, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 15, 2013

Formación prolongada del núcleo y acreción rápida de los protoplanetas

T S Kruijer¹, M Touboul², M Fischer-Gödde³

¹Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Strasse 10, DE-48149 Münster, Germany. ETH Zürich, Inst. of Geochemistry and Petrology, Clausiusstrasse 25, CH-8092 Zürich, Switzerland.

Science (New York, N.Y.)

|June 7, 2014

Resumen

Los primeros procesos del sistema solar dieron forma a los cuerpos madre de los meteoritos. Las variaciones del tungsteno-182 revelan que la formación del núcleo tomó ~ 1 millón de años, lo que sugiere una acreción concurrente a pesar de las diferencias volátiles.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
Cosmoquímica es la cosmoquímica.
Evolución del Sistema Solar Temprano La evolución del sistema solar temprano.

Sus antecedentes:

La formación de núcleos en los cuerpos padres de los meteoritos es clave para comprender la acreción y diferenciación de los protoplanetas.
Los procesos del disco protoplanetario solar son fundamentales para la formación de los planetas.

Objetivo del estudio:

Investigar el momento y los procesos de formación del núcleo en los cuerpos madre de los meteoritos.
Comprender las implicaciones de la sincronización de la formación del núcleo en las variaciones del contenido volátil.

Principales métodos:

Análisis de las variaciones del tungsteno-182 ((182) W) en cinco grupos de meteoritos magmáticos de hierro.
Utilizando el decaimiento del extinto hafnio-182 ((182) Hf) como cronómetro.

Principales resultados:

Las variaciones observadas (182) W de 5 a 20 partes por millón indican una formación prolongada del núcleo durante ~ 1 millón de años.
La evidencia sugiere una segregación temprana de Fe-FeS seguida de una segregación posterior de fundiciones de Fe durante la formación del núcleo.
Los cuerpos madre de meteoritos de hierro probablemente se acrecentaron simultáneamente, ~ 0,1 a 0,3 millones de años después de las inclusiones ricas en calcio y aluminio (CAIs).

Conclusiones:

La formación del núcleo en los cuerpos madre de los meteoritos fue un proceso prolongado, no instantáneo.
Las variaciones de contenido volátil no se deben a diferentes tiempos de acreción, sino a procesos nebulosos locales.
Este estudio refina nuestra comprensión de la dinámica del sistema solar temprano y la formación planetesimal.

Más Videos Relacionados

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

Metal-silicate Partitioning at High Pressure and Temperature: Experimental Methods and a Protocol to Suppress Highly Siderophile Element Inclusions

Metal-silicate Partitioning at High Pressure and Temperature: Experimental Methods and a Protocol to Suppress Highly Siderophile Element Inclusions

Published on: June 13, 2015

Videos de Conceptos Relacionados

Acceleration due to Gravity on Other Planets

Acceleration due to Gravity on Other Planets

The gravitational acceleration of an object near the Earth's surface is called the acceleration due to gravity. It can be measured by conducting simple experiments on Earth. However, such an experiment is impossible to conduct on the surface of other planets.
Astronomical observations are thus used to measure the acceleration due to gravity on other planets. This can be determined by observing the effect of a planet's gravity on objects close to it. The crucial factor that helps in this...

Kepler's First Law of Planetary Motion

Kepler'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,...

Precipitate Formation and Particle Size Control

Precipitate Formation and Particle Size Control

In precipitation gravimetry, the precipitating agent should react specifically or selectively with the analyte. While a specific reagent reacts with the analyte alone, a selective reagent can react with a limited number of chemical species.
The obtained precipitate should be either a pure substance of known composition or easily converted to one by a simple process, such as ignition or drying. In addition, the precipitate should be insoluble and easily filterable. In general, filterability...

Kepler's Second Law of Planetary Motion

Kepler'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...

Kepler's Third Law of Planetary Motion

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...

Conditions on Early Earth

Conditions 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.