Video Experimental Relacionado

Updated: May 3, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 16, 2013

Formación rápida de planetasimales en los discos circunestelares turbulentos

Anders Johansen¹, Jeffrey S Oishi, Mordecai-Mark Mac Low

¹Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany. johansen@mpia.de

|August 31, 2007

Resumen

La formación de planetas se explica por las rocas que se derrumban eficientemente gravitacionalmente dentro de los discos circumestelares. Este proceso supera los desafíos de la adherencia de la roca y el arrastre del gas, formando planetesimales rápidamente.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
La astrofísica es la astrofísica.
Dinámica de fluidos por computación.

Sus antecedentes:

La formación de planetas implica la acumulación de granos de polvo en los discos circumestelares.
El crecimiento de rocas de tamaño de metro a planetesimales a escala de kilómetro es un desafío clave.
Las rocas se enfrentan a una mala adherencia y a la deriva hacia adentro debido a los vientos en contra del gas.

Objetivo del estudio:

Investigar los mecanismos para la transición boulder-to-planetesimal.
Determinar si el colapso gravitacional puede ocurrir en discos protoplanetarios turbulentos.
Identificar las vías para la rápida formación planetesimal.

Principales métodos:

Colapso gravitacional simulado de rocas en discos de gas turbulento.
Concentración analizada de sólidos en regiones de alta presión.
Investigó el papel de la inestabilidad del flujo en la mejora de la densidad de los sólidos.

Principales resultados:

Las rocas se someten eficientemente al colapso gravitacional en regiones de disco excesivamente densas.
Las concentraciones son amplificadas por la inestabilidad del flujo gas-sólido.
Formaron cúmulos gravitatorios con masas de planetas enanos y diversos tamaños de roca.
El colapso ocurre más rápido que la deriva radial.

Conclusiones:

El colapso gravitacional en regiones demasiado densas proporciona un mecanismo viable para la formación planetaria.
Este proceso evita las limitaciones de la adherencia de la roca y la resistencia del gas.
Ofrece una solución para la rápida formación de planetesimales en discos de acreción.

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

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

Published on: May 10, 2020

Videos de Conceptos Relacionados

Non-uniform Circular Motion

Non-uniform Circular Motion

In uniform circular motion, the particle executing circular motion has a constant speed, and the circle is at a fixed radius. However, not all circular motion occurs at a constant speed. A particle can travel in a circle and speed up or slow down, showing an acceleration in the direction of motion. In that case, the motion is called non-uniform circular motion, and an additional acceleration is introduced, which is in the direction tangential to the circle.
For example, such...

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...

Circular Orbits and Critical Velocity for Satellites

Circular Orbits and Critical Velocity for Satellites

The Moon orbits around the Earth. In turn, the Earth (and other planets) orbit the Sun. The space directly above our atmosphere is filled with artificial satellites in orbit. One can examine the circular orbit, the simplest kind of orbit, to understand the relationship between the speed and the period of planets and satellites with respect to their positions and the bodies that they orbit.
Nicolaus Copernicus (1473-1543) first suggested that the Earth and all other planets orbit the Sun in...

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,...

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...