Video Experimental Relacionado
Updated: Apr 26, 2026

11:34
Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
11.5K
Un profundo límite entre la corteza y el manto en el asteroide 4 Vesta
Harold Clenet1, Martin Jutzi2, Jean-Alix Barrat3
1EPSL, Institute of Condensed Matter Physics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Station 3, CH-1015 Lausanne, Switzerland.
Nature
|July 18, 2014
Resumen
El asteroide Vesta fue descubierto.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- Investigación de asteroides Investigación de asteroides.
- La geofísica es la geofísica.
Sus antecedentes:
- El asteroide 4 Vesta exhibe dos grandes cráteres de impacto cerca de su polo sur.
- Estos cráteres exponen material subterráneo, ofreciendo información sobre la estructura interna de Vesta.
- El modelado anterior indicaba diferentes profundidades para el material de la superficie en los hemisferios de Vesta.
Objetivo del estudio:
- Para analizar los datos del asteroide 4 Vesta.
- Para determinar la profundidad del límite entre la corteza y el manto de Vesta (Moho).
- Para investigar la composición de las capas exteriores de Vesta.
Principales métodos:
- Análisis de los datos del cráter de impacto del asteroide 4 Vesta.
- Modelado de la exposición del material subterráneo.
- Interpretación geofísica de la estructura de Vesta.
Principales resultados:
- El material de la superficie en el hemisferio norte de Vesta se origina a una profundidad de ~20 km.
- El material del sur expuesto se origina a 60-100 km de profundidad.
- La ausencia de olivino significativo sugiere que los ~ 100 km exteriores son principalmente corteza ígnea.
Conclusiones:
- El límite de la corteza y el manto (Moho) del asteroide 4 Vesta tiene una profundidad de más de 80 km.
- Las capas exteriores de Vesta están compuestas predominantemente por una corteza ígnea.
- Los eventos de impacto proporcionan datos cruciales para comprender el interior de los asteroides.
Videos de Conceptos Relacionados
Magnetostatic Boundary Conditions
1.9K
An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
1.9K
Acceleration due to Gravity on Other Planets
3.4K
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...
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...
3.4K
Schwarzschild Radius and Event Horizon
2.2K
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...
2.2K
Kepler's First Law of Planetary Motion
4.8K
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,...
4.8K
Elastic Collisions: Case Study
16.9K
Elastic collision of a system demands conservation of both momentum and kinetic energy. To solve problems involving one-dimensional elastic collisions between two objects, the equations for conservation of momentum and conservation of internal kinetic energy can be used. For the two objects, the sum of momentum before the collision equals the total momentum after the collision. An elastic collision conserves internal kinetic energy, and so the sum of kinetic energies before the collision equals...
16.9K
Kepler's Third Law of Planetary Motion
3.6K
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...
3.6K

