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Kepler's First Law of Planetary Motion01:10

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 Motion01:29

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 Motion01:18

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...
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

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 velocity with the...
Detection of Black Holes01:10

Detection of Black Holes

Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Gravitation Between Spherically Symmetric Masses01:14

Gravitation Between Spherically Symmetric Masses

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.

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Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
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Un disco de polvo compacto y caliente alrededor de un objeto estelar joven y masivo.

Stefan Kraus1, Karl-Heinz Hofmann, Karl M Menten

  • 1Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, Michigan 48103, USA. stefankr@umich.edu

Nature
|July 16, 2010
PubMed
Resumen

Los astrónomos observaron un disco compacto y polvoriento alrededor de una estrella joven masiva, lo que proporciona evidencia del modelo de disco de acreción en la formación de estrellas masivas. Este hallazgo desafía las teorías anteriores que sugerían vías de formación alternativas para estrellas de más de 10 masas solares.

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Área de la Ciencia:

  • La astrofísica es la astrofísica.
  • Evolución Estelar Evolución Estelar
  • Formación Estelar Formación Estelar.

Sus antecedentes:

  • Los discos circumestelares son la clave para la formación de estrellas de baja masa.
  • El papel de los discos de acreción en la formación de estrellas >10 masas solares se debate debido a la presión de la radiación.
  • Las teorías alternativas incluyen la fusión estelar o complejas geometrías de caída.

Objetivo del estudio:

  • Para investigar el modo de formación de las estrellas masivas.
  • Para buscar evidencia observacional de discos de acreción alrededor de objetos estelares jóvenes masivos.
  • Para probar la aplicabilidad del paradigma del disco de acreción a la formación de estrellas de alta masa.

Principales métodos:

  • Se utilizaron observaciones interferométricas en el infrarrojo cercano.
  • Resolvió espacialmente la distribución de material caliente alrededor de un objeto estelar joven de alta masa (~20 masas solares).
  • Aplicó modelos geométricos y físicos para analizar la estructura del disco y el gradiente de temperatura.

Principales resultados:

  • Se resolvió una estructura de disco compacta y polvorienta (13 x 19 UA) alrededor del masivo objeto estelar joven.
  • El disco mostró un gradiente de temperatura radial con una región interna libre de polvo (<9,5 UA).
  • Se detectó un flujo de salida bipolar con golpes de arco perpendicular al plano del disco.

Conclusiones:

  • La estructura observada es consistente con un disco visto en una inclinación de 45 grados.
  • Las propiedades del disco son similares a las que se encuentran en la formación estelar de baja masa.
  • Los hallazgos apoyan el modelo de disco de acreción para la formación de estrellas masivas.