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Videos de Conceptos Relacionados

Atomic Structure01:33

Atomic Structure

All matter is composed of atoms, the smallest individual units of elements. Each atom is made up of three subatomic particles: protons, neutrons, and electrons. Together, these three particles account for the mass and the charge of an atom.The History of Atomic TheoryThe first person to propose that everything on Earth is made up of tiny particles was the Greek philosopher Democritus, around 450 B.C. He used the term atomos, Greek for “indivisible,” from which the modern term “atom” is derived.
Atomic Orbitals02:44

Atomic Orbitals

An atomic orbital represents the three-dimensional regions in an atom where an electron has the highest probability to reside. The radial distribution function indicates the total probability of finding an electron within the thin shell at a distance r from the nucleus. The atomic orbitals have distinct shapes which are determined by l, the angular momentum quantum number. The orbitals are often drawn with a boundary surface, enclosing densest regions of the cloud.
Nuclear Stability03:18

Nuclear Stability

Protons and neutrons, collectively called nucleons, are packed together tightly in a nucleus. With a radius of about 10−15 meters, a nucleus is quite small compared to the radius of the entire atom, which is about 10−10 meters. Nuclei are extremely dense compared to bulk matter, averaging 1.8 × 1014 grams per cubic centimeter. If the earth’s density were equal to the average nuclear density, the earth’s radius would be only about 200 meters.
To hold positively charged protons together in the...
Nuclear Fission02:50

Nuclear Fission

Many heavier elements with smaller binding energies per nucleon can decompose into more stable elements that have intermediate mass numbers and larger binding energies per nucleon—that is, mass numbers and binding energies per nucleon that are closer to the “peak” of the binding energy graph near 56. Sometimes neutrons are also produced. This decomposition of a large nucleus into smaller pieces is called fission. The breaking is rather random with the formation of a large number of different...
Nuclear Fusion02:45

Nuclear Fusion

The process of converting very light nuclei into heavier nuclei is also accompanied by the conversion of mass into large amounts of energy, a process called fusion. The principal source of energy in the sun is a net fusion reaction in which four hydrogen nuclei fuse and ultimately produce one helium nucleus and two positrons.
A helium nucleus has a mass that is 0.7% less than that of four hydrogen nuclei; this lost mass is converted into energy during the fusion. This reaction produces about...
Atomic Structure01:17

Atomic Structure

The Greek philosopher Democritus proposed that everything on Earth is made up of tiny particles called atomos, Greek for "indivisible," from which the modern term "atom" is derived. In the 19th century, John Dalton proposed the atomic theory that is still largely correct today. He put forth five postulates to explain how atoms made up the world around us. (1) All matter is composed of infinitely small particles or atoms. (2) All atoms of a given element are identical to one another and (3) are...

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Video Experimental Relacionado

Updated: Jul 19, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
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Simulation of the Planetary Interior Differentiation Processes in the Laboratory

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Formación de estrellas aisladas: desde la formación de nubes hasta el colapso del núcleo.

Derek Ward-Thompson1

  • 1Department of Physics and Astronomy, Cardiff University, Post Office Box 913, Cardiff, UK. D.Ward-Thompson@astro.cf.ac.uk

Science (New York, N.Y.)
|January 5, 2002
PubMed
Resumen

La formación de estrellas es un problema fundamental de la astrofísica. Los modelos actuales luchan por explicar las observaciones de la turbulencia y los campos magnéticos en las regiones de formación estelar, a pesar de la tecnología avanzada y el poder computacional.

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Área de la Ciencia:

  • La astrofísica es la astrofísica.
  • Formación Estelar Formación Estelar.
  • Física cósmica La física cósmica es la física cósmica.

Sus antecedentes:

  • La formación estelar es un problema astrofísico fundamental, crucial para comprender la evolución de la galaxia y el sistema solar.
  • Los procesos físicos clave involucran medios turbulentos y parcialmente ionizados con campos magnéticos no uniformes.
  • El debate en curso se centra en los tiempos de desintegración de la turbulencia y la interacción de los campos magnéticos y la turbulencia.

Objetivo del estudio:

  • Para investigar los complejos procesos físicos que rigen la formación de estrellas.
  • Para conciliar los modelos teóricos con los datos de observación con respecto a la turbulencia y los campos magnéticos.
  • Para avanzar en nuestra comprensión de las escalas de tiempo y los mecanismos en la evolución estelar.

Principales métodos:

  • Utilizando datos avanzados de observación de cámaras de ondas milimétricas para analizar perfiles de temperatura y densidad.
  • Realizar cálculos estadísticos sobre la vida útil de los objetos en colapso y pre-colapso.
  • Desarrollar modelos computacionales complejos que incorporen efectos magnéticos y turbulentos.

Principales resultados:

  • Los avances tecnológicos permiten la observación detallada de las regiones de formación estelar.
  • El aumento de la potencia de cómputo facilita un modelado más sofisticado de los procesos físicos.
  • Ningún modelo actual reproduce con precisión todos los fenómenos observados.

Conclusiones:

  • La formación de estrellas sigue siendo un desafío complejo en la astrofísica.
  • Los modelos actuales son insuficientes para explicar completamente los procesos de formación estelar observados.
  • Se necesita más investigación para integrar los campos magnéticos, la turbulencia y los datos de observación de manera efectiva.