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Videos de Conceptos Relacionados

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...
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...
Emission Spectra02:39

Emission Spectra

When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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...
Atomic Emission Spectroscopy: Overview01:20

Atomic Emission Spectroscopy: Overview

Atomic emission spectroscopy (AES) is an analytical technique used to determine the elemental composition of a sample by analyzing the light emitted from excited atoms. In AES, atoms in a sample are excited to higher energy levels by thermal energy from high-temperature sources, such as plasma, arcs, or sparks. When these excited atoms return to lower energy states, they emit light at specific wavelengths characteristic of each element. The resulting atomic emission spectrum, which consists of...

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Video Experimental Relacionado

Updated: May 26, 2026

Flame Experiments at the Advanced Light Source: New Insights into Soot Formation Processes
10:04

Flame Experiments at the Advanced Light Source: New Insights into Soot Formation Processes

Published on: May 26, 2014

Supernova SN 2011fe de una estrella enana blanca de carbono y oxígeno en explosión.

Peter E Nugent1, Mark Sullivan, S Bradley Cenko

  • 1Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA. penugent@lbl.gov

Nature
|December 16, 2011
PubMed
Resumen

Los astrónomos observaron la supernova SN 2011fe, probablemente una estrella enana blanca explotando. Las primeras observaciones sugieren que su compañera era una estrella de secuencia principal, aclarando los misterios del progenitor de la supernova.

Videos de Experimentos Relacionados

Last Updated: May 26, 2026

Flame Experiments at the Advanced Light Source: New Insights into Soot Formation Processes
10:04

Flame Experiments at the Advanced Light Source: New Insights into Soot Formation Processes

Published on: May 26, 2014

Área de la Ciencia:

  • La astronomía y la astrofísica.
  • Cosmología Cosmología.

Sus antecedentes:

  • Las supernovas de tipo Ia son "velas estándar" cruciales para medir la expansión cósmica.
  • La naturaleza exacta de los sistemas progenitoras de supernovas de tipo Ia sigue siendo en gran medida desconocida.
  • Las observaciones anteriores carecían de proximidad para identificar estrellas progenitoras antes de la explosión.

Objetivo del estudio:

  • Para investigar el sistema progenitor de la supernova SN 2011fe.
  • Para obtener información sobre el mecanismo de explosión de las supernovas de tipo Ia.

Principales métodos:

  • Las primeras observaciones de la supernova SN 2011fe en la galaxia M101 (6.4 Mpc).
  • Análisis espectroscópico de las primeras emisiones de supernovas.
  • Utilizando imágenes previas a la explosión (en un documento complementario).

Principales resultados:

  • La estrella que explotó fue identificada como una enana blanca de carbono-oxígeno.
  • La falta de un choque temprano sugiere una estrella compañera de la secuencia principal.
  • La espectroscopia reveló oxígeno de alta velocidad y una mezcla extensa de elementos.

Conclusiones:

  • SN 2011fe proporciona datos observacionales cruciales sobre los progenitores de supernovas de tipo Ia.
  • Los hallazgos apoyan el modelo binario de estrella de secuencia principal enana blanca para las supernovas de tipo Ia.
  • Este estudio avanza en nuestra comprensión de las explosiones estelares y la aceleración cósmica.