Jove
Visualize
Contáctanos
JoVE
x logofacebook logolinkedin logoyoutube logo
ACERCA DE JoVE
Visión GeneralLiderazgoBlogCentro de Ayuda JoVE
AUTORES
Proceso de PublicaciónConsejo EditorialAlcance y PolíticasRevisión por ParesPreguntas FrecuentesEnviar
BIBLIOTECARIOS
TestimoniosSuscripcionesAccesoRecursosConsejo Asesor de BibliotecasPreguntas Frecuentes
INVESTIGACIÓN
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchivo
EDUCACIÓN
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualCentro de Recursos para ProfesoresSitio de Profesores
Términos y Condiciones de Uso
Política de Privacidad
Políticas

Videos de Conceptos Relacionados

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...
Shock Waves01:16

Shock Waves

While deriving the Doppler formula for the observed frequency of a sound wave, it is assumed that the speed of sound in the medium is greater than the source's speed through it. When this condition is breached, a shock wave occurs.
When the source's speed approaches the speed of sound, constructive interference between successive wavefronts emitted by the source occurs immediately behind it. Initially, scientists believed that this constructive interference would result in such high pressures...
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...
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...
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...

También podría leer

Artículos Relacionados

Artículos vinculados a este trabajo por autores compartidos, revista y gráfico de citas.

Ordenar por
Same author

DebrisWatch II: Digging Deeper for Geosynchronous Debris.

The journal of the astronautical sciences·2026
Same author

Palladium-catalyzed asymmetric carbofluorination of <i>gem</i>-difluorostyrenes with cesium fluoride and allylic acetates.

Chemical communications (Cambridge, England)·2026
Same author

Motivation biases behavior but not perception.

Communications psychology·2026
Same author

Reeler mice show impaired performance in a texture-based novelty recognition task.

Physiology & behavior·2026
Same author

Creation of a psychiatric intensive care unit as a model for violence reduction.

General hospital psychiatry·2026
Same author

Whisking Behaviour Reveals Stronger Evidence of Habituation in Homozygous Reeler Mice Compared to Controls.

Genes, brain, and behavior·2026

Video Experimental Relacionado

Updated: Jul 4, 2026

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses
11:20

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses

Published on: July 2, 2012

El estallido de choque de supernova de una supergigante roja.

Kevin Schawinski1, Stephen Justham, Christian Wolf

  • 1Department of Physics, University of Oxford, Oxford OX1 3RH, UK. kevins@astro.ox.ac.uk

Science (New York, N.Y.)
|June 17, 2008
PubMed
Resumen

Se observaron estrellas masivas que explotaron como supernovas antes de que su impacto llegara a la superficie. Esta detección temprana de supernovas de colapso de núcleo proporciona información sobre el interior estelar y la física de la explosión.

Más Videos Relacionados

Evaluating Primary Blast Effects In Vitro
10:51

Evaluating Primary Blast Effects In Vitro

Published on: September 18, 2017

Videos de Experimentos Relacionados

Last Updated: Jul 4, 2026

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses
11:20

Investigation of Early Plasma Evolution Induced by Ultrashort Laser Pulses

Published on: July 2, 2012

Evaluating Primary Blast Effects In Vitro
10:51

Evaluating Primary Blast Effects In Vitro

Published on: September 18, 2017

Área de la Ciencia:

  • La astronomía y la astrofísica.
  • Evolución Estelar Evolución Estelar
  • Física de las Supernovas Física de las Supernovas

Sus antecedentes:

  • Las estrellas masivas terminan sus vidas en supernovas de colapso de núcleo.
  • Estas explosiones cósmicas son típicamente detectadas días después del evento.
  • Comprender los progenitores de las supernovas es crucial para la astrofísica.

Objetivo del estudio:

  • Para observar y analizar las primeras etapas de una supernova de colapso de núcleo.
  • Para investigar la emisión radiativa precursora antes de que se produzca el choque.
  • Para confirmar el tipo progenitor de la supernova observada.

Principales métodos:

  • Utilizando el telescopio espacial Galaxy Evolution Explorer (GALEX) para las observaciones.
  • El análisis de la curva de luz ultravioleta de la supernova SNLS-04D2dc.c.
  • El empleo de modelos teóricos para interpretar los datos de observación.

Principales resultados:

  • Detectó un precursor radiativo del choque de la supernova antes de la ruptura de la superficie.
  • Observaron la expansión inicial de la estrella progenitora durante la explosión.
  • Confirmó que la estrella progenitora era una supergigante roja a través del modelado teórico.

Conclusiones:

  • La detección temprana de las supernovas es posible mediante la observación de precursores radiativos.
  • Este método permite sondear la física de las supernovas de colapso de núcleo.
  • Proporciona información sobre la estructura interna de los progenitores de las supergigantes rojas.