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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 Transmutation03:20

Nuclear Transmutation

Nuclear transmutation is the conversion of one nuclide into another. It can occur by the radioactive decay of a nucleus, or the reaction of a nucleus with another particle. The first manmade nucleus was produced in Ernest Rutherford’s laboratory in 1919 by a transmutation reaction, the bombardment of one type of nuclei with other nuclei or with neutrons. Rutherford bombarded nitrogen-14 atoms with high-speed α particles from a natural radioactive isotope of radium and observed protons being...
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 Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
Atomic Nuclei: Larmor Precession Frequency01:11

Atomic Nuclei: Larmor Precession Frequency

The earth's gravitational field produces a 'twisting force' perpendicular to the angular momentum of a spinning mass (such as a spinning top) that causes the mass to 'wobble' around the gravitational field axis in a phenomenon called precession. Similarly, the magnetic moment (μ) of a spinning nucleus precesses due to an external magnetic field directed along the z-axis. The precession of the magnetic moment vector about the magnetic field is called Larmor precession, and the angular frequency...

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Video Experimental Relacionado

Updated: Jul 11, 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

¿Cuándo se verá un púlsar en la supernova 1987a?

F C Michel, C F Kennel, W A Fowler

    Science (New York, N.Y.)
    |November 13, 1987
    PubMed
    Resumen

    Los investigadores exploraron la detección de púlsares dentro de la supernova 1987A. Un púlsar es un pulsar.

    Área de la Ciencia:

    • La astrofísica es la astrofísica.
    • Restos de supernovas de las supernovas.
    • Las estrellas de neutrones son estrellas de neutrones.

    Sus antecedentes:

    • La supernova 1987A (SN 1987A) es un objeto clave para el estudio de la evolución estelar y los mecanismos de explosión.
    • Las supernovas de tipo II exhiben curvas de luz con una desintegración más lenta que la radioactiva, cuya causa se debate.

    Objetivo del estudio:

    • Para investigar la posible detección de un púlsar dentro del remanente de la supernova 1987A.
    • Proponer una nueva hipótesis que vincule el decaimiento de la curva de luz observada con la actividad del púlsar y la opacidad de la nebulosa.

    Principales métodos:

    • Análisis de las características de la curva de luz de las supernovas de tipo II, específicamente SN 1987A.
    • Modelado teórico de la transferencia de energía de un púlsar incrustado a través de un remanente dinámico de supernova.

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    Principales resultados:

    • El lento decaimiento observado en las curvas de luz de Tipo II puede no representar el spin-down del púlsar, sino más bien una disminución de la opacidad nebular.
    • Esta opacidad decreciente permitiría que el aumento de la energía de rayos gamma escapara al remanente.

    Conclusiones:

    • La hipótesis sugiere que la energía "falta" en la curva de luz de SN 1987A podría ser observable como rayos gamma que escapan.
    • Probar esto requiere buscar estos rayos gamma, lo que proporciona un nuevo método para la detección de púlsares en restos de supernovas.