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Nuclear Transmutation03:20

Nuclear Transmutation

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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...
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Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

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In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
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Nuclear Fusion02:45

Nuclear Fusion

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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...
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Atomic Nuclei: Magnetic Resonance01:05

Atomic Nuclei: Magnetic Resonance

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The number of nuclear spins aligned in the lower energy state is slightly greater than those in the higher energy state. In the presence of an external magnetic field, as the spins precess at the Larmor frequency, the excess population results in a net magnetization oriented along the z axis. When a pulse or a short burst of radio waves at the Larmor frequency is applied along the x axis, the coupling of frequencies causes resonance and flips the nuclear spins of the excess population from the...
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Magnetism01:30

Magnetism

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Magnets are commonly found in everyday objects, such as toys, hangers, elevators, doorbells, and computer devices. Experimentation on these magnets shows that all magnets have two poles: one is labeled north (N) and the other south (S). Magnetic poles repel if they are alike and attract if unlike. Moreover, both poles of a magnet attract unmagnetized pieces of iron.
An individual magnetic pole cannot be isolated. No matter how small, every piece of a magnet contains a north pole and a south...
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Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

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An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
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High-Temperature and High-Pressure In situ Magic Angle Spinning Nuclear Magnetic Resonance Spectroscopy
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r-Elementos de proceso de las hipernovas magnetorotativas

D Yong1,2, C Kobayashi3,4, G S Da Costa5,3

  • 1Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australian Capital Territory, Australia. david.yong@anu.edu.au.

Nature
|July 8, 2021
PubMed
Resumen
Este resumen es generado por máquina.

Las hipernovas magnetorotativas, no solo las fusiones de estrellas de neutrones, probablemente crearon elementos pesados en el universo temprano. El estudio de las estrellas primitivas revela estas fábricas de elementos cósmicos cruciales y su conexión con las explosiones de rayos gamma.

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Área de la Ciencia:

  • Astronomía y astrofísica
  • La astrofísica nuclear
  • Cosmoquímica

Sus antecedentes:

  • Las fusiones de estrellas de neutrones son sitios confirmados para la producción de elementos de captura rápida de neutrones (proceso r).
  • Los modelos de evolución química galáctica muestran que las fusiones de estrellas de neutrones por sí solas no pueden explicar la abundancia observada de elementos en estrellas pobres en metales.
  • Las estrellas químicamente primitivas en el halo de la Vía Láctea conservan las primeras firmas nucleosintéticas, ofreciendo pistas de sitios de proceso r desconocidos.

Objetivo del estudio:

  • Investigar posibles sitios alternativos para el proceso de nucleosíntesis.
  • Para analizar el patrón de abundancia de elementos de la estrella extremadamente pobre en metales SMSS J200322.54-114203.
  • Para comparar las abundancias observadas con los rendimientos teóricos de diferentes eventos astrofísicos.

Principales métodos:

  • Análisis espectroscópico de la estrella extremadamente pobre en metales SMSS J200322.54-114203.
  • Medición de los patrones de abundancia de elementos, centrándose en los elementos del proceso r.
  • Comparación de los patrones de abundancia observados con los rendimientos nucleosintéticos de un modelo de hipernova magnetorotativa de 25 masas solares.

Principales resultados:

  • La estrella SMSS J200322.54-114203.3 exhibe una mejora significativa de los elementos del proceso r a una metalicidad muy baja.
  • El patrón de abundancia de elementos observado coincide estrechamente con los rendimientos predichos de una sola hipernova magnetorotativa de 25 masas solares.
  • Este modelo de hipernova explica la producción de elementos de proceso r, luz y pico de hierro.

Conclusiones:

  • Las hipernovas magnetorotativas son un sitio viable y significativo para la nucleosíntesis del proceso r en el universo temprano.
  • Estas hipernovas podrían explicar los patrones de abundancia observados en las estrellas pobres en metales, resolviendo las limitaciones de los modelos de fusión de estrellas de neutrones.
  • La asociación de las hipernovas con explosiones de rayos gamma de larga duración sugiere que estos eventos explosivos fueron importantes en el enriquecimiento químico galáctico temprano.