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Grandes variaciones de metalicidad en el medio interestelar galáctico

Annalisa De Cia1, Edward B Jenkins2, Andrew J Fox3

  • 1Department of Astronomy, University of Geneva, Versoix, Switzerland. annalisa.decia@unige.ch.

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|September 9, 2021
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Resumen

El medio interestelar (ISM) muestra variaciones significativas de metalicidad, con mediciones corregidas por polvo que revelan menores abundancias de lo que se suponía anteriormente. Esto sugiere que el gas que se acumula de las nubes de alta velocidad no se mezcla bien con el disco galáctico.

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Área de la Ciencia:

  • Astronomía y astrofísica
  • Cosmoquímica

Sus antecedentes:

  • El medio interestelar (ISM) está compuesto de varios componentes de gas y polvo.
  • La metalicidad en el disco galáctico a menudo se supone que es uniforme en los modelos de evolución química.
  • El agotamiento del polvo complica las mediciones precisas de la metalicidad gaseosa.

Objetivo del estudio:

  • Para determinar la metalicidad corregida por el polvo del ISM neutro.
  • Investigar el alcance de las variaciones de metalicidad en el ISM local.
  • Comprender el impacto del gas de acreción en la homogeneidad química del ISM.

Principales métodos:

  • Se utilizó la espectroscopia de la línea de absorción ultravioleta para medir las abundancias químicas del ISM.
  • Se han aplicado técnicas de corrección del polvo para tener en cuenta los metales incorporados en los granos sólidos.
  • Analizaron datos de 25 estrellas en la Vía Láctea.

Principales resultados:

  • Se han reportado variaciones significativas de metalicidad en el MIS neutro, que abarcan un factor de diez.
  • Se encontró una metalicidad media de 55 ± 7% de metalicidad solar con una desviación estándar de 0,28 dex.
  • Regiones observadas con una metalicidad solar tan baja como del 17%, lo que indica una inhomogeneidad significativa.

Conclusiones:

  • El ISM exhibe inhomogeneidades químicas sustanciales, que desafían las suposiciones de un disco de gas bien mezclado y metálico solar.
  • La acreción de gas prístino a través de nubes de alta velocidad es una causa probable de estas variaciones de metalicidad observadas.
  • La mezcla ineficiente de gas de acreción de baja metalicidad puede explicar las desviaciones de metalicidad en estrellas contemporáneas.