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Reliquias de baja masa de la formación estelar temprana

R Schneider¹, A Ferrara, R Salvaterra

¹Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy.

|April 25, 2003

Resumen

Las primeras estrellas se formaron sin metales, favoreciendo a las estrellas masivas. Sin embargo, el polvo en el gas de muy baja metalicidad permitió la formación de las estrellas de menor masa de hoy.

Área de la Ciencia:

La astronomía es la astronomía.
Cosmología Cosmología.
La astrofísica es la astrofísica.

Sus antecedentes:

Las primeras estrellas, formadas después del Big Bang, influyeron significativamente en las generaciones estelares posteriores.
Investigaciones anteriores sugirieron que las estrellas masivas (hasta 100 masas solares) se formaron en condiciones libres de metales, mientras que las estrellas de baja masa requerían algún enriquecimiento de metales.

Objetivo del estudio:

Para investigar el papel del polvo en la formación de estrellas de baja masa en el Universo temprano.
Para entender la metalicidad mínima requerida para la formación de las estrellas observables de baja masa.

Principales métodos:

Análisis de la estrella más pobre en hierro conocida.
Investigar la presencia y el impacto del polvo en el gas de baja metalicidad.

Principales resultados:

La estrella más pobre en hierro indica la presencia de polvo incluso en metales muy bajos.
Este polvo es crucial para enfriar el gas, permitiendo la fragmentación de las nubes moleculares.
La fragmentación conduce a la formación de estrellas de segunda generación de menor masa.

Conclusiones:

El polvo, no solo los metales, juega un papel crítico en la formación temprana de estrellas.
La presencia de polvo facilita la formación de estrellas de baja masa que pueden sobrevivir hasta nuestros días.

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