Large Scale Star Formation: Molecular Clouds and Massive Stars

Details Large Scale Star Formation: Molecular Clouds and Massive Stars Large Scale Star Formation: Molecular Clouds and Massive Stars

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993rmxaa..26...13f&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 26, 13

Astronomy and Astrophysics

Astronomy

3

Scientific paper

RESUMEN Se describen las principales ideas sobre la formaci6n de grandes nubes interestelares y sobre el papel que juegan las estrellas masivas en el ciclo de formaci6n estelar. Las nubes masivas se pueden formar mediante inestabilidades a gran escala o mediante perturbaciones fuertes en un disco gaseoso con esfuerzos cortantes. La energia inyectada por las estrellas recien formadas puede destruir a sus nubes maternas y la actividad de formaci6n estelar result a ser autolimitada. El mecanismo ma's eficiente para destruir a las nubes es debido a la fotoionizaci6n de las estrellas masivas. El numero maximo de estrellas OB que se pueden formar en las regiones densas de las nubes moleculares es del orden de 10 por cada 10 M0 de gas. Suponiendo un factor de llenado de 0.1 para estas regiones densas, la eficiencia de formaci6n estelar en los complejos moleculares es del 5%. Una vez que las nubes son dispersadas, el efecto combinado de los vientos estelares y las explosiones de supernova de las asociaciones OB generan grandes burbujas en expansi6n. Estas remanentes de multi-supernovas son responsables de mantener la estructura del gas interestelar y de controlar Ia actividad de formaci6n estelar en galaxias aisladas. ABSTRACT The main ideas for the formation of large interstellar cloud complexes and the role of massive stars in the sta formation cycle are reviewed. Massive cloud complexes can be formed via large scale instabilities or by the action of strong perturbations evolving in a sheared disk. The energy injected by new stars can destroy their parental clouds and, hence, the star forming activity in these clouds is self-limited. The most efficient cloud destruction mechanism is due to photoionization from massive stars, which limits the population of massive stars. The maximum number of OB stars that can form within a dense molecular cloud fragment is of order 10 per 10 M0. Assuming a filling factor of 0.1 for these dense fragments, the resulting star forming efficiency within cloud complexes is roughly 5%. Once the parent cloud is dispersed, the combined action of stellar winds and supernova explosions from OB associations generate large expanding bubbles. These multisupernova remnants are responsible for the bulk properties of the general interstellar gas, and can control the overall star forming activity in isolated galaxies. Key words: ISM - CLOUDS ISM - SUPERNOVA REMNANTS - STARS - FORMATION

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