Physical and Spectral Properties of Model Self-Enriched H II Regions

Details Physical and Spectral Properties of Model Self-Enriched H II Regions Physical and Spectral Properties of Model Self-Enriched H II Regions

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9214n&link_type=abstract

American Astronomical Society, AAS Meeting #211, #92.14; Bulletin of the American Astronomical Society, Vol. 39, p.889

Astronomy and Astrophysics

Astronomy

Scientific paper

We report on the physical and spectral properties predicted for 1D evolved and self-enriched H II regions (HIIRs), which are 1) trapped within the supershells produced by the evolution of their ionizing clusters, and 2) fully mixed with the ejecta from embedded massive (M/Msun>8) stars. The ionizing clusters have Mcluster=10^4 Msun, metallicity Z=solar, solar/5 or solar/20, and age 10 Myr. At this age, the least massive O star in each ionizing cluster has just undergone a type II supernova (SNII). In addition, at this age, B stars capable of ionizing H I are still present. The stellar ejecta was uniformly distributed between the HIIR and the superbubble blown by the cluster. The radius of the expanding supershell was computed as prescribed by Mac Low & McCray (1988) for an adiabatic, pressure-driven shell, with continuous mechanical energy injection from SNe. Our goals are 1) to obtain upper limits to the amount of self-enrichment of HIIRs with age 10 Myr, and 2) to determine if this self-enrichment would be observable in the visible. Our preliminary results are the following. (1) At age 10 Myr, HIIRs fail to form at high density (n[H]=10^3 cm^-3) and/or at low Z. (2) Due to the large superbubble volumes, the metal abundance enhancements caused by stellar evolution in the HIIRs are negligible. (3) In evolved HIIRs, the line intensities of [O III]5007 and [O II]3727 are less than or equal to 10^-7 and 10^-1 of Hbeta, respectively. (4) Given the above conditions, self-enrichment in metals of HIIRs would be difficult to observe. This research is supported by NSF grant AST 03-07118 to the University of Oklahoma.

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