Modeling the emission of an H II region containing a bubble-like structure

Abstract

The influence of a bubble-like structure around a starburst within the H II regions on the shape of the ionizing spectrum and the generation of the observed emission lines was studied using multicomponent photoionization modeling. The distributions of density and other physical parameters in such bubble-like structures were determined by Weaver et al. in 1977. The first two components represent the region of the stellar wind from the central starburst region. The gas density and electron temperature distributions in these components were described by the solution of the system of equations of continuity and energy transfer with account for the heat conductivity. The third component represents a thin layer of gas with a high density that emerges due to the passage of a normal shock wave of the stellar wind. The fourth component represents a “typical” H II region. The ionizing radiation spectra were set from the calculated evolutionary models whose free parameters determine the physical conditions within the “bubble.” The influence of the stellar wind bubble on the shape of the ionizing radiation spectrum and the generation of fluxes in important emission lines was analyzed.

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Correspondence to I. O. Koshmak.

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Original Russian Text © I.O. Koshmak, B.Ya. Melekh, 2013, published in Kinematika i Fizika Nebesnykh Tel, 2013, Vol. 29, No. 6, pp. 3–19.

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Koshmak, I.O., Melekh, B.Y. Modeling the emission of an H II region containing a bubble-like structure. Kinemat. Phys. Celest. Bodies 29, 257–268 (2013). https://doi.org/10.3103/S0884591313060020

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Keywords

  • Celestial Body
  • Stellar Wind
  • Fourth Component
  • Diagnostic Ratio
  • Normal Shock Wave