Massive Stars and the Energy Balance of the Interstellar Medium. I. The Impact of an Isolated 60 M☉ Star
By T. Freyer, Gerhard Hensler, H. Yorke. 2003
174 citations recorded by the source corpus.
We present results of numerical simulations carried out with a two-dimensional radiation hydrodynamics code in order to study the impact of massive stars on their surrounding interstellar medium. This first paper deals with the evolution of the circumstellar gas around an isolated 60 M☉ star. The interaction of the photoionized H II region with the stellar wind bubble forms a variety of interesting structures like shells, clouds, fingers, and spokes. These results demonstrate that complex structures found in H II regions are not necessarily relics from the time before the gas became ionized but may result from dynamical processes during the course of the H II region evolution. We have also analyzed the transfer and deposit of the stellar wind and radiation energy into the circumstellar medium until the star explodes as a supernova. Although the total mechanical wind energy supplied by the star is negligible compared to the accumulated energy of the Lyman continuum photons, the kinetic energy imparted to the circumstellar gas over the star's lifetime is 4 times higher than for a comparable windless simulation. Furthermore, the thermal energy of warm photoionized gas is lower by some 55%. Our results document the necessity to consider both ionizing radiation and stellar winds for an appropriate description of the interaction of OB stars with their circumstellar environment.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/86598725235f324f659502f8f1a7a4482e191947
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In Astronomy and Astrophysics
Citations in the corpus
- The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, background): “These photons do not couple efficiently with the surroundingISM (Freyer et al. 2006).”
- The Bubbling Galactic Disk. II. The Inner 20° (2007, background): “Recent numerical models of wind-blown bubbles around stars of mass 35, 60, and 85 M by Freyer et al. (2003, 2006) and Kröger et al. (2006, 2008) confirm the general picture of windblown bubbles predicted by the analytic models noted above, but show that the detailed structure can be considerably…”
- A gallery of bubbles. The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material (2010, background): “Capriotti & Kozminski (2001) and Freyer et al. (2003, 2006) developed analytical models and hydrodynamical simulations of H ii regions, including stellar winds.”
- Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, background): “(Freyer et al. 2006) found that stellar photons do not couple efficiently with the surrounding ISM.”
- Hierarchical formation of bulgeless galaxies – II. Redistribution of angular momentum via galactic fountains (2011, background): “The dynamical effect of this feedback is negligible, as is the overall coupling of energy to the ISM, but high mass star radiation feedback does reduce star formation in the region immediately surrounding a recently formed star particle (full details of this radiative feedback will be presented in a”
- MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, background): “This is the result of the inhomogeneous ISM, with pockets of hot gas building pressure and driving outflows.”
- Before the first supernova: combined effects of H II regions and winds on molecular clouds (2014, unknown): “Freyer et al. (2003) and Freyer et al. (2006) performed detailed 2D hydrodynamic simulations of the growth of wind bubbles inside HIIRs expanding into a smooth medium.”
- Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters (2006, unknown): “…the interstellar medium at the time of the globular cluster formationwas much more dense and thus the matter ejected was slowed down by the bow shock between the ejecta and the ambient medium as shown for instance in the numerical models by Freyer et al. 2003 (see also Garcia-Segura et al. 1996).”