Poster abstract details
X-ray spectra from hot wind-driven bubbles with chemical gradients
Abstract
The first high-resolution X-ray spectroscopy of a planetary nebula, viz. BD+30$^\circ$\,3639 (Yu et al. 2009), opens the possibility to study plasma conditions and chemical compositions of X-ray emitting regions of PNe in much greater detail than before.
This prompted us to develop a model for typical wind-blown bubbles with realistic temperature and density profiles according to thermal conduction theory. The X-ray emission of these bubble models is computed by means of the well-documented CHIANTI code and allows to quickly perform detailed parameter studies without the need for dedicated hydrodynamical simulations. We report first results on how the X-ray spectra depend on chemical composition (hydrogen-rich vs. hydrogen-poor) and how temperature and abundance determinations reflect temperature gradients as well as chemical gradients and mixtures within the bubbles.
This prompted us to develop a model for typical wind-blown bubbles with realistic temperature and density profiles according to thermal conduction theory. The X-ray emission of these bubble models is computed by means of the well-documented CHIANTI code and allows to quickly perform detailed parameter studies without the need for dedicated hydrodynamical simulations. We report first results on how the X-ray spectra depend on chemical composition (hydrogen-rich vs. hydrogen-poor) and how temperature and abundance determinations reflect temperature gradients as well as chemical gradients and mixtures within the bubbles.