Clumping in the winds of O-type CSPNs
M.A. Urbaneja, R.-P. Kudritzki, J. Puls
TL;DR
This paper investigates the inhomogeneous, clumped stellar winds of O-type CSPNs using multi-wavelength observations, aiming to understand wind structures and derive clumping factors through optical and UV spectral analysis.
Contribution
It presents preliminary multi-wavelength results on the wind clumping properties of Galactic O-type CSPNs, highlighting the use of optical and UV lines for clumping diagnostics.
Findings
Evidence of wind clumping in CSPNs from spectral line analysis
Derivation of clumping factors using optical and UV lines
Comparison with massive O-type star winds
Abstract
Recent studies of massive O-type stars present clear evidences of inhomogeneous and clumped winds. O-type (H-rich) central stars of planetary nebulae (CSPNs) are in some ways the low mass-low luminosity analogous of those massive stars. In this contribution, we present preliminary results of our on-going multi-wavelength (FUV, UV and optical) study of the winds of Galactic CSPNs. Particular emphasis will be given to the clumping factors derived by means of optical lines (Halpha and HeII4686) and "classic" FUV (and UV) lines.
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Taxonomy
TopicsDrilling and Well Engineering