The ionization structure of early-B supergiant winds

Content Provider	Semantic Scholar
Author	Prinja, Raman K. Massa, D. M. G. Searle, S.
Copyright Year	1996
Abstract	We present empirically determined ionization conditions f or the winds of 106 luminous B0 to B5 stars observed by IUE. The UV wind lines are modelled to extract products of mass-l o rates times ionization fractions ( Ṁ qi(w), wherew = v/v∞) for N , C , Si , Si , Al  and C. We describe the general behaviour of the Ṁ qi(w) and their ratios, demonstrating that the wind ionizationincreases with distance from the star, contrary to recent findings for O star winds. Using empirical mass-loss rates (from H α observations) and model prescriptions, we derive mean qi(w) values integrated over the wind, 〈qi〉. These〈qi〉 are quite small, never exceeding 15% for Al  or 2% for Si. This is surprising, since the 〈qi〉 for these ions clearly peak within the observed spectral range. We conclude that th e low 〈qi〉 arise because the 〈Ṁ qi〉 are underestimated by the wind models, which assume that the outflows are smooth when they ar e, in fact, highly structured.
File Format	PDF HTM / HTML
Alternate Webpage(s)	http://arxiv.org/pdf/astro-ph/0412315v1.pdf
Alternate Webpage(s)	http://cds.cern.ch/record/810900/files/0412315.pdf
Language	English
Access Restriction	Open
Subject Keyword	Environmental Wind GUCY2C protein, human Ions Luminous Studio Stars, Celestial Stellar classification hearing impairment
Content Type	Text
Resource Type	Article