# AAS 207th Meeting Abstract Submission

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We are pleased to invite you to attend the AAS 207th Meeting of the American Astronomical Society, January 8, 2006 in Washington, DC. Unless there is a problem with your submission, the next email you receive will be when the complete AAS 207th Meeting program is available online.

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\documentstyle[11pt,aasab]{article}
\nofiles
\meetingid{AAS207}
\identifier{871}
\datesubmitted{2005-10-19 12:10:31}
\lastname{Grizzard}
\firstname{Kevin}
\memberid{14349}
\authoremail{Kevin.Grizzard@sjca.edu}
\authorphone{(610) 328-8587}
\correspondentaddress{St. John's College, 60 College Ave., Annapolis MD 21401}
\presentationtype{3}
\sortcategory{5}

\begin{document}
\title{Wind Signatures in the X-ray Emission Line Profiles of the O Supergiant zeta Orionis}
\authorsurname{Grizzard}
\authorgivenname{K.}
\authoraffil{St. John's College}
\authorsurname{Cohen}
\authorgivenname{D. H.}
\authoraffil{Swarthmore College}
\authorsurname{Leutenegger}
\authorgivenname{M. A.}
\authoraffil{Columbia University}
\authorsurname{Reed}
\authorgivenname{C.}
\authoraffil{Swarthmore College}
\authorsurname{Kramer}
\authorgivenname{R. H.}
\authoraffil{Columbia University}
\authorsurname{Owocki}
\authorgivenname{S. P.}
\authoraffil{University of Delaware}

\begin{abstract}
The profiles of X-ray emission lines from several hot stars
are resolved by the Chandra grating spectrometers. These
profile shapes provide information about the kinematics of
the hot plasma around these stars and, via signatures of
continuum attenuation, also provide information about the
overlying cold stellar wind. We present a quantitative
analysis of roughly one dozen emission lines in the Chandra
HETGS spectrum of zeta Ori (O 9.7 Ib), and analyze the
results in the context of the line-force instability shock
model. The distribution in velocity space of the emission,
along with the separate helium-like line ratio results, are
consistent with the wind-shock scenario. But, although there
is statistically significant evidence for some wind
attenuation, the degree of wind attenuation is a factor of
five to ten less than what would be expected in the context
of a smooth, spherically symmetric wind and the UV-derived
wind mass-loss rate. These results are consistent with those
derived from the X-ray emission line profiles of the hotter
O star, zeta Pup, and also with recent, independent evidence
from UV spectroscopy, that O star mass-loss rates have been
overestimated.

We acknowledge support from NASA contract NAS8-03060 and
from the National Science Foundation, through their REU
program at the Keck Northeast Astronomy Consortium, via
contract AST-0353997.
\end{abstract}
\end{document}