We have received the abstract of your presentation; your abstract has a running identifier of 871. Please refer to this number in all communication regarding your abstract.
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.
If you have questions, please contact abs-help@aas.org.
Meeting registration is a separate process from abstract submission. Please remember to register.
Your abstract information has been assembled into a LaTeX file, and that is what appears below. You may save this screen in any of several ways (cut-and-paste or the "Save As" button, for instance) so that you can keep a record of your submission.
If you want to try formatting this LaTeX version, you will need a copy of the AASTeX style file for abstracts. That style file is available from http://www.aas.org/publications/baas/aasab.sty.
\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} \sponsor{David H. Cohen} \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}