stars: early-type; stars: mass loss; stars: winds; outflows; X-rays: stars
Abstract :
[en] The stellar winds of hot stars have an important impact on both stellar and galactic evolution, yet their structure and internal processes are not fully understood in detail. One of the best nearby laboratories for studying such massive stellar winds is the O4I(n)fp star ζ Pup. After briefly discussing existing X-ray observations from Chandra and XMM, we present a simulation of X-ray emission line profile measurements for the upcoming 840 kilosecond Chandra HETGS observation. This simulation indicates that the increased S/N of this new observation will allow several major steps forward in the understanding of massive stellar winds. By measuring X-ray emission line strengths and profiles, we should be able to differentiate between various stellar wind models and map the entire wind structure in temperature and density. This legacy X-ray spectrum of ζ Pup will be a useful benchmark for future X-ray missions.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Miller, Nathan; Department of Physics & Astronomy, University of Wisconsin-Eau Claire, 105 Garfield Avenue, Eau Claire, WI 54701, USA
Waldron, Wayne; Eureka Scientific, Inc., USA
Nichols, Joy; Harvard-Smithsonian Center for Astrophysics, USA
Huenemoerder, David; Massachusetts Institute of Technology, USA
Dahmer, Matthew; Northrop Grumman, USA
Ignace, Richard; East Tennessee State University, USA
Lauer, Jennifer; Harvard-Smithsonian Center for Astrophysics, USA
Moffat, Anthony; University of Montreal, Canada
Nazé, Yaël ; Université de Liège - ULiège > Groupe d'astrophysique des hautes énergies (GAPHE)
Oskinova, Lidia; University of Potsdam, Germany
Richardson, Noël; University of Toledo, USA
Ramiaramanantsoa, Tahina; Arizona State University, USA
