scholarly journals CONSTRAINTS ON POROSITY AND MASS LOSS IN O-STAR WINDS FROM THE MODELING OF X-RAY EMISSION LINE PROFILE SHAPES

2013 ◽  
Vol 770 (1) ◽  
pp. 80 ◽  
Author(s):  
Maurice A. Leutenegger ◽  
David H. Cohen ◽  
Jon O. Sundqvist ◽  
Stanley P. Owocki
Keyword(s):  
Mass Loss ◽  
Emission Line ◽  
Line Profile ◽  
X Ray ◽  
Emission Line Profile

ERRATUM: “CONSTRAINTS ON POROSITY AND MASS LOSS IN O-STAR WINDS FROM MODELING OF X-RAY EMISSION LINE PROFILE SHAPES” (2013, ApJ, 770, 80)

2013 ◽  
Vol 777 (1) ◽  
pp. 81
Author(s):  
Maurice A. Leutenegger ◽  
David H. Cohen ◽  
Jon O. Sundqvist ◽  
Stanley P. Owocki
Keyword(s):  
Mass Loss ◽  
Emission Line ◽  
Line Profile ◽  
X Ray ◽  
Emission Line Profile

scholarly journals X-ray spectroscopy of massive stellar winds: previous and ongoing observations of the hot star ζ Pup

2018 ◽  
Vol 14 (S346) ◽  
pp. 88-92
Author(s):  
N. Miller ◽  
W. Waldron ◽  
J. Nichols ◽  
D. Huenemoerder ◽  
M. Dahmer ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Stellar Wind ◽  
Galactic Evolution ◽  
Stellar Winds ◽  
Hot Stars ◽  
X Ray ◽  
Wind Structure ◽  
Important Impact ◽  
Emission Line Profile

AbstractThe 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.

scholarly journals X-ray emission line profile modeling of hot stars

2003 ◽  
Vol 74 (3) ◽  
pp. 1966-1968 ◽  
Author(s):  
Roban H. Kramer ◽  
Stephanie K. Tonnesen ◽  
David H. Cohen ◽  
Stanley P. Owocki ◽  
Asif ud-Doula ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Hot Stars ◽  
X Ray ◽  
Emission Line Profile ◽  
Profile Modeling

Anomalous Hα Emission Line Profile Detected at the Center of DDO 53

2021 ◽  
Vol 919 (2) ◽  
pp. 73
Author(s):  
Justin A. Kader ◽  
Liese van Zee ◽  
Kristen B. W. McQuinn ◽  
Laura C. Hunter
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Hα Emission ◽  
Emission Line Profile

scholarly journals Simultaneous Spectroscopy and Polarimetry of Be Stars

1987 ◽  
Vol 92 ◽  
pp. 84-86
Author(s):  
D. R. Gies ◽  
David McDavid
Keyword(s):  
Mass Loss ◽  
Emission Line ◽  
Absorption Line ◽  
Line Profile ◽  
Circumstellar Envelope ◽  
Be Stars ◽  
Line Profiles ◽  
Initial Attempt ◽  
Rapid Variability ◽  
Hα Emission

Evidence is now accumulating that many Be stars display photospheric line profile variations on timescales of days or less that are probably caused by nonradial pulsations (Baade 1984; Penrod 1986). In some circumstances these pulsations can promote mass loss into the circumstellar envelope, and consequently the conditions in the inner part of the envelope may vary on similar timescales. Changes in the envelope could produce variations in the polarization and emission line profiles, and observers have reported rapid variability in both. We describe here an initial attempt to search for simultaneous variations in continuum polarization, Hα emission, and the He I λ6678 photospheric absorption line in order to investigate correlated changes on short timescales.

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