Article (Scientific journals)
Ultraviolet line profiles of slowly rotating massive star winds using the 'analytic dynamical magnetosphere' formalism
Erba, C.; David-Uraz, A.; Petit, V. et al.
2021In Monthly Notices of the Royal Astronomical Society, 506, p. 5373-5388
Peer Reviewed verified by ORBi
 

Files


Full Text
2106.13676.pdf
Author preprint (1.4 MB)
Download

All documents in ORBi are protected by a user license.

Send to



Details



Keywords :
line: profiles; radiative transfer; stars: magnetic field; stars: massive; stars: winds; outflows; ultraviolet: stars; Astrophysics - Solar and Stellar Astrophysics
Abstract :
[en] Recent large-scale spectropolarimetric surveys have established that a small but significant percentage of massive stars host stable, surface dipolar magnetic fields with strengths on the order of kG. These fields channel the dense, radiatively driven stellar wind into circumstellar magnetospheres, whose density and velocity structure can be probed using ultraviolet (UV) spectroscopy of wind-sensitive resonance lines. Coupled with appropriate magnetosphere models, UV spectroscopy provides a valuable way to investigate the wind-field interaction, and can yield quantitative estimates of the wind parameters of magnetic massive stars. We report a systematic investigation of the formation of UV resonance lines in slowly rotating magnetic massive stars with dynamical magnetospheres. We pair the analytic dynamical magnetosphere (ADM) formalism with a simplified radiative transfer technique to produce synthetic UV line profiles. Using a grid of models, we examine the effect of magnetosphere size, the line strength parameter, and the cooling parameter on the structure and modulation of the line profile. We find that magnetic massive stars uniquely exhibit redshifted absorption at most viewing angles and magnetosphere sizes, and that significant changes to the shape and variation of the line profile with varying line strengths can be explained by examining the individual wind components described in the ADM formalism. Finally, we show that the cooling parameter has a negligible effect on the line profiles.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Erba, C.;  Department of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE 19716, USA
David-Uraz, A.;  Department of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE 19716, USA ; Department of Physics and Astronomy, Howard University, Washington, DC 20059, USA ; Center for Research and Exploration in Space Science and Technology, and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA
Petit, V.;  Department of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE 19716, USA
Hennicker, L.;  Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
Fletcher, C.;  Science and Technology Institute, Universities Space Research Association, Huntsville, AL 35805, USA
Fullerton, A. W.;  Space Telescope Science Institute, Baltimore, MD 21218, USA
Nazé, Yaël  ;  Université de Liège - ULiège > Groupe d'astrophysique des hautes énergies (GAPHE)
Sundqvist, J.;  Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
ud-Doula, A.;  Department of Physics, Penn State Scranton, 120 Ridge View Drive, Dunmore, PA 18512, USA)
Language :
English
Title :
Ultraviolet line profiles of slowly rotating massive star winds using the 'analytic dynamical magnetosphere' formalism
Publication date :
01 October 2021
Journal title :
Monthly Notices of the Royal Astronomical Society
ISSN :
0035-8711
eISSN :
1365-2966
Publisher :
Oxford University Press, Oxford, United Kingdom
Volume :
506
Pages :
5373-5388
Peer reviewed :
Peer Reviewed verified by ORBi
Available on ORBi :
since 18 August 2021

Statistics


Number of views
36 (2 by ULiège)
Number of downloads
32 (2 by ULiège)

Scopus citations®
 
10
Scopus citations®
without self-citations
2
OpenCitations
 
3

Bibliography


Similar publications



Contact ORBi