Reference : A Changing Wind Collision
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
A Changing Wind Collision
Nazé, Yaël mailto [Université de Liège - ULiège > > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Koenigsberger, Gloria [Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Ave. Universidad S/N, Cuernavaca, 62210, Morelos, México]
Pittard, Julian M. [School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK]
Parkin, Elliot Ross [Groupe d’Astrophysique des Hautes Energies, STAR, Université de Liège, Quartier Agora (B5c, Institut d’Astrophysique et de Géophysique), Allée du 6 Août 19c, B-4000 Sart Tilman, Liège, Belgium]
Rauw, Grégor mailto [Université de Liège - ULiège > > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Corcoran, Michael F. [CRESST and X-ray Astrophysics Laboratory, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA ; The Catholic University of America, 620 Michigan Avenue NE, Washington, DC 20064, USA <ID system="ORCID">0000-0002-7762-3172</ID>]
Hillier, D. John [Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT PACC), University of Pittsburgh, Pittsburgh, PA 15260, USA)]
Astrophysical Journal
IOP Publishing
ID 164 (11p)
Yes (verified by ORBi)
United Kingdom
[en] stars: binaries: eclipsing ; stars: early-type ; stars: winds ; outflows ; stars: Wolf–Rayet ; X-rays: stars
[en] We report on the first detection of a global change in the X-ray emitting properties of a wind–wind collision, thanks to XMM-Newton observations of the massive Small Magellenic Cloud (SMC) system HD 5980. While its light curve had remained unchanged between 2000 and 2005, the X-ray flux has now increased by a factor of ∼2.5, and slightly hardened. The new observations also extend the observational coverage over the entire orbit, pinpointing the light-curve shape. It has not varied much despite the large overall brightening, and a tight correlation of fluxes with orbital separation is found without any hysteresis effect. Moreover, the absence of eclipses and of absorption effects related to orientation suggests a large size for the X-ray emitting region. Simple analytical models of the wind–wind collision, considering the varying wind properties of the eruptive component in HD 5980, are able to reproduce the recent hardening and the flux-separation relationship, at least qualitatively, but they predict a hardening at apastron and little change in mean flux, contrary to observations. The brightness change could then possibly be related to a recently theorized phenomenon linked to the varying strength of thin-shell instabilities in shocked wind regions. Based on XMM-Newton and Chandra data.
Researchers ; Professionals

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