acceleration of particles; radiation mechanisms: non-thermal; gamma- rays: stars; X-rays: stars; Astrophysics - High Energy Astrophysical Phenomena
Abstract :
[en] We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ˜18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, f[SUB]NT,e[/SUB] < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as B[SUB]WCR[/SUB] > 0.3 G. We also argue a putative interpretation of the emission from which we estimate f[SUB]NT,e[/SUB] ≍ 0.006 and B[SUB]WCR[/SUB] ≍ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.
Research Center/Unit :
STAR - Space sciences, Technologies and Astrophysics Research - ULiège
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
del Palacio, S.; Instituto Argentino de Radioastronomía (CONICET ; CICPBA), C.C. No 5, 1894 Villa Elisa, Argentina
García, F.; Kapteyn Astronomical Institute, University of Groningen, PO BOX 800, NL-9700 AV Groningen, the Netherlands
Altamirano, D.; School of Physics and Astronomy, University of Southampton Highfield Campus, Southampton SO17 1PS, UK
Barbá, R. H.; Departamento de Astronomía, Universidad de La Serena, Av. Juan Cisternas 1200 Norte, La Serena, Chile
Bosch-Ramon, V.; Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E-08028 Barcelona, Spain
Corcoran, M.; CRESST II and X-ray Astrophysics Laboratory NASA/GSFC, Greenbelt, MD 20771, USA ; Institute for Astrophysics and Computational Sciences, Department of Physics, The Catholic University of America, Washington, DC 20064, USA
De Becker, Michaël ; Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Origines Cosmologiques et Astrophysiques (OrCa)
Hamaguchi, K.; CRESST II and X-ray Astrophysics Laboratory NASA/GSFC, Greenbelt, MD 20771, USA ; Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
Maíz Apellániz, J.; Centro de Astrobiología, CSIC-INTA, Campus ESAC. C. Bajo del Castillo s/n, E-28 692 Villanueva de la Cañada, Madrid, Spain
Munar Adrover, P.; Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E-08028 Barcelona, Spain
Paredes, J. M.; Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E-08028 Barcelona, Spain
Romero, G. E.; Instituto Argentino de Radioastronomía (CONICET ; CICPBA), C.C. No 5, 1894 Villa Elisa, Argentina
Sana, H.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
Tavani, M.; INAF-IAPS, via del Fosso del Cavaliere 100, I-00133 Roma, Italy ; Dip. di Fisica, Univ. di Roma 'Tor Vergata', via della Ricerca Scientifica 1, I-00133 Roma, Italy
ud-Doula, A.; Department of Physics, Penn State Scranton, 120 Ridge View Drive, Dunmore, PA 18512, USA)
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