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  Exploring the connection between the stellar wind and the non-thermal emission in LS 5039

Bosch-Ramon, V., Motch, C., Ribo, M., Lopes de Oliveria, R., Janot-Pacheco, E., Negueruela, I., et al. (2007). Exploring the connection between the stellar wind and the non-thermal emission in LS 5039. Astronomy & Astrophysics, 473(2), 545-550.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0011-7BF6-A Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0011-7BF7-8
Genre: Journal Article

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Bosch-Ramon, Valenti1, Author              
Motch, Christian2, Author
Ribo, Marc2, Author
Lopes de Oliveria, Raimundo2, Author
Janot-Pacheco, Eduardo2, Author
Negueruela, Ignacio2, Author
Paredes, Josep M.2, Author
Martocchia, Andrea2, Author
Affiliations:
1Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society, ou_904550              
2Observatoire Astronomique, rue de l'Université 11, Strasbourg 67000, France Departament d'Astronomia i Meteorologia, Universitat de Barcelona, c/Martí i Franquès 1, 08028 Barcelona, Catalonia, Spain Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciéncias Atmosféricas - IAG, Departamento de Astronomia, Rua do Matao, 1226 - 05508-900 São Paulo, Brazil Dpto. de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante, Apdo. 99, 03080 Alicante, Spain Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere 100, 00133 Roma, Italy, ou_persistent22              

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 Abstract: LS 5039 has been observed with several X-ray instruments so far. The source presents X-ray variability at orbital timescales in flux and photon index. The system harbors an O-type main sequence star with moderate mass loss. At present, the link between the X-rays and the stellar wind is unclear. New XMM-Newton observations have been performed around periastron and apastron passages in September 2005, when the stellar wind activity was apparently higher. April 2005 Chandra observations on LS 5039 are also revisited. Moreover, a compilation of Halpha EW data obtained since 1992, from which the stellar mass loss evolution can be approximately inferred, is carried out. XMM-Newton observations show higher and harder emission around apastron than around periastron. No signatures of thermal emission or a reflection iron line indicating the presence of an accretion disk are found in the spectrum, and the hydrogen column density (NH) is compatible with being the same in both observations and consistent with the interstellar value. 2005 Chandra observations show a hard X-ray spectrum, and possibly high fluxes. The Halpha EW shows yearly variations of a ~ 10%, and does not seem to be correlated with X-ray fluxes obtained at similar phases, unlike it would be expected in the wind accretion scenario. 2005 XMM-Newton and Chandra observations are consistent with 2003 RXTE/PCA results. The constancy of the NH seems to imply that either the X-ray emitter is located at >~ 1012 cm from the compact object, or the real N_H is 3-27 times smaller than the one predicted by a spherical symmetric wind model. We suggest that the multiwavelength non-thermal emission of LS 5039 is related to the radio jets and unlikely produced inside the binary system.

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Language(s): eng - English
 Dates: 2007-10
 Publication Status: Published in print
 Pages: -
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 Rev. Method: Peer
 Identifiers: eDoc: 317879
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Title: Astronomy & Astrophysics
  Alternative Title : A&A
Source Genre: Journal
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Pages: - Volume / Issue: 473 (2) Sequence Number: - Start / End Page: 545 - 550 Identifier: -