Volume 550, February 2013
|Number of page(s)||4|
|Section||Stellar structure and evolution|
|Published online||04 February 2013|
Is the bowshock of the runaway massive star HD 195592 a Fermi source?
1 Instituto Argentino de Radioastronomía, C.C.5, (1894) Villa Elisa, Buenos Aires, Argentina
2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque, 1900 La Plata, Argentina
3 Institut d’Astrophysique et de Géophysique, Université de Liège, 17 Allée du 6 Août, B5c, 4000 Sart Tilman, Belgium
Received: 26 July 2012
Accepted: 7 December 2012
Context. HD 195592 is an O-type super-giant star, known as a well-established runaway. Recently, a Fermi γ-ray source (2FGL J2030.7+4417) with a position compatible with that of HD 195592 has been reported.
Aims. Our goal is to explore the scenario where HD 195592 is the counterpart of the Fermi γ-ray source, modeling the non-thermal emission produced in the bowshock of the runaway star.
Methods. We calculated the spectral energy distribution of the radiation produced in the bowshock of HD 195592 and we compared it with Fermi observations of the 2FGL J2030.7+4417.
Results. We present relativistic particle losses and the resulting radiation of the bowshock of HD 195592 and show that the latter is compatible with the detected γ-ray emission.
Conclusions. We conclude that the Fermi source 2FGL J2030.7+4417 might be produced, under some energetic assumptions, by inverse Compton up-scattering of photons from the heated dust in the bowshock of the runaway star. Therefore, HD 195592 might be the very first object detected belonging to the category of γ-ray emitting runaway massive stars, whose existence has been recently predicted.
Key words: stars: early-type / gamma-rays: general / radiation mechanisms: non-thermal / stars individual: HD 195592
© ESO, 2013
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