Computer Science
Scientific paper
Nov 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mshe.work...69a&link_type=abstract
"Proceedings of "Massive Stars and High-Energy Emission in OB Associations", a workshop of the JENAM 2005, "Distant Worlds", hel
Computer Science
3
Scientific paper
We analyse the XMM-Newton observations of the close massive (O5V((f)) + O9.5V) FO 15 binary system. X-ray spectra are described by a combination of absorption models wabs (NH, ISM) and absori (NH, wind) with two absorbed thermal (apec) models (kT1 = 0.22 ± 0.01 and kT2 = 1.43 ± 0.40 keV) plus a non-thermal Power-Law (po) model (Γ = 1.50 ± 0.46). Observed emission lines from high ionization states of N, O, Ca, Si, Ne and Fe are produced by thermal plasma temperatures according to those obtained from our X-ray spectral fit model. The hard thermal component comes from the colliding wind region (CWR) of the primary stellar wind onto the secondary surface. We find Lx/Lbol is about 9.0×10-7 in excess with respect to the relation of single O-type stars, likely due to the CWR of the system. We estimate that CWR gas reaches the radiative limit, and mostly emits absorbed soft X-ray photons, while hard X-ray photons come from the inner part of the CWR throughout Inverse Compton (IC) scattering processes. Finally, we confirm the existence of short-term variability which seems to be related to radiative gas at the outer zones of the CWR, since the variability is only present in the soft X-ray band, while the hard X-ray emission remains constant.
Albacete Colombo Juan Facundo
Micela Giuseppina
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