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X-ray Observations of Bow Shocks around Runaway O Stars. The case of $\zeta$ Oph and BD+43$^{\circ}$3654
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abstract
Non-thermal radiation has been predicted within bow shocks around runaway stars by recent theoretical works. We present X-ray observations towards the runaway stars $\zeta$ Oph (Chandra and Suzaku) and BD+43$^{\circ}$3654 (XMM-Newton) to search for the presence of non-thermal X-ray emission. We found no evidence of non-thermal emission spatially coincident with the bow shocks, nonetheless, diffuse emission is detected in the vicinity of $\zeta$ Oph. After a careful analysis of its spectral characteristics we conclude that this emission has a thermal nature with a plasma temperature of $T \approx 2 \times10^{6}$ K. The cometary shape of this emission seems to be in line with recent predictions of radiation-hydrodynamic models of runaway stars. The case of BD+43$^{\circ}$3654 is puzzling as non-thermal emission has been reported in a previous work for this source.
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Cited by 2 Pith papers
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An Halpha survey of infrared bow-shocks around OB-type stars
Fifteen plus one serendipitous clear H-alpha bow shocks are detected among 78 IR candidates; several are consistent with radiation-supported regimes while others match classical wind-supported shocks.
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Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry
Bulk interstellar gas motion, not stellar motion, dominates most massive star bow shocks; only about 21% are classical aligned bow shocks.
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