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Revealing the Accelerating Wind in the Inner Region of Colliding-wind Binary WR 112

  • Authors: John D. Monnier, Yinuo Han, Michael F. Corcoran, Sanne Bloot, Joseph R. Callingham, William Danchi, Philip G. Edwards, Lincoln Greenhill, Kenji Hamaguchi, Matthew J. Hankins, Ryan Lau, Jon M. Miller, Anthony F. J. Moffat, Garreth Ruane, Christopher M. P. Russell, Anthony Soulain, Samaporn Tinyanont, Peter Tuthill, Jason J. Wang, Peredur M. Williams

John D. Monnier et al 2025 The Astronomical Journal 170 .

  • Provider: AAS Journals

Caption: Figure 4.

The summed Chandra/ACIS X-ray spectrum of WR 112. The data are binned for visual clarity. The best-fit two-temperature plasma model is shown in red (tbabs×vapec+vapec). The kT = 0.5 keV and kT = 2 keV components are shown in cyan and blue, respectively. The strongest lines in the model are He-like Si XIII, S XVI, Ar XVII, and Fe XXV (1.87, 2.46, 3.14, and 6.70 keV, respectively). The spectrum is obscured at low energy by the high line-of-sight column density. See Table 3 for model parameters and errors.

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