Volume 644, December 2020
|Number of page(s)||1|
|Published online||24 November 2020|
Radiography in high mass X-ray binaries
Micro-structure of the stellar wind through variability of the column density (Corrigendum)
Centre for mathematical Plasma Astrophysics, Department of Mathematics,
KU Leuven, Celestijnenlaan 200B,
2 Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
3 Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
4 NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA
Key words: stars: mass-loss / stars: massive / stars: winds, outflows / X-rays: binaries / radiative transfer / errata, addenda
Equation (14) for the duration d of an eclipse with respect to the orbital period P is wrong. If we assume a spherical donor star of radius R and a circular orbit of the compact object around the donor star with orbital separation a, the right formula is: (1)
where i is the orbital inclination (i = 90° for an edge-on configuration). We retrieve the condition R < acosi to have an eclipse of the X-ray point source by the donor star. This equation did not directly intervene in the other computations performed in the paper so it does not change the conclusions, neither qualitatively nor quantitatively.
© ESO 2020
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