{ "id": "1403.5601", "version": "v1", "published": "2014-03-22T02:02:41.000Z", "updated": "2014-03-22T02:02:41.000Z", "title": "CIR Modulation of the X-ray Flux from the O7.5 III(n)((f)) Star xi Persei?", "authors": [ "D. Massa", "L. Oskinova", "A. W. Fullerton", "R. K. Prinja", "D. A. Bohlender", "N. D. Morrison", "M. Blake", "W. Pych" ], "comment": "Accepted by MNRAS. 9 pages, 9 figures", "categories": [ "astro-ph.SR" ], "abstract": "We analyze a 162 ks HETG Chandra observation of the O7.5 III(n)((f)) star xi Per, together with contemporaneous H alpha observations. The X-ray spectrum of this star is similar to other single O stars, and not pathological in any way. Its UV wind lines are known to display cyclical time variability, with a period of 2.086 days, which is thought to be associated with co-rotating interaction regions (CIRs). We examine the Chandra and H alpha data for variability on this time scale. We find that the X-rays vary by about 15% over the course of the observations and that this variability is out of phase with variable absorption on the blue wing of the H alpha profiles (assumed to be a surrogate for the UV absorption associated with CIRs). While not conclusive, both sets of data are consistent with models where the CIRs are either a source of X-rays or modulate them.", "revisions": [ { "version": "v1", "updated": "2014-03-22T02:02:41.000Z" } ], "analyses": { "keywords": [ "star xi persei", "x-ray flux", "cir modulation", "ks hetg chandra observation", "uv wind lines" ], "tags": [ "journal article" ], "publication": { "doi": "10.1093/mnras/stu565", "journal": "Monthly Notices of the Royal Astronomical Society", "year": 2014, "month": "Jul", "volume": 441, "number": 3, "pages": 2173 }, "note": { "typesetting": "TeX", "pages": 9, "language": "en", "license": "arXiv", "status": "editable", "adsabs": "2014MNRAS.441.2173M" } } }