{ "id": "0912.4209", "version": "v2", "published": "2009-12-21T16:52:34.000Z", "updated": "2010-01-27T11:20:36.000Z", "title": "Mass fluxes for hot stars", "authors": [ "L. B. Lucy" ], "comment": "Accepted by A&A; 6 pages, 5 figures; minor changes from v1", "categories": [ "astro-ph.SR" ], "abstract": "In an attempt to understand the extraordinarily small mass-loss rates of late-type O dwarfs, mass fluxes in the relevant part of (T_{eff}, g)-space are derived from first principles using a previously-described code for constructing moving reversing layers. From these mass fluxes, a weak-wind domain is identified within which a star's rate of mass loss by a radiatively-driven wind is less than that due to nuclear burning. The five weak-wind stars recently analysed by Marcolino et al. (2009) fall within or at the edge of this domain. But although the theoretical mass fluxes for these stars are ~ 1.4 dex lower than those derived with the formula of Vink et al. (2000), the observed rates are still not matched, a failure that may reflect our poor understanding of low-density supersonic outflows. Mass fluxes are also computed for two strong-wind O4 stars analysed by Bouret et al. (2005). The predictions agree with the sharply reduced mass loss rates found when Bouret et al. take wind clumping into account.", "revisions": [ { "version": "v2", "updated": "2010-01-27T11:20:36.000Z" } ], "analyses": { "keywords": [ "hot stars", "low-density supersonic outflows", "strong-wind o4 stars", "sharply reduced mass loss rates", "extraordinarily small mass-loss rates" ], "tags": [ "journal article" ], "publication": { "doi": "10.1051/0004-6361/200913400", "journal": "Astronomy and Astrophysics", "year": 2010, "month": "Mar", "volume": 512 }, "note": { "typesetting": "TeX", "pages": 6, "language": "en", "license": "arXiv", "status": "editable", "inspire": 840899, "adsabs": "2010A&A...512A..33L" } } }