{ "id": "2104.03263", "version": "v1", "published": "2021-04-07T17:09:41.000Z", "updated": "2021-04-07T17:09:41.000Z", "title": "Analytical Solutions for Radiation-Driven Winds in Massive Stars II: The $δ$-slow Regime", "authors": [ "I. Araya", "A. Christen", "M. Curé", "L. S. Cidale", "R. O. J. Venero", "C. Arcos", "A. C. Gormaz-Matamala", "M. Haucke", "P. Escárate", "H. Clavería" ], "comment": "8 pages, 1 figure, accepted for publication in MNRAS", "categories": [ "astro-ph.SR" ], "abstract": "Accurate mass-loss rates and terminal velocities from massive stars winds are essential to obtain synthetic spectra from radiative transfer calculations and to determine the evolutionary path of massive stars. From a theoretical point of view, analytical expressions for the wind parameters and velocity profile would have many advantages over numerical calculations that solve the complex non-linear set of hydrodynamic equations. In a previous work, we obtained an analytical description for the fast wind regime. Now, we propose an approximate expression for the line-force in terms of new parameters and obtain a velocity profile closed-form solution (in terms of the Lambert $W$ function) for the $\\delta$-slow regime. Using this analytical velocity profile, we were able to obtain the mass-loss rates based on the m-CAK theory. Moreover, we established a relation between this new set of line-force parameters with the known stellar and m-CAK line-force parameters. To this purpose, we calculated a grid of numerical hydrodynamical models and performed a multivariate multiple regression. The numerical and our descriptions lead to good agreement between their values.", "revisions": [ { "version": "v1", "updated": "2021-04-07T17:09:41.000Z" } ], "analyses": { "keywords": [ "massive stars", "slow regime", "radiation-driven winds", "analytical solutions", "fast wind regime" ], "note": { "typesetting": "TeX", "pages": 8, "language": "en", "license": "arXiv", "status": "editable" } } }