TY  - JOUR
A1  - Oskinova, Lida
A1  - Kubatova, Brankica
A1  - Hamann, Wolf-Rainer
T1  - Moving inhomogeneous envelopes of stars
JF  - Transport in Porous Media
N2  - Massive stars are extremely luminous and drive strong winds, blowing a large part of their matter into the galactic environment before they finally explode as a supernova. Quantitative knowledge of massive star feedback is required to understand our Universe as we see it. Traditionally, massive stars have been studied under the assumption that their winds are homogeneous and stationary, largely relying on the Sobolev approximation. However, Observations with the newest instruments, together with progress in model calculations, ultimately dictate a cardinal change of this paradigm: stellar winds are highly inhomogeneous. Hence, we are now advancing to a new stage in our understanding of stellar winds. Using the foundations laid by V.V. Sobolev and his school, we now update and further develop the stellar spectral analysis techniques. New sophisticated 3-D models of radiation transfer in inhomogeneous expanding media elucidate the physics of stellar winds and improve classical empiric mass-loss rate diagnostics. Applications of these new techniques to multiwavelength observations of massive stars yield consistent and robust stellar wind parameters. (C) 2016 Elsevier Ltd. All rights reserved.
KW  - Stars: mass-loss
KW  - Stars: winds
KW  - Outflows
KW  - Stars: atmospheres early type
Y1  - 2016
U6  - https://doi.org/10.1016/j.jqsrt.2016.06.017
SN  - 0022-4073
SN  - 1879-1352
VL  - 183
SP  - 100
EP  - 112
PB  - Elsevier
CY  - Oxford
ER  -