TY - CONF

T1 - Chaos and its regularization in the stellar wind

AU - Kholtygin, Alexander F.

PY - 2012/1/1

Y1 - 2012/1/1

N2 - It is well known that the power stellar wind of OB and Wolf-Rayet (WR) stars consist of the numerous dense inhomogenuities (clumps) and more rarefied homogeneous interclump medium. Clumps are randomly distributed in the whole volume of stellar wind and have arbitrary sizes and fluxes. Formation of the clumps appears to be the chaotic process connected with internal instability of the radiation dominated stellar wind. Our modelling of the line profiles in spectra of OB and WR stars with clumped wind show that initially chaotic ensemble of the clumps can be regularized. As a result of that regularization the clusters of clumps which manifest themselves as strong bumps on the line profiles cam be developed.

AB - It is well known that the power stellar wind of OB and Wolf-Rayet (WR) stars consist of the numerous dense inhomogenuities (clumps) and more rarefied homogeneous interclump medium. Clumps are randomly distributed in the whole volume of stellar wind and have arbitrary sizes and fluxes. Formation of the clumps appears to be the chaotic process connected with internal instability of the radiation dominated stellar wind. Our modelling of the line profiles in spectra of OB and WR stars with clumped wind show that initially chaotic ensemble of the clumps can be regularized. As a result of that regularization the clusters of clumps which manifest themselves as strong bumps on the line profiles cam be developed.

KW - Chaos

KW - Clumps

KW - Regularization

KW - Stellar wind

UR - http://www.scopus.com/inward/record.url?scp=85072407397&partnerID=8YFLogxK

M3 - Paper

SP - 233

EP - 242

T2 - 5th International Conference on Chaotic Modeling and Simulation, CHAOS 2012

Y2 - 12 June 2012 through 15 June 2012

ER -