KRTIČKA, Jiří. Wind mass-loss rates in main-sequence B stars. In G. Mathys, E. Griffin, O. Kochukhov, R. Monier, G. Wahlgren. Putting A Stars into Context: Evolution, Environment, and Related Stars. Moskva, Rusko: Pero, 2014, s. 250-255. ISBN 978-5-00086-273-5. |
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@inproceedings{1229865, author = {Krtička, Jiří}, address = {Moskva, Rusko}, booktitle = {Putting A Stars into Context: Evolution, Environment, and Related Stars}, editor = {G. Mathys, E. Griffin, O. Kochukhov, R. Monier, G. Wahlgren}, keywords = {mass-loss; hot stars}, howpublished = {tištěná verze "print"}, language = {eng}, location = {Moskva, Rusko}, isbn = {978-5-00086-273-5}, pages = {250-255}, publisher = {Pero}, title = {Wind mass-loss rates in main-sequence B stars}, url = {http://adsabs.harvard.edu/abs/2014psce.conf..250K}, year = {2014} }
TY - JOUR ID - 1229865 AU - Krtička, Jiří PY - 2014 TI - Wind mass-loss rates in main-sequence B stars PB - Pero CY - Moskva, Rusko SN - 9785000862735 KW - mass-loss KW - hot stars UR - http://adsabs.harvard.edu/abs/2014psce.conf..250K N2 - We calculate wind mass-loss rates in main-sequence B stars. The calculations are based on our radiatively-driven NLTE wind models. The main sequence mass-loss rate depends strongly on effective temperature. For the hottest B stars the mass-loss rate amounts to 1e-9 Mo/yr, while for the coolest ones it is lower by three orders of magnitude. Main sequence B stars with effective temperatures lower than about 15 000 K (i.e., later than spectral type B5) do not have a homogeneous line-driven wind. The wind mass-loss rate also strongly depends on the chemical composition; it may either increase or decrease with increasing abundances, depending on whether the emergent flux redistribution is significant or not. ER -
KRTIČKA, Jiří. Wind mass-loss rates in main-sequence B stars. In G. Mathys, E. Griffin, O. Kochukhov, R. Monier, G. Wahlgren. \textit{Putting A Stars into Context: Evolution, Environment, and Related Stars}. Moskva, Rusko: Pero, 2014, s.~250-255. ISBN~978-5-00086-273-5.
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