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@inproceedings{1374140,
author = {Kurfürst, Petr and Feldmeier, Achim and Krtička, Jiří},
address = {San Francisco, USA},
booktitle = {The B[e] Phenomenom: Forty Years of Studies},
edition = {508},
editor = {Anatoly Miroshnichenko, Sergey Zharikov, Daniela Korčáková, Marek Wolf},
keywords = {dense disks or rings; viscous heating; neutral hydrogen layers},
howpublished = {elektronická verze "online"},
language = {eng},
location = {San Francisco, USA},
isbn = {978-1-58381-900-5},
pages = {17-22},
publisher = {Astronomical Society of the Pacific},
title = {Modeling sgB[e] Circumstellar Disks},
year = {2017}
}
TY - JOUR
ID - 1374140
AU - Kurfürst, Petr - Feldmeier, Achim - Krtička, Jiří
PY - 2017
TI - Modeling sgB[e] Circumstellar Disks
PB - Astronomical Society of the Pacific
CY - San Francisco, USA
SN - 9781583819005
KW - dense disks or rings
KW - viscous heating
KW - neutral hydrogen layers
N2 - During their evolution, massive stars are characterized by a significant loss of mass either via spherically symmetric stellar winds or by aspherical mass-loss mechanisms, namely outflowing equatorial disks. However, the scenario that leads to the formation of a disk or rings of gas and dust around these objects is still under debate. Is it a viscous disk or an ouftlowing disk-forming wind or some other mechanism? It is also unclear how various physical mechanisms that act on the circumstellar environment of the stars affect its shape, density, kinematic, and thermal structure. We assume that the disk-forming mechanism is a viscous transport within an equatorial outflowing disk of a rapidly or even critically rotating star. We study the hydrodynamic and thermal structure of optically thick dense parts of outflowing circumstellar disks that may form around, e.g., Be stars, sgB[e] stars, or Pop III stars. We calculate self-consistent time-dependent models of the inner dense region of the disk that is strongly affected either by irradiation from the central star and by contributions of viscous heating effects. We also simulate the dynamic effects of collision between expanding ejecta of supernovae and circumstellar disks that may be form in sgB[e] stars and, e.g., LBVs or Pop III stars.
ER -
KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA. Modeling sgB[e] Circumstellar Disks. Online. In Anatoly Miroshnichenko, Sergey Zharikov, Daniela Korčáková, Marek Wolf. \textit{The B[e] Phenomenom: Forty Years of Studies}. 508. vyd. San Francisco, USA: Astronomical Society of the Pacific, 2017, s.~17-22. ISBN~978-1-58381-900-5.
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