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@inproceedings{1374335,
author = {Krtička, Jiří and Krtičková, Iva},
address = {San Francisco, USA},
booktitle = {The B[e] Phenomenom: Forty Years of Studies},
edition = {508},
editor = {Miroshnichenko, A., Zharikov, S, Korcakova, D.},
keywords = {hot stars; B[e] stars; variability},
howpublished = {tištěná verze "print"},
language = {eng},
location = {San Francisco, USA},
isbn = {978-1-58381-900-5},
pages = {383-384},
publisher = {Astronomical Society of the Pacific},
title = {Ultraviolet Variability of B[e] Stars},
url = {http://www.aspbooks.org/a/volumes/article_details/?paper_id=38037},
year = {2017}
}
TY - JOUR
ID - 1374335
AU - Krtička, Jiří - Krtičková, Iva
PY - 2017
TI - Ultraviolet Variability of B[e] Stars
PB - Astronomical Society of the Pacific
CY - San Francisco, USA
SN - 9781583819005
KW - hot stars
KW - B[e] stars
KW - variability
UR - http://www.aspbooks.org/a/volumes/article_details/?paper_id=38037
N2 - Hot stars emit most of their light in the ultraviolet. Therefore, the visual domain in which the variability is mostly studied traces just a small part of the spectral energy distribution. To overcome this, we searched archival data of the IUE satellite for the ultraviolet spectra of B[e] stars. We studied each star individually and identified the differences between the variability in the near and far ultraviolet domains. Although the data are typically very sparse, we detected the variability of the spectral energy distribution and of the line profiles. The variability has several sources of origin, including the light absorption by the dust clouds and the disk, pulsations, and eclipses in the case of binaries. The ultraviolet domain is the key to understanding the variability of B[e] stars.
ER -
KRTIČKA, Jiří a Iva KRTIČKOVÁ. Ultraviolet Variability of B[e] Stars. In Miroshnichenko, A., Zharikov, S, Korcakova, D. \textit{The B[e] Phenomenom: Forty Years of Studies}. 508. vyd. San Francisco, USA: Astronomical Society of the Pacific, 2017, s.~383-384. ISBN~978-1-58381-900-5.
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