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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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