Ultraviolet Variability of B[e] Stars

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F17%3A00094659" target="_blank" >RIV/00216224:14310/17:00094659 - isvavai.cz</a>
Result on the web
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DOI - Digital Object Identifier
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Result language
angličtina
Original language name
Ultraviolet Variability of B[e] Stars
Original language description
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.
Czech name
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Czech description
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Project
<a href="/en/project/GA16-01116S" target="_blank" >GA16-01116S: Atmospheres and circumstellar environment of magnetic hot stars</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year
2017
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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