. . . . . "GA205/02/0445" . . "1"^^ . . "Neuvedeno."@en . . "1"^^ . "Pr\u00E1ce na \u0159e\u0161en\u00ED projektu Fyzika hork\u00FDch hv\u011Bzd a hv\u011Bzdn\u00FDch soustav s hork\u00FDmi slo\u017Ekami p\u0159inesla \u0159adu nov\u00FDch v\u00FDsledk\u016F prezentovan\u00FDch na konferenc\u00EDch, p\u0159edn\u00E1\u0161k\u00E1ch i ve vysoko\u0161kolsk\u00FDch skriptech. Projekt napomohl profilaci odborn\u00E9ho zam\u011B\u0159en\u00ED obou pracovi\u0161\u0165 a"@cs . "http://www.isvav.cz/projectDetail.do?rowId=GA205/02/0445"^^ . . . "Physics of hot stars and stellar systems with hot components"@en . . . . "The present common project of Bmo and Ond\u0159ejov stellar astronomers is aimed at the layout of current thorny problems of the physics of hot stars and stellar systems containing hot components. First, we want to contribute to elucidation of mutual relationamong magnetic field geometry, spectroscopic and photometric spots or belts occurring on the surface of chemically peculiar (CP) stars. For the localization of spots of chemical elements by the analysis of their line profile variations a special technique of Doppler imaging will be used. Particularly, by means of a detailed study of a prototype of cool CP2 stars CQ UMa we want to solve the puzzle of the variable depression in energy distribution around 410 nm, typical for such a type of CP stars. Various hypotheses explaining the origin of Be-phenomenon will be tested by the observation of several B star with emission lines in their spectra. From the both theoretical and observational point of view will be studied extended atmospheres of"@en . . "P\u0159edlo\u017Een\u00FD spole\u010Dn\u00FD projekt brn\u011Bnsk\u00FDch a ond\u0159ejovsk\u00FDch stel\u00E1rn\u00EDch astronom\u016F je zac\u00EDlen na \u0159e\u0161en\u00ED sou\u010Dasn\u00FDch pal\u010Div\u00FDch fyziky hork\u00FDch hv\u011Bzd a hv\u011Bzdn\u00FDch syst\u00E9m\u016F obsahuj\u00EDc\u00EDch hork\u00E9 slo\u017Eky. P\u0159edn\u011B chceme p\u0159isp\u011Bt k osv\u011Btlen\u00ED vz\u00E1jemn\u00FDch vztah\u016F mezi geometri\u00ED magnetick\u00E9ho pole, spektroskopick\u00FDmi a fotometrick\u00FDmi skvrnami nach\u00E1zej\u00EDc\u00EDmi se na povrchu chemicky pekuli\u00E1rn\u00EDch (CP) hv\u011Bzd. Pro lokalizaci skvrn chemick\u00FDch prvk\u016F na z\u00E1klad\u011B rozboru profil\u016F jejich spektr\u00E1ln\u00EDch car bude pou\u017Eita zvl\u00E1\u0161tn\u00ED technika tzv. Dopplerova zobrazov\u00E1n\u00ED. Speci\u00E1ln\u011B pak chceme prost\u0159ednictv\u00EDm detailn\u00EDho studia prototypu tzv. chladn\u00FDch CP2 hv\u011Bzd, hv\u011Bzdy CQ UMa, vy\u0159e\u0161it h\u00E1danku prom\u011Bnn\u00E9 deprese v rozlo\u017Een\u00ED energie kolem 410 nm, kter\u00E1 je pro tento typ CP hv\u011Bzd typick\u00E1. Na z\u00E1klad\u011B pozorov\u00E1n\u00ED n\u011Bkolika vybran\u00FDch hv\u011Bzd spektr\u00E1ln\u00EDho typu B s emisn\u00EDmi \u010Darami budou testov\u00E1ny hypot\u00E9zy vzniku Be jevu. Z teoretick\u00E9ho i pozorovatelsk\u00E9ho hlediska budou studov\u00E1ny rozs\u00E1hl\u00E9 atmosf\u00E9ry hork\u00FDch hv\u011Bzd a jejich non-LTE model\u016F, stejn\u011B jako hv\u011Bzdn\u00E9" . "The solution of the project Physics of hot stars and stellar systems with hot components has fetched many new scientific results presented by a number ways (conferences, lectures, publications, textbooks). The project have helped to deepen the orientatio"@en . . . . . "Fyzika hork\u00FDch hv\u011Bzd a hv\u011Bzdn\u00FDch syst\u00E9m\u016F s hork\u00FDmi slo\u017Ekami" . "51"^^ . "51"^^ . "2008-06-02+02:00"^^ . "0"^^ . .