"1"^^ . "9"^^ . . "\u010Clen\u016Fm \u0159e\u0161itelsk\u00E9ho t\u00FDmu se poda\u0159ilo vypracovat hydrodynamick\u00FD k\u00F3d pro \u010Dasov\u011B z\u00E1visl\u00E9 modely v\u00EDceslo\u017Ekov\u00FDch hv\u011Bzdn\u00FDch v\u011Btr\u016F. S vyu\u017Eit\u00EDm tohoto k\u00F3du jsme analyzovali a prov\u011B\u0159ovali stabilitu r\u016Fzn\u00FDch model\u016F v\u011Btru hork\u00FDch hv\u011Bzd. Tyto modely v\u0161ak v sob\u011B zahrnovaly n\u011Bkolik aproximac\u00ED. Hlavn\u00ED aproximace spo\u010D\u00EDv\u00E1 ve zjednodu\u0161uj\u00EDc\u00EDm tvaru z\u00E1\u0159iv\u00E9 s\u00EDly, kter\u00FD je platn\u00FD pouze v Sobolevov\u011B aproximaci. Pro konzistentn\u00ED posouzen\u00ED stability a p\u0159edev\u0161\u00EDm pak generace p\u0159\u00EDpadn\u00FDch nestabilit, je t\u0159eba nam\u00EDsto tohoto jednoduch\u00E9ho lok\u00E1ln\u00EDho vyj\u00E1d\u0159en\u00ED zahrnout v rozumn\u00E9 m\u00ED\u0159e absorpci i rozptyl z\u00E1\u0159en\u00ED. C\u00EDlem p\u0159edkl\u00E1dan\u00E9ho projektu je roz\u0161\u00ED\u0159en\u00ED k\u00F3du o detailn\u011Bj\u0161\u00ED v\u00FDpo\u010Dty z\u00E1\u0159iv\u00E9 s\u00EDly, zahrnuj\u00EDc\u00ED v sob\u011B absorpci a rozptyl. D\u00E1le potom nam\u00EDsto izotermick\u00FDch proces\u016F posoudit a zahrnout vliv z\u00E1\u0159iv\u00E9ho ochlazovan\u00ED a oh\u0159evu."@cs . "0"^^ . . . "2005-01-01+01:00"^^ . . "2007-12-01+01:00"^^ . "2"^^ . . "Time dependent models of multicomponent stellar winds"@en . "645"^^ . "Members of the team sucesfully completed hydrodynamical code for time dependent models of multicomponent stellar winds. With this code we analysed stability of various models of radiatively driven stellar winds from hot stars. But these models were simplified due to the expression of radiative force, which is right only in Sobolev approximation. For consistent review of stability and for analyse of instabilities generated in the radiatively driven stellar winds we must include in radiative force non-local radiative processes. The aim of the proposed project is extension of the code for more detail calculation of radiative force . Moreover, instead of isothermal processes we plan to use energy balance equation with radiative cooling and heating term."@en . . "stellar wind; hot stars; hydrodynamics; instabilities"@en . "\u010Casov\u011B z\u00E1visl\u00E9 modely v\u00EDceslo\u017Ekov\u00E9ho hv\u011Bzdn\u00E9ho v\u011Btru"@cs . . . . . "9"^^ . . "645"^^ . .