"hot stars" . "2007-01-01+01:00"^^ . "14"^^ . "Stellar winds of first stars in the Universe"@en . "GA205/07/0031" . "14"^^ . " hydrodynamics" . "Pova\u017Eovat v\u00FDsledky \u0159e\u0161en\u00ED za dostate\u010Dn\u011B pr\u016Fkazn\u00E9. Publika\u010Dn\u00ED v\u00FDstupy jsou dostate\u010Dn\u011B kvalitn\u00ED a po\u010Dtem odpov\u00EDdaj\u00ED velikosti \u0159e\u0161itelsk\u00E9ho kolektivu. Finan\u010Dn\u00ED hospoda\u0159en\u00ED bez z\u00E1vad."@cs . . . "0"^^ . . . "1"^^ . "hot stars; stellar wind; hydrodynamics; first stars in the Universe"@en . . "1"^^ . "Chemical composition of first stars in the Universe was given by the primordial nucleosynthesis: first stars were composed basically only from hydrogen and helium. Numerical simulations of their formation show that first stars were very massive and consequently hot. Present hot stars have stellar winds accelerated due to the light absorption in the lines of heavier elements (carbon, nitrogen, etc.). We plan to test if massive first stars in the Universe had stellar winds. We will test the influenceof rotation on the stellar winds of first stars. We plan to study stellar winds of very low metallicity stars. We derive the minimum metallicity necessary to launch a normal stellar wind. We also plan to study purely metallic winds of these stars. The detailed study of stellar winds of first stars is necessary for the prediction of the evolution of these stars and for our understanding of the state of the interstellar medium. We also plan to provide emergent fluxes from atmospheres and possibly winds"@en . . "2015-01-22+01:00"^^ . "2009-12-31+01:00"^^ . "Chemick\u00E9 slo\u017Een\u00ED prvn\u00EDch hv\u011Bzd ve vesm\u00EDru bylo d\u00E1no prvotn\u00ED nukleosynt\u00E9zou: prvn\u00ED hv\u011Bzdy byly slo\u017Eeny v podstat\u011B pouze z vod\u00EDku a helia. Numerick\u00E9 simulace vzniku prvn\u00EDch hv\u011Bzd vedou k z\u00E1v\u011Bru, \u017Ee prvn\u00ED hv\u011Bzdy ve vesm\u00EDru byly velmi hmotn\u00E9 a tedy hork\u00E9. Dne\u0161n\u00ED hork\u00E9 hv\u011Bzdy maj\u00ED hv\u011Bzdn\u00FD v\u00EDtr urychlovan\u00FD absorpc\u00ED z\u00E1\u0159en\u00ED v \u010Dar\u00E1ch t\u011B\u017E\u0161\u00EDch prvk\u016F (jako jsou uhl\u00EDk, dus\u00EDk, atd.). Pl\u00E1nujeme zjistit, zda hmotn\u00E9 prvn\u00ED hv\u011Bzdy tak\u00E9 m\u011Bly hv\u011Bzdn\u00E9 v\u011Btry. Budeme testovat vliv rotace na p\u0159\u00EDpadn\u00FD vznik hv\u011Bzdn\u00E9ho v\u011Btru prvn\u00EDch hv\u011Bzd. Pl\u00E1nujeme studovat hv\u011Bzdn\u00E9 v\u011Btry hv\u011Bzd s velmi mal\u00FDm obsahem t\u011B\u017E\u0161\u00EDch prvk\u016F. Ur\u010D\u00EDme minim\u00E1ln\u00ED obsah t\u011B\u017E\u0161\u00EDch prvk\u016F nutn\u00FDch pro urychlen\u00ED b\u011B\u017En\u00E9ho hv\u011Bzdn\u00E9ho v\u011Btru. Tak\u00E9 budeme studovat hv\u011Bzdn\u00E9 v\u011Btry t\u011Bchto hv\u011Bzd slo\u017Een\u00E9 pouze z t\u011B\u017E\u0161\u00EDch prvk\u016F. Podrobn\u00E9 studium hv\u011Bzdn\u00FDch v\u011Btr\u016F prvn\u00EDch hv\u011Bzd je d\u016Fle\u017Eit\u00E9 pro v\u00FDpo\u010Det jejich v\u00FDvoje a pro pochopen\u00ED stavu mezihv\u011Bzdn\u00E9ho prost\u0159ed\u00ED. V\u00FDsledkem \u0159e\u0161en\u00ED projektu budou mimo jin\u00E9 spo\u010Dten\u00E9 z\u00E1\u0159iv\u00E9 toky vych\u00E1zej\u00EDc\u00ED z atmosf\u00E9r a p\u0159\u00EDpadn\u00FDch v\u011Btr\u016F prvn\u00EDch hv\u011Bzd," . "."@en . "http://www.isvav.cz/projectDetail.do?rowId=GA205/07/0031"^^ . . . . . . . . . " stellar wind" . "2009-04-22+02:00"^^ . . . "Hv\u011Bzdn\u00E9 v\u011Btry prvn\u00EDch hv\u011Bzd ve vesm\u00EDru" . . .