"2015-12-31+01:00"^^ . . "evolved stars; massive stars; mass-loss; circumstellar shells; dust and molecules"@en . . . . . . " mass-loss" . "2014-01-01+01:00"^^ . "Tracing the mass-loss history in evolved massive stars"@en . . " massive stars" . . . "1"^^ . . "0"^^ . "2015-05-28+02:00"^^ . . . "1"^^ . "In this collaboration project we will study the mass-loss history in evolved massive stars, focusing in particular on stars in the LBV and the B[e]SG phases. Our investigations aim mainly at using and processing data obtained from the new generation of 6-8 mts telescopes, such as those in GEMINI and ESO observatories. All these new data, spreading from the optical up to the radio regime, are fundamental to study the structure and kinematics of the circumstellar material of these objects. The aim of the proposed research project is to deepen our understanding of the physics of stellar winds and the formation of circumstellar disks, shells, and nebulae around massive, evolved stars. This is of fundamental importance, because these objects display a short but nevertheless highly important role in the evolution of massive stars which is still not understood. Our current lack in understanding the physics that causes the strongly enhanced mass-loss in these short-lived phases together with proper estimates of the mass-loss rates in these objects is the major reason why these highly important phases can still not be predicted with modern numerical evolution codes. These evolutionary phases are characterized by some enormous mass-loss from the central star resulting in the formation of dense, sometimes disk- or ring-like structures of ejected material. This circumstellar material is so cool and dense that molecules and dust can form and survive under the rather harsh conditions usually given in the close vicinity of such hot and luminous objects. Both the LBV and the B[e] supergiant phenomena are unique in the evolution of massive stars, and as long as we do not understand these specific phases, we miss very important pieces of the puzzle called massive star evolution."@en . . "1"^^ . "Sledov\u00E1n\u00ED historie ztr\u00E1ty hmoty vyvinut\u00FDch masivn\u00EDch hv\u011Bzd" . "http://www.isvav.cz/projectDetail.do?rowId=7AMB14AR017"^^ . " circumstellar shells" . "2014-03-17+01:00"^^ . . "7AMB14AR017" . "evolved stars" . . "V tomto projektu spolupr\u00E1ce budeme studovat historii-ztr\u00E1ty hmoty vyvinut\u00FDch masivn\u00EDch hv\u011Bzd se zam\u011B\u0159en\u00EDm zejm\u00E9na na hv\u011Bzdy ve f\u00E1z\u00EDch z\u00E1\u0159iv\u00FDch modr\u00FDch prom\u011Bnn\u00FDch (LBV) a B[e] veleobr\u016F. N\u00E1\u0161 v\u00FDzkum je zam\u011B\u0159en p\u0159edev\u0161\u00EDm na vyu\u017Eit\u00ED a zpracov\u00E1n\u00ED dat z\u00EDskan\u00FDch z nov\u00E9 generace 6-8 metrov\u00FDch dalekohled\u016F, jako jsou na observato\u0159\u00EDch GEMINI a ESO. V\u0161echna tato nov\u00E1 data od optick\u00E9 a\u017E do r\u00E1diov\u00E9 oblasti maj\u00ED z\u00E1sadn\u00ED v\u00FDznam pro studium struktury a kinematiky okolohv\u011Bzdn\u00E9 hmoty t\u011Bchto objekt\u016F. C\u00EDlem navrhovan\u00E9ho v\u00FDzkumn\u00E9ho projektu je prohloubit na\u0161e ch\u00E1p\u00E1n\u00ED fyziky hv\u011Bzdn\u00FDch v\u011Btr\u016F a formov\u00E1n\u00ED cirkumstel\u00E1rn\u00EDch disk\u016F, skupek a mlhovin kolem masivn\u00EDch vyvinut\u00FDch hv\u011Bzd. To m\u00E1 z\u00E1sadn\u00ED v\u00FDznam, proto\u017Ee tyto objekty zobrazuj\u00ED kr\u00E1tkou, ale p\u0159esto velmi v\u00FDznamnou a p\u0159itom neprozkoumanou roli ve v\u00FDvoji velmi masivn\u00EDch hv\u011Bzd. N\u00E1\u0161 sou\u010Dasn\u00FD nedostatek v pochopen\u00ED fyziky, kter\u00E1 zp\u016Fsobuje v\u00FDrazn\u011B vy\u0161\u0161\u00ED ztr\u00E1tu hmoty v t\u011Bchto kr\u00E1tkodob\u00FDch f\u00E1z\u00EDch, spole\u010Dn\u011B s v\u011Brohodn\u00FDmi odhady rychlosti ztr\u00E1ty hmoty v t\u011Bchto objektech je hlavn\u00ED d\u016Fvod, pro\u010D tyto velmi v\u00FDznamn\u00E9 f\u00E1ze st\u00E1le nelze p\u0159edv\u00EDdat pomoc\u00ED modern\u00EDch numerick\u00FDch v\u00FDvojov\u00FDch k\u00F3d\u016F. Tyto v\u00FDvojov\u00E9 f\u00E1ze se vyzna\u010Duj\u00ED ohromnou ztr\u00E1tou hmoty z centr\u00E1ln\u00ED hv\u011Bzdy, \u010D\u00EDm\u017E doch\u00E1z\u00ED k tvorb\u011B hust\u00FDch, n\u011Bkdy diskov\u00FDch nebo prstencov\u00FDch struktur vypou\u0161t\u011Bn\u00E9ho materi\u00E1lu. Tento okolohv\u011Bzdn\u00FD materi\u00E1l je tak chladn\u00FD a hust\u00FD, \u017Ee prach \u010Di molekuly se mohou vytv\u00E1\u0159et a p\u0159e\u017E\u00EDvat v drsn\u00FDch podm\u00EDnk\u00E1ch, kter\u00E9 oby\u010Dejn\u011B panuj\u00ED v t\u011Bsn\u00E9 bl\u00EDzkosti t\u011Bchto hork\u00FDch a z\u00E1\u0159iv\u00FDch objekt\u016F. Jevy v LBV hv\u011Bzd\u00E1ch i v B[e] veleobrech jsou jedine\u010Dn\u00E9 ve v\u00FDvoji masivn\u00EDch hv\u011Bzd, a tak dokud nepochop\u00EDme tyto specifick\u00E9 f\u00E1ze, budou n\u00E1m chyb\u011Bt velmi d\u016Fle\u017Eit\u00E9 \u010D\u00E1sti \u0159e\u0161en\u00ED probl\u00E9mu v\u00FDvoje masivn\u00EDch hv\u011Bzd." . . "0"^^ . .