. "stars" . . "2014-03-31+02:00"^^ . . . . " spectroscopy" . . . "We aim toward new insights of the magnetic chemically peculiar (mCP) stars of the upper main sequence. This star group is an excellent astrophysical laboratory for testing processes like diffusion, accretion, and mass loss. The found variability of mCP stars is explained in terms of the oblique rotator model according to which, the period of the observed light, spectrum and magnetic field variations is correlated to the rotational period. Accurate knowledge of the period of variability of mCP stars is a fundamental step in understanding their complex behavior, especially as far as it concerns the phase relation between the magnetic, spectral and light variations. It has been suggested that CP stars undergo magnetic braking during their main sequence lifetime, due to mass accretion and/or mass loss. But no conclusive results are available by now. Deriving the periods of variable CP stars in different clusters from photometry in combination with the known age results of these clusters, it is finally possible to gain information about the evolution of rotational periods and thus the effects of magnetic braking. In addition, we propose to apply the tool of Doppler imaging which has become very successful to gain information on inhomogeneities on the surface of a rotating star caused by changing abundance and/or magnetic field structure. The DI technique uses the information contained in the time series of spectra and inverts them into elemental surface distributions."@en . . . . "Shed more light on magnetic stars"@en . " magnetic stars" . "0"^^ . "2014-01-01+01:00"^^ . "7AMB14AT015" . "0"^^ . "http://www.isvav.cz/projectDetail.do?rowId=7AMB14AT015"^^ . "1"^^ . "Nov\u00FD pohled na magnetick\u00E9 hv\u011Bzdy" . "stars; magnetic stars; spectroscopy; photometry"@en . "9"^^ . . "2015-05-28+02:00"^^ . . "9"^^ . . "2015-12-31+01:00"^^ . . . . "Na\u0161\u00EDm c\u00EDlem je nov\u00FD pohled na magneticky chemick\u00E9 pekuni\u00E1rn\u00ED hv\u011Bzdy (mCP) horn\u00ED \u010D\u00E1sti hlavn\u00ED posloupnosti. Tato skupina hv\u011Bzd je excelentn\u00ED astrofyzik\u00E1ln\u00ED laborato\u0159\u00ED pro testov\u00E1n\u00ED proces\u016F jako jsou difuse, akrece a ztr\u00E1ta hmoty. Nalezen\u00ED prom\u011Bnnosti mCP hv\u011Bzd je vysv\u011Btlov\u00E1no pomoc\u00ED modelu \u0161ikm\u00E9ho rot\u00E1toru, podle kter\u00E9ho perioda pozorovan\u00FDch zm\u011Bn ve sv\u011Btle, spektru a magnetick\u00E9m poli je korelov\u00E1na s rota\u010Dn\u00ED periodou. P\u0159esn\u00E9 poznatky o zm\u011Bn\u011B periody prom\u011Bnnosti mCP hv\u011Bzd je z\u00E1kladn\u00ED krok v pochopen\u00ED jejich komplexn\u00EDho chov\u00E1n\u00ED, zejm\u00E9na pokud se zam\u011B\u0159\u00EDme na f\u00E1zov\u00E9 relace mezi magnetick\u00FDmi, spektr\u00E1ln\u00EDmi a sv\u011Bteln\u00FDmi zm\u011Bnami. Bylo navr\u017Eeno, \u017Ee CP hv\u011Bzdy podstupuj\u00ED b\u011Bhem sv\u00E9ho \u017Eivota na hlavn\u00ED posloupnosti magnetick\u00E9 brzd\u011Bn\u00ED prost\u0159ednictv\u00EDm akrece hmoty a nebo jej\u00ED ztr\u00E1tou. Do sou\u010Dasnosti v\u0161ak nen\u00ED k dispozici pr\u016Fkazn\u00FD argument. Ur\u010Den\u00ED period prom\u011Bnn\u00FDch CP hv\u011Bzd v r\u016Fzn\u00FDch uskupen\u00EDch z fotometrie v kombinaci se zn\u00E1m\u00FDm v\u011Bkem t\u011Bchto uskupen\u00ED m\u016F\u017Ee v\u00E9st k z\u00EDsk\u00E1n\u00ED informace o v\u00FDvoji rota\u010Dn\u00ED periody v \u010Dase a \u00FA\u010Dinc\u00EDch magnetick\u00E9ho brzd\u011Bn\u00ED. Krom\u011B toho chceme pou\u017E\u00EDt metody Dopplerovsk\u00E9ho zobrazov\u00E1n\u00ED, kter\u00E1 se stala velmi u\u017Eite\u010Dnou p\u0159i z\u00EDsk\u00E1v\u00E1n\u00ED informac\u00ED o nehomogenit\u00E1ch na povrchu rotuj\u00EDc\u00ED hv\u011Bzdy, kter\u00E9 mohou b\u00FDt zp\u016Fsoben\u00E9 r\u016Fzn\u00FDmi abundancemi prvk\u016F a nebo strukturou magnetick\u00E9ho pole. Technika Dopplerovsk\u00E9ho zobrazen\u00ED vyu\u017E\u00EDv\u00E1 informace obsa\u017Een\u00E9 v \u010Dasov\u00E9 \u0159ad\u011B spekter, ze kter\u00E9 je pak mo\u017En\u00E9 z\u00EDskat rozlo\u017Een\u00ED jednoliv\u00FDch prvk\u016F na povrchu hv\u011Bzdy. K tomuto \u00FA\u010Delu vyu\u017Eijeme i unik\u00E1tn\u00ED sadu spekter, kter\u00E1 jsme z\u00EDskali b\u011Bhem dvou pozorovac\u00EDch mis\u00ED na p\u0159\u00EDstroji FEROS v letech 2011 a 2012." . .